Info for CDF datasets:

AC_H0_SWE
Description
SWEPAM - Solar Wind Electron Proton Alpha Monitor 
References: http://www.srl.caltech.edu/ACE/  
The quality of ACE level 2 data is such that it is suitable for serious 
scientific study.  However, to avoid confusion and misunderstanding, it 
is recommended that users consult with the appropriate ACE team members
before publishing work derived from the data. The ACE team has worked 
hard to ensure that the level 2 data are free from errors, but the team 
cannot accept responsibility for erroneous data, or for misunderstandings 
about how the data may be used. This is especially true if the appropriate 
ACE team members are not consulted before publication. At the very 
least, preprints should be forwarded to the ACE team before publication.


Modification History
Initial Release 02/23/00.
12/04/02: Fixed alpha/proton ratio precision bug.
12/04/02: Fixed description of Epoch time variable.


Variable Notes

Solar Wind Proton Number Density, scalar
Np is the proton number density in units of cm-3, as calculated by integrating
the ion distribution function.
Solar Wind Bulk Speed
Vp is the solar wind proton speed, or more generally just the solar wind (bulk)
speed. It is obtained by integrating the ion (proton) distribution function.
radial component of the proton temperature
The radial component of the proton temperature is the (1,1) component of the
temperature tensor, along the radial direction. It is obtained by integration of
the ion (proton) distribution function.
alpha to proton density ratio
Alpha ratio (Na/Np) - is the ratio of the number density of helium++ ions to the
number density of protons.
Solar Wind Velocity in GSE coord., 3 components
Solar Wind Velocity in GSE coord., 3 components
Solar Wind Velocity in RTN coord., 3 components
Solar Wind Velocity in RTN coord., 3 components
Solar Wind Velocity in GSM coord., 3 comp.
Solar Wind Velocity in GSM coord., 3 comp.
ACE s/c position, 3 comp. in GSE coord.
ACE s/c position, 3 comp. in GSE coord.
Label for ACE Position (GSE)
Label for ACE Position (GSE)
ACE s/c position, 3 comp. in GSM coord.
ACE s/c position, 3 comp. in GSM coord.


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AC_H2_EPM
Description
The Electron, Proton, and Alpha Monitor (EPAM) is composed of five 
telescope apertures of three different types.  Two Low Energy 
Foil Spectrometers (LEFS) measure the flux and direction of electrons 
above 30 keV (geometry factor = 0.397 cm2*sr), two Low Energy Magnetic 
Spectrometers (LEMS) measure the flux  and direction of ions greater than 50 keV 
(geometry factor = 0.48 cm2*sr), and the Composition Aperture (CA) 
measures the elemental composition of the ions (geometry factor = 0.24 
cm2*sr). The telescopes use the spin of the spacecraft to sweep the full 
sky. Solid-state detectors are used to measure the energy and composition 
of the incoming particles. 
For more information about the EPAM instrument, visit the EPAM Home Page, 
at JHU/APL: http://www.srl.caltech.edu/ACE/  
The quality of ACE level 2 data is such that it is suitable for serious 
scientific study.  However, to avoid confusion and misunderstanding, it 
is recommended that users consult with the appropriate ACE team members
before publishing work derived from the data. The ACE team has worked 
hard to ensure that the level 2 data are free from errors, but the team 
cannot accept responsibility for erroneous data, or for misunderstandings 
about how the data may be used. This is especially true if the appropriate 
ACE team members are not consulted before publication. At the very 
least, preprints should be forwarded to the ACE team before publication.


Modification History
Initial Release 01/10/03




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AC_H2_SWE
Description
SWEPAM - Solar Wind Electron Proton Alpha Monitor 
References: http://www.srl.caltech.edu/ACE/  
The quality of ACE level 2 data is such that it is suitable for serious 
scientific study.  However, to avoid confusion and misunderstanding, it 
is recommended that users consult with the appropriate ACE team members
before publishing work derived from the data. The ACE team has worked 
hard to ensure that the level 2 data are free from errors, but the team 
cannot accept responsibility for erroneous data, or for misunderstandings 
about how the data may be used. This is especially true if the appropriate 
ACE team members are not consulted before publication. At the very 
least, preprints should be forwarded to the ACE team before publication.


Modification History
Initial Release 04/04/02.
12/04/02: Fixed alpha/proton ratio precision bug.
12/04/02: Fixed description of Epoch time variable.
12/04/02: -9999.9 fill-data values changed to -1.0e+31.


Variable Notes

Solar Wind Proton Number Density, scalar
Np is the proton number density in units of cm-3, as calculated by integrating
the ion distribution function.
Solar Wind Bulk Speed
Vp is the solar wind proton speed, or more generally just the solar wind (bulk)
speed. It is obtained by integrating the ion (proton) distribution function.
radial component of the proton temperature
The radial component of the proton temperature is the (1,1) component of the
temperature tensor, along the radial direction. It is obtained by integration of
the ion (proton) distribution function.
alpha to proton density ratio
Alpha ratio (Na/Np) - is the ratio of the number density of helium++ ions to the
number density of protons.
Solar Wind Velocity in GSE coord., 3 components
Solar Wind Velocity in GSE coord., 3 components
Solar Wind Velocity in RTN coord., 3 components
Solar Wind Velocity in RTN coord., 3 components
Solar Wind Velocity in GSM coord., 3 comp.
Solar Wind Velocity in GSM coord., 3 comp.
ACE s/c position, 3 comp. in GSE coord.
ACE s/c position, 3 comp. in GSE coord.
Label for ACE Position (GSE)
Label for ACE Position (GSE)
ACE s/c position, 3 comp. in GSM coord.
ACE s/c position, 3 comp. in GSM coord.


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AC_H2_SWI
Description
SWICS - Solar Wind Electron Proton Alpha Monitor 
References: http://www.srl.caltech.edu/ACE/  
The quality of ACE level 2 data is such that it is suitable for serious 
scientific study.  However, to avoid confusion and misunderstanding, it 
is recommended that users consult with the appropriate ACE team members
before publishing work derived from the data. The ACE team has worked 
hard to ensure that the level 2 data are free from errors, but the team 
cannot accept responsibility for erroneous data, or for misunderstandings 
about how the data may be used. This is especially true if the appropriate 
ACE team members are not consulted before publication. At the very 
least, preprints should be forwarded to the ACE team before publication.


Modification History
Initial Release 04/04/02


Variable Notes

Velocity of H+ in km/s
vH is the mean Hydrogen+ ion speed in km/s, as measured bythe Solar Wind Ion
Composition Spectrometer (SWICS).
Thermal Velocity of H+ in km/s
vthH is the thermal speed of H+ in km/s, as measured by the Solar Wind Ion
Composition Spectrometer (SWICS).
Velocity of He+ in km/s
vHe is the mean Helium++ ion speed in km/s, as measured bythe Solar Wind Ion
Composition Spectrometer (SWICS).
Thermal Velocity of He++ in km/s
vthHe is the thermal speed of He++ in km/s, as measured by the Solar Wind Ion
Composition Spectrometer (SWICS).
Velocity of O+6 in km/s
vO6 is the mean Oxygen+6 ion speed in km/s, as measured bythe Solar Wind Ion
Composition Spectrometer (SWICS).
Thermal Velocity of He++ in km/s
vthO6 is the thermal speed of Oxygen+6 in km/s, as measured by the Solar Wind
Ion Composition Spectrometer (SWICS).
Velocity of O+6 in km/s
vMg is the mean Mg+10 ion speed in km/s, as measured bythe Solar Wind Ion
Composition Spectrometer (SWICS).
Thermal Velocity of Mg+10 in km/s
vthMg is the thermal speed of Mg+10 in km/s, as measured by the Solar Wind Ion
Composition Spectrometer (SWICS).
Velocity of Fe+11 in km/s
vFe is the mean Fe+11 ion speed in km/s, as measured bythe Solar Wind Ion
Composition Spectrometer (SWICS).
Thermal Velocity of Fe+11 in km/s
vthFe is the thermal speed of Fe+11 in km/s, as measured by the Solar Wind Ion
Composition Spectrometer (SWICS).
4He++ to O+6 Ratio
Ratio He/O - is the ratio of  the number density of Helium++ ions to the number
density of O++6 ions.
20Ne+8 to O+6 Ratio
Ratio NetoO - is the ratio of  the number density of 20Ne+8 ions to the number
density of O+6 ions.
24Mg+10 to O+6 Ratio
Ratio Mg/O - is the ratio of  the number density of 24Mg+10 ions to the number
density of O+6 ions.
56Fe+(7 to 12) to O+6 Ratio
Ratio Fe/O - is the ratio of  the number density of 56Fe+(7 to 12) ions to the
number density of O++6 ions.
3He++ to 4He++ Ratio
Ratio He3to4 - is the ratio of  the number density of 3He++ ions to the number
density of 4He++ ions.
22Ne+8 to 20Ne+8 Ratio
Ratio Ne22to20 - is the ratio of  the number density of  22Ne+8 ions to the
number density of 20Ne+8 ions.
24Mg+10 to 26Mg+10 Ratio
Ratio Mg24to26 - is the ratio of  the number density of  24Mg+10 ions to the
number density of 26Mg+10 Ratio ions.
12C+5/12C+6 Ratio
Ratio C5to6 - is the ratio of  the number density of 12C+5 ions to the number
density of 12C+6 ions.
16O+7/16O+6 Ratio
Ratio O7/O6 - is the ratio of  the number density of 16O+7 ions to the number
density of 16O+6 ions.
56Fe+11/56Fe+9 Ratio
Ratio Fe11to9 - is the ratio of  the number density of 56Fe+11 ions to the
number density of 56Fe+9 ions.


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AC_K0_MFI
Description
MAG - ACE Magnetic Field Experiment
References: http://www.srl.caltech.edu/ACE/  



ACE browse data is designed for monitoring large scale particle and field 
behavior and for selecting interesting time periods. The data is automatically 
generated from the spacecraft data stream using simple algorithms provided by 
the instrument teams. It is not routinely checked for accuracy and is subject 
to revision. Use this data at your own risk, and consult with the appropriate 
instrument teams about citing it. 
MAG Browse data is not validated by the experimenters and should not be used 
except for preliminary examination prior to detailed studies.


Modification History
Initial Release 11/10/98




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AC_K0_SIS
Description
SIS - ACE Solar Isotope Spectrometer
References: http://www.srl.caltech.edu/ACE/ 
ACE browse data is designed for monitoring large scale particle and field 
behavior and for selecting interesting time periods. The data is automatically 
generated from the spacecraft data stream using simple algorithms provided by 
the instrument teams. It is not routinely checked for accuracy and is subject 
to revision. Use this data at your own risk, and consult with the appropriate 
instrument teams about citing it. 
SIS Browse data is not validated by the experimenters and should not be used 
except for preliminary examination prior to detailed studies.


Modification History
Initial Release 04/10/99


Variable Notes

Proton Flux (E > 10 MeV)
E > 10 MeV/nuc
Proton Flux (E > 30 MeV)
E > 30 MeV/nuc
CNO Flux (7-10 MeV/nuc)
Flux of CNO with 7-10 MeV/nuc
CNO Flux (10-15 MeV/nuc)
Flux of CNO with 10-15 MeV/nuc
Z >= 10 flux (9-21 MeV/nuc)
Flux of Z >= 10 with 9-21 MeV/nuc


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AC_K0_SWE
Description
SWEPAM - Solar Wind Electron Proton Alpha Monitor 
References: http://www.srl.caltech.edu/ACE/ 
ACE browse data is designed for monitoring large scale particle and field 
behavior and for selecting interesting time periods. The data is automatically 
generated from the spacecraft data stream using simple algorithms provided by 
the instrument teams. It is not routinely checked for accuracy and is subject 
to revision. Use this data at your own risk, and consult with the appropriate 
instrument teams about citing it. 
SWEPAM Browse data is not validated by the experimenters and should not be used 
except for preliminary examination prior to detailed studies.


Modification History
Initial Release 12/01/98


Variable Notes

[PRELIMINARY VALUES - BROWSE USE ONLY] Solar Wind Proton Number Density, scalar
Np is the proton number density in units of cm-3, as calculated by integrating
the ion distribution function.
[PRELIMINARY VALUES - BROWSE USE ONLY] Solar Wind Bulk Speed
Vp is the solar wind proton speed, or more generally just the solar wind (bulk)
speed. It is obtained by integrating the ion (proton) distribution function.
[PRELIMINARY VALUES - BROWSE USE ONLY] Percent of Helium++ ions to protons
He_ratio is the ratio of the number density of helium++ ions to the number
density of protons.
[PRELIMINARY VALUES - BROWSE USE ONLY] radial component of the proton temperature
The radial component of the proton temperature is the (1,1) component of the
temperature tensor, along the radial direction. It is obtained by integration of
the ion (proton) distribution function.


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AC_K1_MFI
Description
MAG - ACE Magnetic Field Experiment
References: http:// www.srl.caltech.edu/ACE/  



ACE browse data is designed for monitoring large scale particle and field 
behavior and for selecting interesting time periods. The data is automatically 
generated from the spacecraft data stream using simple algorithms provided by 
the instrument teams. It is not routinely checked for accuracy and is subject 
to revision. Use this data at your own risk, and consult with the appropriate 
instrument teams about citing it. 
MAG Browse data is not validated by the experimenters and should not be used 
except for preliminary examination prior to detailed studies.


Modification History
Initial Release 11/10/98




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AC_K1_SWE
Description
SWEPAM - Solar Wind Electron Proton Alpha Monitor 
References: http://www.srl.caltech.edu/ACE/ 
ACE browse data is designed for monitoring large scale particle and field 
behavior and for selecting interesting time periods. The data is automatically 
generated from the spacecraft data stream using simple algorithms provided by 
the instrument teams. It is not routinely checked for accuracy and is subject 
to revision. Use this data at your own risk, and consult with the appropriate 
instrument teams about citing it. 
SWEPAM Browse data is not validated by the experimenters and should not be used 
except for preliminary examination prior to detailed studies.


Modification History
Initial Release 12/01/98


Variable Notes

[PRELIMINARY VALUES - BROWSE USE ONLY] Solar Wind Proton Number Density, scalar
Np is the proton number density in units of cm-3, as calculated by integrating
the ion distribution function.
[PRELIMINARY VALUES - BROWSE USE ONLY] Solar Wind Bulk Speed
Vp is the solar wind proton speed, or more generally just the solar wind (bulk)
speed. It is obtained by integrating the ion (proton) distribution function.
[PRELIMINARY VALUES - BROWSE USE ONLY] Percent of Helium++ ions to protons
He_ratio is the ratio of the number density of helium++ ions to the number
density of protons.
[PRELIMINARY VALUES - BROWSE USE ONLY] radial component of the proton temperature
The radial component of the proton temperature is the (1,1) component of the
temperature tensor, along the radial direction. It is obtained by integration of
the ion (proton) distribution function.


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AC_K2_MFI
Description
MAG - ACE Magnetic Field Experiment
References: http://www.srl.caltech.edu/ACE/  



ACE browse data is designed for monitoring large scale particle and field 
behavior and for selecting interesting time periods. The data is automatically 
generated from the spacecraft data stream using simple algorithms provided by 
the instrument teams. It is not routinely checked for accuracy and is subject 
to revision. Use this data at your own risk, and consult with the appropriate 
instrument teams about citing it. 
MAG Browse data is not validated by the experimenters and should not be used 
except for preliminary examination prior to detailed studies.


Modification History
Initial Release 11/10/98




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AC_OR_SSC
Description
GROUP 1    Satellite   Resolution   Factor
            ace           720         1
                                          
                                          
           Start Time           Stop Time 
           1999   1 00:00       1999   2 23:60   
                                          
                                          
Coord/            Min/Max   Range Filter       Filter
Component   Output Markers  Minimum  Maximum   Mins/Maxes 
GSE X        YES      -        -        -           -        -           -   
GSE Y        YES      -        -        -           -        -           -   
GSE Z        YES      -        -        -           -        -           -   
GSE Lat      YES      -        -        -           -        -           -   
GSE Lon      YES      -        -        -           -        -           -   
                                          
                                          
Addtnl             Min/Max   Range Filter       Filter
Options     Output Markers  Minimum  Maximum   Mins/Maxes
dEarth       YES      -        -        -           -   
                                          
                                          
Formats and units:                          
    Day/Time format: YYYY DDD HH:MM
    Degrees/Hemisphere format: Decimal degrees with 2 place(s).
        Longitude 0 to 360, latitude -90 to 90.
    Distance format: Kilometers with 2 place(s).


Modification History
Originated 03/14/96




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C1_JP_PMP
Description
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
JSOC predicted magnetic positions.




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C1_JP_PSE
Description
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)
AP _ Apogee
CY 1 Start of visibility window at Canberra (5 deg elevation)
CY 2 Start of visibility window at Canberra (5 deg elevation)
CY 3 Start of visibility window at Canberra (5 deg elevation)
CZ 1 End of visibility window at Canberra (5 deg elevation)
CZ 2 End of visibility window at Canberra (5 deg elevation)
CZ 3 End of visibility window at Canberra (5 deg elevation)
CZ 4 End of visibility window at Canberra (5 deg elevation)
DY 1 Start of visibility window at Vilspa (5 deg elevation)
DY 2 Start of visibility window at Vilspa (5 deg elevation)
DY 3 Start of visibility window at Vilspa (5 deg elevation)
DY 4 Start of visibility window at Vilspa (5 deg elevation)
DY 5 Start of visibility window at Vilspa (5 deg elevation)
DZ 1 End of visibility window at Vilspa (5 deg elevation)
DZ 2 End of visibility window at Vilspa (5 deg elevation)
DZ 3 End of visibility window at Vilspa (5 deg elevation)
DZ 4 End of visibility window at Vilspa (5 deg elevation)
GY 1 Start of visibility window at Goldstone (5 deg elevation)
GY 2 Start of visibility window at Goldstone (5 deg elevation)
GY 3 Start of visibility window at Goldstone (5 deg elevation)
GY 4 Start of visibility window at Goldstone (5 deg elevation)
GZ 1 End of visibility window at Goldstone (5 deg elevation)
GZ 2 End of visibility window at Goldstone (5 deg elevation)
GZ 3 End of visibility window at Goldstone (5 deg elevation)
JY 1 Start of visibility window at Maspalomas (5 deg elevation)
JY 2 Start of visibility window at Maspalomas (5 deg elevation)
JY 3 Start of visibility window at Maspalomas (5 deg elevation)
JY 4 Start of visibility window at Maspalomas (5 deg elevation)
JZ 1 End of visibility window at Maspalomas (5 deg elevation)
JZ 2 End of visibility window at Maspalomas (5 deg elevation)
JZ 3 End of visibility window at Maspalomas (5 deg elevation)
KA 1 Start of visibility window at Kourou (5 deg elevation)
KA 2 Start of visibility window at Kourou (5 deg elevation)
KA 3 Start of visibility window at Kourou (5 deg elevation)
KA 4 Start of visibility window at Kourou (5 deg elevation)
KL 1 End of visibility window at Kourou (5 deg elevation)
KL 2 End of visibility window at Kourou (5 deg elevation)
KL 3 End of visibility window at Kourou (5 deg elevation)
KL 4 End of visibility window at Kourou (5 deg elevation)
MY 1 Start of visibility window at Madrid (5 deg elevation)
MY 2 Start of visibility window at Madrid (5 deg elevation)
MY 3 Start of visibility window at Madrid (5 deg elevation)
MY 4 Start of visibility window at Madrid (5 deg elevation)
MZ 1 End of visibility window at Madrid (5 deg elevation)
MZ 2 End of visibility window at Madrid (5 deg elevation)
MZ 3 End of visibility window at Madrid (5 deg elevation)
NS S Southbound neutral sheet
NT I Enter north tail lobe from inner magnetosphere
PA 1 Start of visibility window at Perth (5 deg elevation)
PA 2 Start of visibility window at Perth (5 deg elevation)
PA 3 Start of visibility window at Perth (5 deg elevation)
PA 4 Start of visibility window at Perth (5 deg elevation)
PE _ Perigee
PL 1 End of visibility window at Perth (5 deg elevation)
PL 2 End of visibility window at Perth (5 deg elevation)
PL 3 End of visibility window at Perth (5 deg elevation)
PL 4 End of visibility window at Perth (5 deg elevation)
PL 5 End of visibility window at Perth (5 deg elevation)
QL I Inbound critical L value for auroral zone
QL O Outbound critical L value for auroral zone
RA 1 Start of visibility window at Redu (5 deg elevation)
RA 2 Start of visibility window at Redu (5 deg elevation)
RA 3 Start of visibility window at Redu (5 deg elevation)
RA 4 Start of visibility window at Redu (5 deg elevation)
RL 1 End of visibility window at Redu (5 deg elevation)
RL 2 End of visibility window at Redu (5 deg elevation)
RL 3 End of visibility window at Redu (5 deg elevation)
RL 4 End of visibility window at Redu (5 deg elevation)
RL 5 End of visibility window at Redu (5 deg elevation)
ST O Leave south tail lobe for inner magnetosphere
TL I Inbound radiation belt entry for WEC
TL O Outbound radiation belt exit for WEC
VL I Inbound critical L value for EDI
VL O Outbound critical L value for EDI
XL I Inbound critical L value for PEACE
XL O Outbound critical L value for PEACE
YL I Inbound critical L value for RAPID
YL O Outbound critical L value for RAPID
ZL I Inbound critical L value for CIS
ZL O Outbound critical L value for CIS


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
IGRF2000 pole used to calculate GSM latitude and MLT 
 in PSE files produced after 25 June 2001.


Caveats
JSOC predicted scientific events.




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C1_PP_ASP
Description
K. Torkar et al, Active spacecraft potential control for Cluster -
implementation and first results
Ann. Geophys., 19,  pp 1289 - 1302, 2001)


Modification History
none
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats




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C1_PP_CIS
Description
H. Reme et al, First multispacecraft ion measurements in and near 
the Earth's magnetosphere with the identical 
Cluster Ion Spectrometry (CIS) experiment
Annales Geophysicae, 19, pp 1303 - 1354, 2001


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
CIS not commissioned on this spacecraft.




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C1_PP_DWP
Description
L. J. C. Woolliscroft et al, The Digital Wave-Processing Experiment on Cluster
Space Sci. Rev., 79,  pp 209 - 231, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
Refer to the PI or NDC for access to ongoing caveat information
Use correlator data with caution




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C1_PP_EDI
Description
G. Paschmann et al, The Electron Drift Instrument for Cluster
Space Sci. Rev., 79,  pp 233 - 269, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
 
1) EDI's automated analysis algorithm has a known susceptibility to
producing occasional incorrect values of the drift velocities (and electric
fields). The code attempts to prevent these bad values to be output
to the cdf file. No further removal is done in the validation process.
2) When drift velocities become sufficiently large, there can be a
180-degree ambiguity in drift direction that is usually flagged in bit 7
(counting from 0) of Status Byte 3.
3) There are two methods to ananlyze a spin's worth of EDI data. If bits 5 
6 in Status Byte 3 are NOT set, the employed method was triangulation. If
either bit 5 or 6 are set, then the results are from time-of-flight
analysis.
4) The reported drift velocities and electric field refer to inertial
coordinates, i.e., have been corrected for spacecraft velocity. However, the
magnitude errors (in %) and the angle errors (in degrees), reported in
Status Bytes 5 & 6, respectively, refer to the spacecraft frame and have NOT
yet been converted to inertial coordinates.
5) The reduced chi-square reported as a data word is a measure of the
goodness-of-fit of the triangulation analysis.




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C1_PP_EFW
Description
G. Gustafsson et al, The Electric Field and Wave Experiment for Cluster
Space Sci. Rev., 79,  pp 137 - 156, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Data calibration may be unreliable at this early stage of the mission


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
*** CSDS data are not for publication ***
Be aware that data may be reprocessed as necessary to improve quality
For questions on data validity please contact sdc-adm@plasma.kth.se
Fill value inserted for U_probe_sc__C1_PP_EFW: No reason given
for time range 2002-01-07T17:50:00Z to 2002-01-10T18:18:00Z
Fill value inserted for E_dusk__C1_PP_EFW: No reason given
for time range 2002-01-10T18:15:00Z to 2002-01-10T18:18:00Z
Fill value inserted for E_pow_f1__C1_PP_EFW: No reason given
for time range 2002-01-10T18:15:00Z to 2002-01-10T18:18:00Z
Fill value inserted for E_pow_f2__C1_PP_EFW: No reason given
for time range 2002-01-10T18:15:00Z to 2002-01-10T18:18:00Z
Fill value inserted for E_sigma__C1_PP_EFW: No reason given
for time range 2002-01-10T18:15:00Z to 2002-01-10T18:18:00Z




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C1_PP_FGM
Description
A. Balogh et al, The Cluster Magnetic Field Investigation
Space Sci. Rev., 79,  pp 65 - 92, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
*** CAUTION Preliminary calibrations used: not for publication ***




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C1_PP_PEA
Description
A. D. Johnstone et al, Peace, A Plasma Electron and Current Experiment
Space Sci. Rev., 79,  pp 351 - 398, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
LEEA
HEEA
Polar
Azimuth
Refer to the PI or NDC for access to ongoing caveat information
Dr Andrew Fazakerley > MSSL > anf@mssl.ucl.ac.uk
***************************************************************
*** UNVALIDATED - Data has not been validated by PI team    ***
*** Moments use first flight update of calibration factors  ***
*** Moments are calculated from HEEA only                   ***
*** Beware switch on/off (first/last few minutes of data)   ***
---------------------------------------------------------------




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C1_PP_RAP
Description
B. Wilken et al, RAPID, The Imaging Energetic Particle Spectrometer on Cluster
Space Sci. Rev., 79,  pp 399 - 473, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
RAPID Data produced with best-effort general calibration files.
Expert IIMS calibration: with approx. inter-SC factors.
The results are not to be considered final.
Energy threshold corrections have been applied.
Background count rates have been subtracted.
Removed background count rates are zero.




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C1_PP_STA
Description
N. Cornilleau et al,
The Cluster Spatio-Temporal Analysis of Field Fluctuations (Staff) Experiment
Space Sci. Rev., 79,  pp 107 - 136, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats




Back to Top
C1_PP_WHI
Description
P. M. E. Decreau et al, WHISPER, A Resonance Sounder and Wave Analyser:
Performances and Perspectives for the Cluster Mission
Space Sci. Rev., 79,  pp 157 - 193, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
Two types of parameters are provided by WHISPER:
1) Density values (and quality): N_e_res and N_e_res_q, are related to sounding
operations.
The N_e_res value is calculated from an algorithm for resonance recognition,
which cannot take account of all level of information available to the
experimenter. The reliability of N_e_res parameters derived at the CSDS level
is thus limited in an unknown manner.
The N_e_res_q parameter (one value for each N_e_res data point) provides a crude
idea of the probability that the N_e_res value is actually correct. A value of
0 means that the value is probably wrong, a value above 80 that it is probably
correct. Anything in between reflects a crude evaluation of the chances. Refer
to PI for details.
2) Wave power values: E_pow_f4, E_pow_f5, E_pow_f6, E_pow_su and E_var_ts, are
related to recording of natural wave emissions.
Those parameters, not affected by variations in instrument's transfer functions,
are globally OK.
However, two factors can affect the precision of the measurements:
a) the occasional presence of spurious emissions created by operations of the
EDI instrument increases the wave power values measured on SC1, SC2 and SC3,
from an unknown amount,
b) the limited dynamical range of the instrument leads to an underestimation of
the E_pow parameters values when the voltage difference measured by the double
sphere antenna signal in the 2 - 80 kHz band is higher than 150 mVp or 600 mVp
(depending of the gain chosen). As a consequence, high values have to be taken
with special caution.




Back to Top
C2_JP_PMP
Description
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
JSOC predicted magnetic positions.




Back to Top
C2_JP_PSE
Description
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)
AP _ Apogee
CY 1 Start of visibility window at Canberra (5 deg elevation)
CY 2 Start of visibility window at Canberra (5 deg elevation)
CY 3 Start of visibility window at Canberra (5 deg elevation)
CZ 1 End of visibility window at Canberra (5 deg elevation)
CZ 2 End of visibility window at Canberra (5 deg elevation)
CZ 3 End of visibility window at Canberra (5 deg elevation)
CZ 4 End of visibility window at Canberra (5 deg elevation)
DY 1 Start of visibility window at Vilspa (5 deg elevation)
DY 2 Start of visibility window at Vilspa (5 deg elevation)
DY 3 Start of visibility window at Vilspa (5 deg elevation)
DY 4 Start of visibility window at Vilspa (5 deg elevation)
DZ 1 End of visibility window at Vilspa (5 deg elevation)
DZ 2 End of visibility window at Vilspa (5 deg elevation)
DZ 3 End of visibility window at Vilspa (5 deg elevation)
GY 1 Start of visibility window at Goldstone (5 deg elevation)
GY 2 Start of visibility window at Goldstone (5 deg elevation)
GY 3 Start of visibility window at Goldstone (5 deg elevation)
GY 4 Start of visibility window at Goldstone (5 deg elevation)
GZ 1 End of visibility window at Goldstone (5 deg elevation)
GZ 2 End of visibility window at Goldstone (5 deg elevation)
GZ 3 End of visibility window at Goldstone (5 deg elevation)
JY 1 Start of visibility window at Maspalomas (5 deg elevation)
JY 2 Start of visibility window at Maspalomas (5 deg elevation)
JY 3 Start of visibility window at Maspalomas (5 deg elevation)
JY 4 Start of visibility window at Maspalomas (5 deg elevation)
JZ 1 End of visibility window at Maspalomas (5 deg elevation)
JZ 2 End of visibility window at Maspalomas (5 deg elevation)
JZ 3 End of visibility window at Maspalomas (5 deg elevation)
KA 1 Start of visibility window at Kourou (5 deg elevation)
KA 2 Start of visibility window at Kourou (5 deg elevation)
KA 3 Start of visibility window at Kourou (5 deg elevation)
KA 4 Start of visibility window at Kourou (5 deg elevation)
KL 1 End of visibility window at Kourou (5 deg elevation)
KL 2 End of visibility window at Kourou (5 deg elevation)
KL 3 End of visibility window at Kourou (5 deg elevation)
KL 4 End of visibility window at Kourou (5 deg elevation)
MY 1 Start of visibility window at Madrid (5 deg elevation)
MY 2 Start of visibility window at Madrid (5 deg elevation)
MY 3 Start of visibility window at Madrid (5 deg elevation)
MY 4 Start of visibility window at Madrid (5 deg elevation)
MZ 1 End of visibility window at Madrid (5 deg elevation)
MZ 2 End of visibility window at Madrid (5 deg elevation)
MZ 3 End of visibility window at Madrid (5 deg elevation)
NS S Southbound neutral sheet
NT I Enter north tail lobe from inner magnetosphere
PA 1 Start of visibility window at Perth (5 deg elevation)
PA 2 Start of visibility window at Perth (5 deg elevation)
PA 3 Start of visibility window at Perth (5 deg elevation)
PE _ Perigee
PL 1 End of visibility window at Perth (5 deg elevation)
PL 2 End of visibility window at Perth (5 deg elevation)
PL 3 End of visibility window at Perth (5 deg elevation)
PL 4 End of visibility window at Perth (5 deg elevation)
QL I Inbound critical L value for auroral zone
QL O Outbound critical L value for auroral zone
RA 1 Start of visibility window at Redu (5 deg elevation)
RA 2 Start of visibility window at Redu (5 deg elevation)
RA 3 Start of visibility window at Redu (5 deg elevation)
RA 4 Start of visibility window at Redu (5 deg elevation)
RL 1 End of visibility window at Redu (5 deg elevation)
RL 2 End of visibility window at Redu (5 deg elevation)
RL 3 End of visibility window at Redu (5 deg elevation)
RL 4 End of visibility window at Redu (5 deg elevation)
ST O Leave south tail lobe for inner magnetosphere
TL I Inbound radiation belt entry for WEC
TL O Outbound radiation belt exit for WEC
VL I Inbound critical L value for EDI
VL O Outbound critical L value for EDI
WL I Inbound critical L value for ASPOC
WL O Outbound critical L value for ASPOC
XL I Inbound critical L value for PEACE
XL O Outbound critical L value for PEACE
YL I Inbound critical L value for RAPID
YL O Outbound critical L value for RAPID
ZL I Inbound critical L value for CIS
ZL O Outbound critical L value for CIS


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
IGRF2000 pole used to calculate GSM latitude and MLT 
 in PSE files produced after 25 June 2001.


Caveats
JSOC predicted scientific events.




Back to Top
C2_PP_ASP
Description
K. Torkar et al, Active spacecraft potential control for Cluster -
implementation and first results
Ann. Geophys., 19,  pp 1289 - 1302, 2001)


Modification History
none
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
One raw data format (5.15 seconds) of bad data may occur
when the instrument is powered on.




Back to Top
C2_PP_CIS
Description
H. Reme et al, First multispacecraft ion measurements in and near 
the Earth's magnetosphere with the identical 
Cluster Ion Spectrometry (CIS) experiment
Annales Geophysicae, 19, pp 1303 - 1354, 2001


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
CIS Switched-OFF on this s/c.




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C2_PP_DWP
Description
L. J. C. Woolliscroft et al, The Digital Wave-Processing Experiment on Cluster
Space Sci. Rev., 79,  pp 209 - 231, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
Refer to the PI or NDC for access to ongoing caveat information
Use correlator data with caution




Back to Top
C2_PP_EDI
Description
G. Paschmann et al, The Electron Drift Instrument for Cluster
Space Sci. Rev., 79,  pp 233 - 269, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
 
1) EDI's automated analysis algorithm has a known susceptibility to
producing occasional incorrect values of the drift velocities (and electric
fields). The code attempts to prevent these bad values to be output
to the cdf file. No further removal is done in the validation process.
2) When drift velocities become sufficiently large, there can be a
180-degree ambiguity in drift direction that is usually flagged in bit 7
(counting from 0) of Status Byte 3.
3) There are two methods to ananlyze a spin's worth of EDI data. If bits 5 
6 in Status Byte 3 are NOT set, the employed method was triangulation. If
either bit 5 or 6 are set, then the results are from time-of-flight
analysis.
4) The reported drift velocities and electric field refer to inertial
coordinates, i.e., have been corrected for spacecraft velocity. However, the
magnitude errors (in %) and the angle errors (in degrees), reported in
Status Bytes 5 & 6, respectively, refer to the spacecraft frame and have NOT
yet been converted to inertial coordinates.
5) The reduced chi-square reported as a data word is a measure of the
goodness-of-fit of the triangulation analysis.




Back to Top
C2_PP_EFW
Description
G. Gustafsson et al, The Electric Field and Wave Experiment for Cluster
Space Sci. Rev., 79,  pp 137 - 156, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Data calibration may be unreliable at this early stage of the mission


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
*** CSDS data are not for publication ***
Be aware that data may be reprocessed as necessary to improve quality
For questions on data validity please contact sdc-adm@plasma.kth.se




Back to Top
C2_PP_FGM
Description
A. Balogh et al, The Cluster Magnetic Field Investigation
Space Sci. Rev., 79,  pp 65 - 92, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
*** CAUTION Preliminary calibrations used: not for publication ***




Back to Top
C2_PP_PEA
Description
A. D. Johnstone et al, Peace, A Plasma Electron and Current Experiment
Space Sci. Rev., 79,  pp 351 - 398, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
LEEA
HEEA
Polar
Azimuth
Refer to the PI or NDC for access to ongoing caveat information
Dr Andrew Fazakerley > MSSL > anf@mssl.ucl.ac.uk
***************************************************************
*** UNVALIDATED - Data has not been validated by PI team    ***
*** Moments use first flight update of calibration factors  ***
*** Moments are calculated from HEEA only                   ***
*** Beware switch on/off (first/last few minutes of data)   ***
---------------------------------------------------------------




Back to Top
C2_PP_RAP
Description
B. Wilken et al, RAPID, The Imaging Energetic Particle Spectrometer on Cluster
Space Sci. Rev., 79,  pp 399 - 473, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
RAPID Data produced with best-effort general calibration files.
Expert IIMS calibration: with approx. inter-SC factors.
The results are not to be considered final.
Central ion head not functioning, no sensitivity near ecliptic.
Energy threshold corrections have been applied.
Background count rates have been subtracted.
Removed background count rates are zero.




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C2_PP_STA
Description
N. Cornilleau et al,
The Cluster Spatio-Temporal Analysis of Field Fluctuations (Staff) Experiment
Space Sci. Rev., 79,  pp 107 - 136, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats




Back to Top
C2_PP_WHI
Description
P. M. E. Decreau et al, WHISPER, A Resonance Sounder and Wave Analyser:
Performances and Perspectives for the Cluster Mission
Space Sci. Rev., 79,  pp 157 - 193, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
Two types of parameters are provided by WHISPER:
1) Density values (and quality): N_e_res and N_e_res_q, are related to sounding
operations.
The N_e_res value is calculated from an algorithm for resonance recognition,
which cannot take account of all level of information available to the
experimenter. The reliability of N_e_res parameters derived at the CSDS level
is thus limited in an unknown manner.
The N_e_res_q parameter (one value for each N_e_res data point) provides a crude
idea of the probability that the N_e_res value is actually correct. A value of
0 means that the value is probably wrong, a value above 80 that it is probably
correct. Anything in between reflects a crude evaluation of the chances. Refer
to PI for details.
2) Wave power values: E_pow_f4, E_pow_f5, E_pow_f6, E_pow_su and E_var_ts, are
related to recording of natural wave emissions.
Those parameters, not affected by variations in instrument's transfer functions,
are globally OK.
However, two factors can affect the precision of the measurements:
a) the occasional presence of spurious emissions created by operations of the
EDI instrument increases the wave power values measured on SC1, SC2 and SC3,
from an unknown amount,
b) the limited dynamical range of the instrument leads to an underestimation of
the E_pow parameters values when the voltage difference measured by the double
sphere antenna signal in the 2 - 80 kHz band is higher than 150 mVp or 600 mVp
(depending of the gain chosen). As a consequence, high values have to be taken
with special caution.




Back to Top
C3_JP_PMP
Description
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
JSOC predicted magnetic positions.




Back to Top
C3_JP_PSE
Description
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)
AP _ Apogee
CY 1 Start of visibility window at Canberra (5 deg elevation)
CY 2 Start of visibility window at Canberra (5 deg elevation)
CY 3 Start of visibility window at Canberra (5 deg elevation)
CZ 1 End of visibility window at Canberra (5 deg elevation)
CZ 2 End of visibility window at Canberra (5 deg elevation)
CZ 3 End of visibility window at Canberra (5 deg elevation)
CZ 4 End of visibility window at Canberra (5 deg elevation)
DY 1 Start of visibility window at Vilspa (5 deg elevation)
DY 2 Start of visibility window at Vilspa (5 deg elevation)
DY 3 Start of visibility window at Vilspa (5 deg elevation)
DZ 1 End of visibility window at Vilspa (5 deg elevation)
DZ 2 End of visibility window at Vilspa (5 deg elevation)
DZ 3 End of visibility window at Vilspa (5 deg elevation)
GY 1 Start of visibility window at Goldstone (5 deg elevation)
GY 2 Start of visibility window at Goldstone (5 deg elevation)
GY 3 Start of visibility window at Goldstone (5 deg elevation)
GY 4 Start of visibility window at Goldstone (5 deg elevation)
GZ 1 End of visibility window at Goldstone (5 deg elevation)
GZ 2 End of visibility window at Goldstone (5 deg elevation)
GZ 3 End of visibility window at Goldstone (5 deg elevation)
JY 1 Start of visibility window at Maspalomas (5 deg elevation)
JY 2 Start of visibility window at Maspalomas (5 deg elevation)
JY 3 Start of visibility window at Maspalomas (5 deg elevation)
JY 4 Start of visibility window at Maspalomas (5 deg elevation)
JZ 1 End of visibility window at Maspalomas (5 deg elevation)
JZ 2 End of visibility window at Maspalomas (5 deg elevation)
JZ 3 End of visibility window at Maspalomas (5 deg elevation)
KA 1 Start of visibility window at Kourou (5 deg elevation)
KA 2 Start of visibility window at Kourou (5 deg elevation)
KA 3 Start of visibility window at Kourou (5 deg elevation)
KA 4 Start of visibility window at Kourou (5 deg elevation)
KL 1 End of visibility window at Kourou (5 deg elevation)
KL 2 End of visibility window at Kourou (5 deg elevation)
KL 3 End of visibility window at Kourou (5 deg elevation)
KL 4 End of visibility window at Kourou (5 deg elevation)
MY 1 Start of visibility window at Madrid (5 deg elevation)
MY 2 Start of visibility window at Madrid (5 deg elevation)
MY 3 Start of visibility window at Madrid (5 deg elevation)
MY 4 Start of visibility window at Madrid (5 deg elevation)
MZ 1 End of visibility window at Madrid (5 deg elevation)
MZ 2 End of visibility window at Madrid (5 deg elevation)
MZ 3 End of visibility window at Madrid (5 deg elevation)
NS S Southbound neutral sheet
NT I Enter north tail lobe from inner magnetosphere
PA 1 Start of visibility window at Perth (5 deg elevation)
PA 2 Start of visibility window at Perth (5 deg elevation)
PA 3 Start of visibility window at Perth (5 deg elevation)
PE _ Perigee
PL 1 End of visibility window at Perth (5 deg elevation)
PL 2 End of visibility window at Perth (5 deg elevation)
PL 3 End of visibility window at Perth (5 deg elevation)
PL 4 End of visibility window at Perth (5 deg elevation)
QL I Inbound critical L value for auroral zone
QL O Outbound critical L value for auroral zone
RA 1 Start of visibility window at Redu (5 deg elevation)
RA 2 Start of visibility window at Redu (5 deg elevation)
RA 3 Start of visibility window at Redu (5 deg elevation)
RA 4 Start of visibility window at Redu (5 deg elevation)
RL 1 End of visibility window at Redu (5 deg elevation)
RL 2 End of visibility window at Redu (5 deg elevation)
RL 3 End of visibility window at Redu (5 deg elevation)
ST O Leave south tail lobe for inner magnetosphere
TL I Inbound radiation belt entry for WEC
TL O Outbound radiation belt exit for WEC
VL I Inbound critical L value for EDI
VL O Outbound critical L value for EDI
WL I Inbound critical L value for ASPOC
WL O Outbound critical L value for ASPOC
XL I Inbound critical L value for PEACE
XL O Outbound critical L value for PEACE
YL I Inbound critical L value for RAPID
YL O Outbound critical L value for RAPID
ZL I Inbound critical L value for CIS
ZL O Outbound critical L value for CIS


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
IGRF2000 pole used to calculate GSM latitude and MLT 
 in PSE files produced after 25 June 2001.


Caveats
JSOC predicted scientific events.




Back to Top
C3_PP_ASP
Description
K. Torkar et al, Active spacecraft potential control for Cluster -
implementation and first results
Ann. Geophys., 19,  pp 1289 - 1302, 2001)


Modification History
none
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
One raw data format (5.15 seconds) of bad data may occur
when the instrument is powered on.




Back to Top
C3_PP_CIS
Description
H. Reme et al, First multispacecraft ion measurements in and near 
the Earth's magnetosphere with the identical 
Cluster Ion Spectrometry (CIS) experiment
Annales Geophysicae, 19, pp 1303 - 1354, 2001


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
CIS in PROM mode on this spacecraft.




Back to Top
C3_PP_DWP
Description
L. J. C. Woolliscroft et al, The Digital Wave-Processing Experiment on Cluster
Space Sci. Rev., 79,  pp 209 - 231, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
Refer to the PI or NDC for access to ongoing caveat information
Use correlator data with caution




Back to Top
C3_PP_EDI
Description
G. Paschmann et al, The Electron Drift Instrument for Cluster
Space Sci. Rev., 79,  pp 233 - 269, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
 
1) EDI's automated analysis algorithm has a known susceptibility to
producing occasional incorrect values of the drift velocities (and electric
fields). The code attempts to prevent these bad values to be output
to the cdf file. No further removal is done in the validation process.
2) When drift velocities become sufficiently large, there can be a
180-degree ambiguity in drift direction that is usually flagged in bit 7
(counting from 0) of Status Byte 3.
3) There are two methods to ananlyze a spin's worth of EDI data. If bits 5 
6 in Status Byte 3 are NOT set, the employed method was triangulation. If
either bit 5 or 6 are set, then the results are from time-of-flight
analysis.
4) The reported drift velocities and electric field refer to inertial
coordinates, i.e., have been corrected for spacecraft velocity. However, the
magnitude errors (in %) and the angle errors (in degrees), reported in
Status Bytes 5 & 6, respectively, refer to the spacecraft frame and have NOT
yet been converted to inertial coordinates.
5) The reduced chi-square reported as a data word is a measure of the
goodness-of-fit of the triangulation analysis.




Back to Top
C3_PP_EFW
Description
G. Gustafsson et al, The Electric Field and Wave Experiment for Cluster
Space Sci. Rev., 79,  pp 137 - 156, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Data calibration may be unreliable at this early stage of the mission


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
*** CSDS data are not for publication ***
Be aware that data may be reprocessed as necessary to improve quality
For questions on data validity please contact sdc-adm@plasma.kth.se




Back to Top
C3_PP_FGM
Description
A. Balogh et al, The Cluster Magnetic Field Investigation
Space Sci. Rev., 79,  pp 65 - 92, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
*** CAUTION Preliminary calibrations used: not for publication ***




Back to Top
C3_PP_PEA
Description
A. D. Johnstone et al, Peace, A Plasma Electron and Current Experiment
Space Sci. Rev., 79,  pp 351 - 398, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
LEEA
HEEA
Refer to the PI or NDC for access to ongoing caveat information
Dr Andrew Fazakerley > MSSL > anf@mssl.ucl.ac.uk
***************************************************************
*** UNVALIDATED - Data has not been validated by PI team    ***
*** Moments use first flight update of calibration factors  ***
*** Moments are calculated from HEEA only                   ***
*** Beware switch on/off (first/last few minutes of data)   ***
---------------------------------------------------------------




Back to Top
C3_PP_RAP
Description
B. Wilken et al, RAPID, The Imaging Energetic Particle Spectrometer on Cluster
Space Sci. Rev., 79,  pp 399 - 473, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
RAPID Data produced with best-effort general calibration files.
Expert IIMS calibration: with approx. inter-SC factors.
The results are not to be considered final.
Energy threshold corrections have been applied.
Background count rates have been subtracted.
Removed background count rates are zero.




Back to Top
C3_PP_STA
Description
N. Cornilleau et al,
The Cluster Spatio-Temporal Analysis of Field Fluctuations (Staff) Experiment
Space Sci. Rev., 79,  pp 107 - 136, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats




Back to Top
C3_PP_WHI
Description
P. M. E. Decreau et al, WHISPER, A Resonance Sounder and Wave Analyser:
Performances and Perspectives for the Cluster Mission
Space Sci. Rev., 79,  pp 157 - 193, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
Two types of parameters are provided by WHISPER:
1) Density values (and quality): N_e_res and N_e_res_q, are related to sounding
operations.
The N_e_res value is calculated from an algorithm for resonance recognition,
which cannot take account of all level of information available to the
experimenter. The reliability of N_e_res parameters derived at the CSDS level
is thus limited in an unknown manner.
The N_e_res_q parameter (one value for each N_e_res data point) provides a crude
idea of the probability that the N_e_res value is actually correct. A value of
0 means that the value is probably wrong, a value above 80 that it is probably
correct. Anything in between reflects a crude evaluation of the chances. Refer
to PI for details.
2) Wave power values: E_pow_f4, E_pow_f5, E_pow_f6, E_pow_su and E_var_ts, are
related to recording of natural wave emissions.
Those parameters, not affected by variations in instrument's transfer functions,
are globally OK.
However, two factors can affect the precision of the measurements:
a) the occasional presence of spurious emissions created by operations of the
EDI instrument increases the wave power values measured on SC1, SC2 and SC3,
from an unknown amount,
b) the limited dynamical range of the instrument leads to an underestimation of
the E_pow parameters values when the voltage difference measured by the double
sphere antenna signal in the 2 - 80 kHz band is higher than 150 mVp or 600 mVp
(depending of the gain chosen). As a consequence, high values have to be taken
with special caution.




Back to Top
C4_JP_PMP
Description
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
JSOC predicted magnetic positions.




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C4_JP_PSE
Description
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)
AP _ Apogee
CY 1 Start of visibility window at Canberra (5 deg elevation)
CY 2 Start of visibility window at Canberra (5 deg elevation)
CY 3 Start of visibility window at Canberra (5 deg elevation)
CZ 1 End of visibility window at Canberra (5 deg elevation)
CZ 2 End of visibility window at Canberra (5 deg elevation)
CZ 3 End of visibility window at Canberra (5 deg elevation)
CZ 4 End of visibility window at Canberra (5 deg elevation)
DY 1 Start of visibility window at Vilspa (5 deg elevation)
DY 2 Start of visibility window at Vilspa (5 deg elevation)
DY 3 Start of visibility window at Vilspa (5 deg elevation)
DY 4 Start of visibility window at Vilspa (5 deg elevation)
DZ 1 End of visibility window at Vilspa (5 deg elevation)
DZ 2 End of visibility window at Vilspa (5 deg elevation)
DZ 3 End of visibility window at Vilspa (5 deg elevation)
GY 1 Start of visibility window at Goldstone (5 deg elevation)
GY 2 Start of visibility window at Goldstone (5 deg elevation)
GY 3 Start of visibility window at Goldstone (5 deg elevation)
GY 4 Start of visibility window at Goldstone (5 deg elevation)
GZ 1 End of visibility window at Goldstone (5 deg elevation)
GZ 2 End of visibility window at Goldstone (5 deg elevation)
GZ 3 End of visibility window at Goldstone (5 deg elevation)
JY 1 Start of visibility window at Maspalomas (5 deg elevation)
JY 2 Start of visibility window at Maspalomas (5 deg elevation)
JY 3 Start of visibility window at Maspalomas (5 deg elevation)
JY 4 Start of visibility window at Maspalomas (5 deg elevation)
JZ 1 End of visibility window at Maspalomas (5 deg elevation)
JZ 2 End of visibility window at Maspalomas (5 deg elevation)
JZ 3 End of visibility window at Maspalomas (5 deg elevation)
KA 1 Start of visibility window at Kourou (5 deg elevation)
KA 2 Start of visibility window at Kourou (5 deg elevation)
KA 3 Start of visibility window at Kourou (5 deg elevation)
KA 4 Start of visibility window at Kourou (5 deg elevation)
KL 1 End of visibility window at Kourou (5 deg elevation)
KL 2 End of visibility window at Kourou (5 deg elevation)
KL 3 End of visibility window at Kourou (5 deg elevation)
KL 4 End of visibility window at Kourou (5 deg elevation)
MY 1 Start of visibility window at Madrid (5 deg elevation)
MY 2 Start of visibility window at Madrid (5 deg elevation)
MY 3 Start of visibility window at Madrid (5 deg elevation)
MY 4 Start of visibility window at Madrid (5 deg elevation)
MZ 1 End of visibility window at Madrid (5 deg elevation)
MZ 2 End of visibility window at Madrid (5 deg elevation)
MZ 3 End of visibility window at Madrid (5 deg elevation)
NS S Southbound neutral sheet
NT I Enter north tail lobe from inner magnetosphere
PA 1 Start of visibility window at Perth (5 deg elevation)
PA 2 Start of visibility window at Perth (5 deg elevation)
PA 3 Start of visibility window at Perth (5 deg elevation)
PA 4 Start of visibility window at Perth (5 deg elevation)
PE _ Perigee
PL 1 End of visibility window at Perth (5 deg elevation)
PL 2 End of visibility window at Perth (5 deg elevation)
PL 3 End of visibility window at Perth (5 deg elevation)
PL 4 End of visibility window at Perth (5 deg elevation)
PL 5 End of visibility window at Perth (5 deg elevation)
QL I Inbound critical L value for auroral zone
QL O Outbound critical L value for auroral zone
RA 1 Start of visibility window at Redu (5 deg elevation)
RA 2 Start of visibility window at Redu (5 deg elevation)
RA 3 Start of visibility window at Redu (5 deg elevation)
RL 1 End of visibility window at Redu (5 deg elevation)
RL 2 End of visibility window at Redu (5 deg elevation)
RL 3 End of visibility window at Redu (5 deg elevation)
ST O Leave south tail lobe for inner magnetosphere
TL I Inbound radiation belt entry for WEC
TL O Outbound radiation belt exit for WEC
VL I Inbound critical L value for EDI
VL O Outbound critical L value for EDI
WL B Outbound critical L value 2 for ASPOC
WL I Inbound critical L value for ASPOC
WL O Outbound critical L value for ASPOC
XL I Inbound critical L value for PEACE
XL O Outbound critical L value for PEACE
YL I Inbound critical L value for RAPID
YL O Outbound critical L value for RAPID
ZL I Inbound critical L value for CIS
ZL O Outbound critical L value for CIS


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
IGRF2000 pole used to calculate GSM latitude and MLT 
 in PSE files produced after 25 June 2001.


Caveats
JSOC predicted scientific events.




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C4_PP_ASP
Description
K. Torkar et al, Active spacecraft potential control for Cluster -
implementation and first results
Ann. Geophys., 19,  pp 1289 - 1302, 2001)


Modification History
none
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
One raw data format (5.15 seconds) of bad data may occur
when the instrument is powered on.




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C4_PP_CIS
Description
H. Reme et al, First multispacecraft ion measurements in and near 
the Earth's magnetosphere with the identical 
Cluster Ion Spectrometry (CIS) experiment
Annales Geophysicae, 19, pp 1303 - 1354, 2001


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
CIS2 (HIA) switched-off on this spacecraft.
Incorrect value of detector sensitivity status word.
No CODIF Moments during RPA mode.




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C4_PP_DWP
Description
L. J. C. Woolliscroft et al, The Digital Wave-Processing Experiment on Cluster
Space Sci. Rev., 79,  pp 209 - 231, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
Refer to the PI or NDC for access to ongoing caveat information
Use correlator data with caution




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C4_PP_EDI
Description
G. Paschmann et al, The Electron Drift Instrument for Cluster
Space Sci. Rev., 79,  pp 233 - 269, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Data and calibration may be unreliable


Caveats
See also `TEXT' global attr. for Caveats file location
First production run test - User beware!
The drift step AND the electric field are reported in SCS, not GSE!  This is only temporary.
No filtering using error analysis implemented yet.
No filtering WRT large magnetic field variance implemented yet
1) Contrary to the variable names, the drift velocities and the electric
field vectors are the the SCS (Spacecraft Coordinate System), not GSE!  This
is temporary.
2) EDI's automated spin-average algorithm has a known susceptibility
to producing occassional incorrect, large values of electric fields (and
drift velocities) under certain conditions.  These bad values are usually
obvious in plots of the spin-averaged data as single-spin, large spikes.
Future revisions of the software will remove these bad values.
3) The time resolution of EDI data varies between spacecraft, and with time,
due to the success of the electron-beam "tracking" algorithm.  At the time
of these data the tracking algorithm, and its use of onboard IEL data,
were still being optimized.




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C4_PP_EFW
Description
G. Gustafsson et al, The Electric Field and Wave Experiment for Cluster
Space Sci. Rev., 79,  pp 137 - 156, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Data calibration may be unreliable at this early stage of the mission


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
*** CSDS data are not for publication ***
Be aware that data may be reprocessed as necessary to improve quality
For questions on data validity please contact sdc-adm@plasma.kth.se




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C4_PP_FGM
Description
A. Balogh et al, The Cluster Magnetic Field Investigation
Space Sci. Rev., 79,  pp 65 - 92, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
*** CAUTION Preliminary calibrations used: not for publication ***




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C4_PP_PEA
Description
A. D. Johnstone et al, Peace, A Plasma Electron and Current Experiment
Space Sci. Rev., 79,  pp 351 - 398, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
LEEA
HEEA
Polar
Azimuth
Refer to the PI or NDC for access to ongoing caveat information
Dr Andrew Fazakerley > MSSL > anf@mssl.ucl.ac.uk
***************************************************************
*** UNVALIDATED - Data has not been validated by PI team    ***
*** Moments use first flight update of calibration factors  ***
*** Moments are calculated from HEEA only                   ***
*** Beware switch on/off (first/last few minutes of data)   ***
---------------------------------------------------------------




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C4_PP_RAP
Description
B. Wilken et al, RAPID, The Imaging Energetic Particle Spectrometer on Cluster
Space Sci. Rev., 79,  pp 399 - 473, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
RAPID Data produced with best-effort general calibration files.
Expert IIMS calibration: with approx. inter-SC factors.
The results are not to be considered final.
Energy threshold corrections have been applied.
Background count rates have been subtracted.
Removed background count rates are zero.




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C4_PP_STA
Description
N. Cornilleau et al,
The Cluster Spatio-Temporal Analysis of Field Fluctuations (Staff) Experiment
Space Sci. Rev., 79,  pp 107 - 136, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats




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C4_PP_WHI
Description
P. M. E. Decreau et al, WHISPER, A Resonance Sounder and Wave Analyser:
Performances and Perspectives for the Cluster Mission
Space Sci. Rev., 79,  pp 157 - 193, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
Two types of parameters are provided by WHISPER:
1) Density values (and quality): N_e_res and N_e_res_q, are related to sounding
operations.
The N_e_res value is calculated from an algorithm for resonance recognition,
which cannot take account of all level of information available to the
experimenter. The reliability of N_e_res parameters derived at the CSDS level
is thus limited in an unknown manner.
The N_e_res_q parameter (one value for each N_e_res data point) provides a crude
idea of the probability that the N_e_res value is actually correct. A value of
0 means that the value is probably wrong, a value above 80 that it is probably
correct. Anything in between reflects a crude evaluation of the chances. Refer
to PI for details.
2) Wave power values: E_pow_f4, E_pow_f5, E_pow_f6, E_pow_su and E_var_ts, are
related to recording of natural wave emissions.
Those parameters, not affected by variations in instrument's transfer functions,
are globally OK.
However, two factors can affect the precision of the measurements:
a) the occasional presence of spurious emissions created by operations of the
EDI instrument increases the wave power values measured on SC1, SC2 and SC3,
from an unknown amount,
b) the limited dynamical range of the instrument leads to an underestimation of
the E_pow parameters values when the voltage difference measured by the double
sphere antenna signal in the 2 - 80 kHz band is higher than 150 mVp or 600 mVp
(depending of the gain chosen). As a consequence, high values have to be taken
with special caution.




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CC_C9_CC00
Description
CC00 product from CDAW9 DB.
Data from all CDAW-9 events A-E


Modification History
Converted to CDAWeb Feb 2000




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CC_C9_CC01
Description
Derived from CC01 in CDAW9 DB.
Data for all CDAW9 events A-E
Spurious values were noted in some variables, particularly in the  up/down and left/right ASYM
variables.


Modification History
Converted to CDAWeb Feb 2000




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CC_C9_CC02
Description
Derived from cc02 in CDAW9. 
Data from all CDAW9 events A-E.


Modification History
Converted to CDAWeb Feb 2000




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CC_C9_CC03
Description
Derived from cc03 datasets in CDAW9.
Data from all CDAW9 events A-E.


Modification History
Converted to CDAWeb Feb 2000




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CC_C9_CC04
Description
Converted from CC04 in CDAW9 DB.
Data for all CDAW-9 Events A-E.


Modification History
Converted to CDAWeb Feb 2000




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CC_C9_CC05
Description
Derived from CC05 in CDAW9 DB.
Data from all CDAW9 events A-E.
Magnetic field vectors near perigee should be ignored, because of s/c eclipse.


Modification History
Converted to CDAWeb Feb 2000




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CC_C9_CC1H
Description
Converted from  the CDAW9 DB.
Data for all CDAW9 events A-E.
Noise reduction applied.


Modification History
Converted to CDAWeb Feb 2000




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CC_C9_CCMD
Description
Derived from the CDAW9 DB.
Data from all CDAW9 events A-E.
Dataset created by NSSDC (S. Kayser)


Modification History
Converted to CDAWeb Feb 2000




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CL_JP_PCY
Description
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
JSOC predicted Solar cycle trends.




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CL_JP_PGP
Description
M.A. Hapgood et al, The Joint Science Operations Centre,
 Space Sci. Rev. 79, 487-525 1997
For geometrical configuration parameters, p328 of Tetrahedron Geometric Factors
by P.Robert et al, in Analysis Methods for Multi-Spacecraft Data,
ed. G.Paschmann & P.Daly, pub. 1998 by the European Space Agency and
the International Space Institute, Bern.


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
IGRF2000 pole used to calculate dipole tilt and GSE-GSM 
 angle in PGP files produced after 25 June 2001.


Caveats
JSOC predicted Orbits.
 Using spacecraft C3 as reference spacecraft.




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CL_SP_ASP
Description
K. Torkar et al, Active spacecraft potential control for Cluster -
implementation and first results
Ann. Geophys., 19,  pp 1289 - 1302, 2001)


Modification History
none
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
One raw data format (5.15 seconds) of bad data may occur
when the instrument is powered on.




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CL_SP_AUX
Description
Orbital Parameters Calculated from Short Term Orbit File of RDM
For geometry configuration parameters, see p 328 of Tetrahedron Geometric Factors
by P.Robert et al, in Analysis Methods for Multi-Spacecraft Data,
ed. G.Paschmann & P.Daly, pub. 1998 by the European Space Agency and
the International Space Institute, Bern.


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats




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CL_SP_CIS
Description
H. Reme et al, First multispacecraft ion measurements in and near 
the Earth's magnetosphere with the identical 
Cluster Ion Spectrometry (CIS) experiment
Annales Geophysicae, 19, pp 1303 - 1354, 2001


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
CIS in PROM mode on this spacecraft.




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CL_SP_DWP
Description
L. J. C. Woolliscroft et al, The Digital Wave-Processing Experiment on Cluster
Space Sci. Rev., 79,  pp 209 - 231, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software
SP file for S/C Cluster 3


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
Refer to the PI or NDC for access to ongoing caveat information
Use correlator data with caution




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CL_SP_EDI
Description
G. Paschmann et al, The Electron Drift Instrument for Cluster
Space Sci. Rev., 79,  pp 233 - 269, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
 
1) EDI's automated analysis algorithm has a known susceptibility to
producing occasional incorrect values of the drift velocities (and electric
fields). The code attempts to prevent these bad values to be output
to the cdf file. No further removal is done in the validation process.
2) When drift velocities become sufficiently large, there can be a
180-degree ambiguity in drift direction that is usually flagged in bit 7
(counting from 0) of Status Byte 3.
3) There are two methods to ananlyze a spin's worth of EDI data. If bits 5 
6 in Status Byte 3 are NOT set, the employed method was triangulation. If
either bit 5 or 6 are set, then the results are from time-of-flight
analysis.
4) The reported drift velocities and electric field refer to inertial
coordinates, i.e., have been corrected for spacecraft velocity. However, the
magnitude errors (in %) and the angle errors (in degrees), reported in
Status Bytes 5 & 6, respectively, refer to the spacecraft frame and have NOT
yet been converted to inertial coordinates.
5) The reduced chi-square reported as a data word is a measure of the
goodness-of-fit of the triangulation analysis.




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CL_SP_EFW
Description
G. Gustafsson et al, The Electric Field and Wave Experiment for Cluster
Space Sci. Rev., 79,  pp 137 - 156, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Data calibration may be unreliable at this early stage of the mission


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
*** CSDS data are not for publication ***
Be aware that data may be reprocessed as necessary to improve quality
For questions on data validity please contact sdc-adm@plasma.kth.se
Fill value inserted for U_probe_sc__CL_SP_EFW: No reason given
for time range 2002-01-07T17:50:00Z to 2002-01-10T18:18:00Z




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CL_SP_FGM
Description
A. Balogh et al, The Cluster Magnetic Field Investigation
Space Sci. Rev., 79,  pp 65 - 92, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software
SP file for S/C Cluster 3


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
*** CAUTION Preliminary calibrations used: not for publication ***




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CL_SP_PEA
Description
A. D. Johnstone et al, Peace, A Plasma Electron and Current Experiment
Space Sci. Rev., 79,  pp 351 - 398, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software
SP file for S/C Cluster 3


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
LEEA
HEEA
Refer to the PI or NDC for access to ongoing caveat information
Dr Andrew Fazakerley > MSSL > anf@mssl.ucl.ac.uk
***************************************************************
*** UNVALIDATED - Data has not been validated by PI team    ***
*** Moments use first flight update of calibration factors  ***
*** Moments are calculated from HEEA only                   ***
*** Beware switch on/off (first/last few minutes of data)   ***
---------------------------------------------------------------




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CL_SP_RAP
Description
B. Wilken et al, RAPID, The Imaging Energetic Particle Spectrometer on Cluster
Space Sci. Rev., 79,  pp 399 - 473, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
RAPID Data produced with best-effort general calibration files.
Expert IIMS calibration: with approx. inter-SC factors.
The results are not to be considered final.
Energy threshold corrections have been applied.
Background count rates have been subtracted.
Removed background count rates are zero.




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CL_SP_STA
Description
N. Cornilleau et al,
The Cluster Spatio-Temporal Analysis of Field Fluctuations (Staff) Experiment
Space Sci. Rev., 79,  pp 107 - 136, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats




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CL_SP_WHI
Description
P. M. E. Decreau et al, WHISPER, A Resonance Sounder and Wave Analyser:
Performances and Perspectives for the Cluster Mission
Space Sci. Rev., 79,  pp 157 - 193, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
Two types of parameters are provided by WHISPER:
1) Density values (and quality): N_e_res and N_e_res_q, are related to sounding
operations.
The N_e_res value is calculated from an algorithm for resonance recognition,
which cannot take account of all level of information available to the
experimenter. The reliability of N_e_res parameters derived at the CSDS level
is thus limited in an unknown manner.
The N_e_res_q parameter (one value for each N_e_res data point) provides a crude
idea of the probability that the N_e_res value is actually correct. A value of
0 means that the value is probably wrong, a value above 80 that it is probably
correct. Anything in between reflects a crude evaluation of the chances. Refer
to PI for details.
2) Wave power values: E_pow_f4, E_pow_f5, E_pow_f6, E_pow_su and E_var_ts, are
related to recording of natural wave emissions.
Those parameters, not affected by variations in instrument's transfer functions,
are globally OK.
However, two factors can affect the precision of the measurements:
a) the occasional presence of spurious emissions created by operations of the
EDI instrument increases the wave power values measured on SC1, SC2 and SC3,
from an unknown amount,
b) the limited dynamical range of the instrument leads to an underestimation of
the E_pow parameters values when the voltage difference measured by the double
sphere antenna signal in the 2 - 80 kHz band is higher than 150 mVp or 600 mVp
(depending of the gain chosen). As a consequence, high values have to be taken
with special caution.




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CL_ST_ASP
Description
W. Riedler et al, Active Spacecraft Potential Control,
Space Sci. Rev., 79,  pp 271 - 302, 1997)


Modification History
none
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See also `TEXT' global attr. for Caveats file location
Commissioning data. Validated for CVP SFT
Instrument operation mode:Standby




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CL_ST_AUX
Description
Orbital Parameters Calculated from Short Term Orbit File of RDM
For geometry configuration parameters, see p 328 of Tetrahedron Geometric Factors
by P.Robert et al, in Analysis Methods for Multi-Spacecraft Data,
ed. G.Paschmann & P.Daly, pub. 1998 by the European Space Agency and
the International Space Institute, Bern.


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See also `TEXT' global attr. for Caveats file location
sc_status(3) (Spacecraft status for Samba) is unreliable between
2000-12-12T22:29:57Z and 2000-12-12T22:56:32Z - it may be 1 instead of 0




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CL_ST_CIS
Description
H. Reme et al, The Cluster Ion Spectrometry (CIS) Experiment
Space Sci. Rev., 79,  pp 303 - 350, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
 Insufficient CODIF counting statistics when density (H) < 5.0000e-03 (118 times, first at
2000-12-09T13:00:30Z)
 CODIF possibly saturated when density (H) > 2.0000e+00 (42 times, first at 2000-12-09T22:11:30Z)
 Insufficient CODIF counting statistics when density (L) < 5.0000e-03 (1 times, first at
2000-12-09T14:03:30Z)
 Insufficient HIA counting statistics when density (H) < 2.0000e-02 (421 times, first at
2000-12-09T13:02:30Z)
 Imprecise Proton Temperature (H) when < 1.0000e+00 (658 times, first at 2000-12-09T13:00:30Z)
 Imprecise Proton Temperature (L) when < 1.0000e+00 (2 times, first at 2000-12-09T14:03:30Z)
 Imprecise Hot Ion Temperature (H) when < 5.0000e+00 (650 times, first at 2000-12-09T13:02:30Z)
Preliminary Calibration Values.
Incorrect Temperature Values.
File Validated for Test Purposes Only.




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CL_ST_DWP
Description
L. J. C. Woolliscroft et al, The Digital Wave-Processing Experiment on Cluster
Space Sci. Rev., 79,  pp 209 - 231, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Test version of UKCDHF Pipeline software
SP file for S/C Cluster 3


Caveats
See also `TEXT' global attr. for Caveats file location
Refer to the PI or NDC for access to ongoing caveat information
*** COMMISSIONING DATA - Not intended for science use       ***




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CL_ST_EDI
Description
G. Paschmann et al, The Electron Drift Instrument for Cluster
Space Sci. Rev., 79,  pp 233 - 269, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Data and calibration may be unreliable


Caveats
See also `TEXT' global attr. for Caveats file location
First production run test - User beware!
The drift step AND the electric field are reported in SCS, not GSE!  This is only temporary.
No filtering using error analysis implemented yet.
No filtering WRT large magnetic field variance implemented yet
1) Contrary to the variable names, the drift velocities and the electric
field vectors are the the SCS (Spacecraft Coordinate System), not GSE!  This
is temporary.
2) EDI's automated spin-average algorithm has a known susceptibility
to producing occassional incorrect, large values of electric fields (and
drift velocities) under certain conditions.  These bad values are usually
obvious in plots of the spin-averaged data as single-spin, large spikes.
Future revisions of the software will remove these bad values.
3) The time resolution of EDI data varies between spacecraft, and with time,
due to the success of the electron-beam "tracking" algorithm.  At the time
of these data the tracking algorithm, and its use of onboard IEL data,
were still being optimized.




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CL_ST_EFW
Description
G. Gustafsson et al, The Electric Field and Wave Experiment for Cluster
Space Sci. Rev., 79,  pp 137 - 156, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Data calibration may be unreliable at this early stage of the mission


Caveats
See also `TEXT' global attr. for Caveats file location
NOTE: Preliminary, UNVERIFIED data only
Refer to the PI or NDC for access to ongoing caveat information




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CL_ST_FGM
Description
A. Balogh et al, The Cluster Magnetic Field Investigation
Space Sci. Rev., 79,  pp 65 - 92, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Test version of UKCDHF Pipeline software
SP file for S/C Cluster 3


Caveats
See also `TEXT' global attr. for Caveats file location
*** WARNING Data processing software not under configuration control ***




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CL_ST_PEA
Description
A. D. Johnstone et al, Peace, A Plasma Electron and Current Experiment
Space Sci. Rev., 79,  pp 351 - 398, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Test version of UKCDHF Pipeline software
SP file for S/C Cluster 3


Caveats
See also `TEXT' global attr. for Caveats file location
LEEA
HEEA
*** INTERFERENCE CAMPAIGN DATA - Not intended for any other use ***
*** TEST DATA - Not intended for science use                ***




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CL_ST_RAP
Description
B. Wilken et al, RAPID, The Imaging Energetic Particle Spectrometer on Cluster
Space Sci. Rev., 79,  pp 399 - 473, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Data processed on 2001-01-09T10:08:33Z


Caveats
See also `TEXT' global attr. for Caveats file location
Cluster SC 3 contains RAPID flight unit F6, a new unit for Cluster-II
These data have been produced with pre-launch s/w and calibration data.
It is likely that they will be updated after the commissioning phase.
IIMS dead time flag set   435 times
Commissioning data for SFT only; do not use otherwise




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CL_ST_STA
Description
N. Cornilleau et al,
The Cluster Spatio-Temporal Analysis of Field Fluctuations (Staff) Experiment
Space Sci. Rev., 79,  pp 107 - 136, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See also `TEXT' global attr. for Caveats file location
E_pow_f1, E_pow_f2 : Calibration doubtfull
Fill value inserted for ALL: TEST
for time range 2000-12-09T13:00:00Z to 2000-12-09T13:15:59Z




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CL_ST_WHI
Description
P. M. E. Decreau et al, WHISPER, A Resonance Sounder and Wave Analyser:
Performances and Perspectives for the Cluster Mission
Space Sci. Rev., 79,  pp 157 - 193, 1997)


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See also `TEXT' global attr. for Caveats file location
The following informations are issued from an automatic process
TBW




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CN_K0_ASI
Description
Images and intensities. 557.7nm Images binned to geodetic grid
References: 1.Rostoker, G., Samson, J.C., Creutzberg, F., Hughes, T.J.,
McDiarmid, D.R., McNamara, A.G., Vallance Jones, A., Wallis, D.D.,
Cogger, L.L.; CANOPUS - a ground based instrument array for remote sensing the 
high latitude ionosphere during the ISTP/GGS program, 
Space Sci. Rev., submitted for publication, 1993.


Modification History
Created 29-DEC-1994




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CN_K0_BARS
Description
North & East Velocity components at 336.5 EDFL long. from 64.2 to 67.0 EDFL lat.
References: 1.Rostoker, G., Samson, J.C., Creutzberg, F., Hughes, T.J.,
McDiarmid, D.R., McNamara, A.G., Vallance Jones, A., Wallis, D.D.,
Cogger, L.L.; CANOPUS - a ground based instrument array for remote sensing the 
high latitude ionosphere during the ISTP/GGS program, 
Space Sci. Rev., submitted for publication, 1993.


Modification History
Created 18-JUL-1994




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CN_K0_MARI
Description
Magnetic Field Extrema and Location
References: 1.Rostoker, G., Samson, J.C., Creutzberg, F., Hughes, T.J.,
McDiarmid, D.R., McNamara, A.G., Vallance Jones, A., Wallis, D.D.,
Cogger, L.L.; CANOPUS - a ground based instrument array for remote sensing the 
high latitude ionosphere during the ISTP/GGS program, 
Space Sci. Rev., submitted for publication, 1993.


Modification History
Created 19-AUG-1994


Variable Notes

Data quality flag, Number of sites (0-16) contributing to measurements
More sites => greater quality
Local Auroral Electrojet index, Upper bound, CU
Local equivalent to AU index, but computed from magnetic field perturbations
measured at specific stations of the CANOPUS array
Geodetic latitude of stationused to compute the local auroral electrojet index CU
Geodetic latitude of station that measured the extrema used to compute the local
auroral electrojet idex CU
Geodetic longitude of station used to compute the local auroral electrojet index CU
Geodetic longitude of station that measured the extrema used to compute the
local auroral electrojet idex CU
Local Auroral Electrojet index, Lower bound, CL
Local equivalent to AL index, but computed from magnetic field perturbations
measured at stations of the CANOPUS array
Geodetic latitude of station used to compute the local auroral electrojet index CL
Geodetic latitude of station that measured the extrema used to compute the local
auroral electrojet idex CL
Geodetic longitude of station used to compute the local auroral electrojet idex CL
Geodetic longitude of station that measured the extrema used to compute the
local auroral electrojet idex CL


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CN_K0_MPA
Description
Station Status, Merged Scaled 5577A Scans and Peak Intensity
Merged Scans>from 3 stations along constant Geodetic Long. of 265, from Lat. 46 to 67
References: 1.Rostoker, G., Samson, J.C., Creutzberg, F., Hughes, T.J.,
McDiarmid, D.R., McNamara, A.G., Vallance Jones, A., Wallis, D.D.,
Cogger, L.L.; CANOPUS - a ground based instrument array for remote sensing the 
high latitude ionosphere during the ISTP/GGS program, 
Space Sci. Rev., submitted for publication, 1993.
2.Samson, J.C., Lyons, L.R., Newell, P.T., Creutzberg, F. and 
Xu, B., Proton aurora substorm intensifications, Geophys. Res. Letters,
19, 2167, 1992. 3.Samson, J.C., Hughes, T.J., Creutzberg, F., 
Wallis, D.D., Greenwald, R.A. and Ruohoniemi, J.M.,
Observations of a detached discrete arc in association with 
field line resonances, J. Geophys. Res., 96, 15, 683, 1991.


Modification History
Created 18-DEC-1994




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CN_K1_MARI
Description
Riometer measurements and Location
References: 1.Rostoker, G., Samson, J.C., Creutzberg, F., Hughes, T.J.,
McDiarmid, D.R., McNamara, A.G., Vallance Jones, A., Wallis, D.D.,
Cogger, L.L.; CANOPUS - a ground based instrument array for remote sensing the 
high latitude ionosphere during the ISTP/GGS program, 
Space Sci. Rev., submitted for publication, 1993.


Modification History
Created 19-AUG-1994




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CT_JP_PSE
Description
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)
NS S Southbound neutral sheet
NT I Enter north tail lobe from inner magnetosphere
ST O Leave south tail lobe for inner magnetosphere


Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
IGRF2000 pole used to calculate GSM latitude and MLT 
 in PSE files produced after 25 June 2001.


Caveats
JSOC predicted scientific events.




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D1_C9_D100
Description
Data derived from the CDAW9 DB.
Data for all CDAW9 events A-E.
Data created by the Satellite Situation Center


Modification History
Converted to CDAWeb Feb 2000




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D1_C9_D103
Description
Derived from D103 in CDAW9 DB.
These South Pole UV auroral images (123-155 nm) can be best seen from within the NACS software by
selecting the Mapped Image Plot option in Graphics. Recommended settings for the parameters in this
option are: 
1.  Choose MLAT,MLT,KRAY for X,Y,Z. 2.  Choose Nearest1 algorithm and 100 gridpoints. 3.  Choose
Orthographic projection, -90 for the pole, magnification of 3,       and set MAPDATA to 10 to turn
off continent outlines. 
4.  You may change the plotted range of intensities from default values. 5.  Select times that
include the start time of the desired image. 6.  Fill in the plot Title, save_filename, Username,
etc. 
Images are 12 min apart for Events A and B, 8 or 12 min for Event C, 6 min for Event D, and 8 min
for Event E.  The geomagnetic coordinates are corrected (IGRF 1980, Gustafsson) magnetic latitude
and magnetic local time, in degrees.  
The original ungridded images are also available on the MAC, via NCSA Image.  A program is available
(9/91), to run on a Sun workstation, which displays the ungridded images, saves values of selected
points, and presents a mapped gridded image on request (geographic or geomagnetic).  
!!! The images for the last half of Event E were revised in August 1990 to fix a drift in the
location values caused by onboard nadir-determination problems. 
Discard any DE-1 Event E plots of SAI data made before 8/90.      In addition, a handful of pixels
in most images have bad coordinate values  in CDFs made before 7/92. These are unlikely to have
caused problems.


Modification History
Corrected for scan line position, pixel offset 5/92   .
Converted to CDAWeb Feb 2000.




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D1_C9_D104
Description
Derived from D104 in CDAW9 DB.
Data only for CDAW9 events A,B and D.
One-minute averages of H+ and He+ ion counts are presented in 5 degree wide bins covering a full
spin.  The pitch angle variable gives the center spin angle of the bin, with 0 deg in the direction
of the spacecraft velocity.  Times are at the start of the interval.


Modification History
Converted to CDAWeb Feb 2000




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D1_C9_D16D
Description
Derived from D16d data in CDAW9 DB.
Data for all CDAW9 Events A-E.


Modification History
Converted to CDAWeb Feb 2000




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D1_C9_D16F
Description
Derived from D16F dataset
Data for all CDAW9 events A-E.


Modification History
Converted to CDAWeb Feb 2000




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D1_C9_D1MD
Description
Derived from the D1MD dataset in CDAW9 DB.
Data for all CDAW9 events A-E.    
Orinally computed by S. Kayser


Modification History
Converted to CDAWeb Feb 2000




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DE_UV_SAI
Description
   Instrument functional description:
 
       The spin-scan auroral imagers (SAI) comprise three photometers which
   provide images of Earth at various wavelengths via interference filters
   mounted on a wheel and selected by ground command.  Two of the photometers
   provide visible wavelength images, and the third provides images at
   vacuum-ultraviolet wavelengths.
       The three photometers are mounted on the spacecraft such that their
   fields of view are separated by about 120 degrees in a plane oriented
   perpendicular to the spin axis.  Each photometer in operation collects
   one scan line during each spacecraft rotation, with an internal mirror
   stepping once per rotation to start a new scan line.
       An auroral image is a nadir-centered two-dimensional pixel array
   provided by the spacecraft rotation and the photometer's stepping mirror
   which advances the field of view 0.25 degrees once per rotation in a
   direction perpendicular to the plane of rotation.  A change in mirror-
   stepping direction signals the start of a new image.  One, two, or
   three photometers may be in operation at one time.  The images from all
   operating photometers are telemetered simultaneously with image repetition
   rates that typically vary from about 3 to 12 minutes.
       One of the three imaging photometers is equipped with filters and a
   photocathode for observations at vacuum-ultraviolet wavelengths, in
   particular emissions of the Lyman-Birge-Hopfield band of molecular
   nitrogen at about 140 to 170 nm.  Imaging at these wavelengths allows
   coverage of the auroral oval in both the dark and sunlit ionospheres.
   The filter array for the vacuum-ultraviolet imaging photometer also
   includes filters for atomic hydrogen Lyman alpha at 121.6 nm and oxygen
   lines at 130.4 and 135.6 nm.
       The full width of the fields of view of the photometers
   corresponding to a single pixel is 0.29 degrees.  An image frame
   consists of all scan lines obtained by mirror steps in one direction
   which deflect the field of view by 0.25 degrees per rotation.  The
   angular separation of two consecutive pixels in the direction of
   spacecraft rotation is about 0.23 degrees.  A full frame has 120
   scan lines or 30 degrees of width.  For routine processing the
   angular width along a scan line is 150 pixels, or about 34.5 degrees
   of length.  The frame width is occasionally adjusted to less than
   120 scan lines.
 
 
   Reference:
 
   Frank, L. A., J. D. Craven, K. L. Ackerson, M. R. English, R. H. Eather,
       and R. L. Carovillano, Global auroral imaging instrumentation for
       the Dynamics Explorer mission, Space Sci. Inst., 5, 369-393, 1981.
 
 
   Data set description:
 
       Each DE SAI UV image CDF contains all of images collected by the
   UV photometer during one day of operations.  The displayable image
   counts are in variable 3.
       Coordinates are calculated for each position of the image count array.
   These coordinates are in variables 14, 15, and 16.
       To facilitate viewing of the images, a mapping of pixel value to a
   recommended color table based on the characteristics of the selected
   filter will be included with each image.  See the description of variables
   17, 18, and 19 below.
       A relative intensity scale is provided by the uncompressed count
   table of variable 20.  Approximate intensity levels in kiloRayleighs are
   given in the intensity table of variable 21.
       Other variables provide orbit and attitude data and information about
   the selected filter and the mirror stepping direction.
 
 
 Variable descriptions:
 
  1,2. Start time
        The time assigned to an image is the start time of the initial scan
        line within a resolution of one second.
 
    3. Image counts
        Image pixel counts range from 0 to 255.  They are stored in a two-
        dimensional byte array of 121 columns by 150 rows.  Each column
        contains one scan line.  Images will generally not fill all of the
        121 columns.  When an image is displayed with row 1 at the top and
        column 1 on the left, the spacecraft spin axis is oriented to the
        left in the display, and the orbit normal vector is oriented to the
        right.
 
    4. Filter
        Twelve filters are available for ultra-violet imaging; the filter
        number, 1-12, is given here.  In addition, the peak wavelength in
        Angstroms is given for the selected filter.
 
    5. Presumed altitude of emissions
        The presumed altitude of the emissions seen in the image varies
        with the characteristics of the filter used.
 
  6,7. First and last mirror location counters (MLCs)
        The MLC range is from 28 in column 1 (leftmost) to 148 in column 121
        (rightmost).  The direction of mirror stepping motion is shown by
        comparing first and last MLCs.
 
    8. Orbit/attitude time
        Whenever possible, the approximate center time of the image is used
        for determining the orbit and attitude parameters.  If O/A data is
        not available for the center time, the closest available O/A time
        is used.
 
    9. Spacecraft position vector, GCI
 
   10. Spacecraft velocity vector, GCI
 
   11. Spacecraft spin axis unit vector, GCI
 
   12. Sun position unit vector, GCI
 
   13. Orbit normal unit vector, GCI
 
   14. Geographic longitude or right ascension
        East longitude is given for each image pixel on the Earth at the
        altitude given in variable 5.  When the pixel altitude is greater
        than the value of variable 5, the right ascension is given.
 
   15. Geographic latitude or declination
        North latitude is given for each image pixel on the Earth at the
        altitude given in variable 5.  When the pixel altitude is greater
        than the value of variable 5, the declination is given.
 
   16. Pixel altitude
        For each image pixel on the Earth, the presumed altitude of the
        emissions is used.  This is equal to the value of variable 5.  For each
        pixel off the Earth, the altitude of the line of sight is used.
 
   17. Pixel UT
        This array gives the start time for the collection of each image pixel.
 
   18. RGB color table
        This is the recommended color table to be used with the
        limits given in variables 19 and 20.
 
19,20. Low and high color mapping limits
        The low and high color limits are recommended for remapping
        the color table entries, as follows:
            For pixel values less than the low limit, use the color
                at table position 1.
            For pixel values greater than or equal to the low limit
                and less than or equal to the high limit, use the color
                at table position (pix-low)/(high-low) x 255 + 1.
            For pixel values greater than the high limit, use the color
                at table position 256.
 
   21. Expanded count table
        The image pixel counts are quasi-logarithmically compressed to the
        range 0-255.  This table gives the average of the uncompressed range
        for each compressed count value.  Table entries 1-128 correspond to
        compressed counts 0-127 respectively.  Count levels greater than
        127 are considered overflow.
 
   22. Intensity table
        For each of the twelve filters, approximate intensity levels in
        kiloRayleighs are given for each compressed count value.  Table
        entries 1-128 correspond to compressed counts 0-127 respectively.
        No count conversion data is available for count levels greater than
        127.
 
 
   Supporting software:
 
         Directions for obtaining supporting software is available on the SAI
   website at the URL .http://www-pi.physics.uiowa.edu/www/desai/software/. 
   Included is an IDL program that displays the images with the recommended
   color bar and provides approximate intensities and coordinate data for
   each pixel.


Modification History


Variable Notes

Ultraviolet Image (quasi-logarithmically compressed counts)
Image_Counts contains the displayable image in 121 columns by 150 rows of
pixels.  Most images will use 120 of the columns.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> Ultraviolet Mapped Image (quasi-logarithmically compressed counts)
Image_Counts contains the displayable image in 121 columns by 150 rows of
pixels.  Most images will use 120 of the columns.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
Geographic longitudes, or Right Ascensions
Geographic east longitude for every image pixel on the Earth, right ascension
for every pixel off the Earth
Geographic latitudes, or Declinations
Geographic north latitude for every image pixel on the Earth, declination for
every pixel off the Earth
Altitudes of pixels, km.
Presumed altitude of emissions for every pixel on the Earth, equal to the value
of the variable AltF; altitude of line of sight for every pixel off the Earth
RGB color lookup table
RGBColorTable should be remapped for displaying an image using the low and high
limits given for each image in Limit_Lo and Limit_Hi.Image_Counts count values
less than Limit_Lo use the color at table position 1.  Count values greater than
Limit_Hi use the color at table position 256.  For count values greater than or
equal to Limit_Lo and less than or equal to Limit_Hi, the table position is
(Count-Limit_Lo)/(Limit_Hi-Limit_Lo) x 255 + 1.At the selected table position C,
the color components are Red at RGBColorTable(1,C), Green at RGBColorTable(2,C),
and Blue at RGBColorTable(3,C).
Expanded count table: quasi-logarithmically uncompressed pixel counts
Image_Counts contains pixel counts which have been quasi-logarithmically
compressed by the instrument.  Approximate uncompressed value
forImage_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Compressed pixel
counts greater than 127 are considered overflow.
Approximate intensity levels in kiloRayleighs for each filter
Approximate intensity in kR for Image_Counts(i,j) is Intens_Tables(
Image_Counts(i,j)+1), Filter(1) ).  Intensities cannot be computed for image
count values greater than 127.


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DE_VS_EICS
No TEXT global attribute. 
Metadata providedby W.K. Peterson with the helpof Mona Kessel


Modification History
Created October, 1995 by W.K. Peterson
Add Q_FLAG_FILE_CORRUPTED variable to indicate intervals for which full data quality information is
not available. 10/10/95


Variable Notes

NSSDC standard-reference time value. 
Center time of 96 second accumulation intervals, starting at 0 seconds of each
UT day
Time PB5, centered
Center time of 96 second accumulation intervals, starting at 0 seconds of each
UT day
H+ number flux, at 15 energies (~0.01 to ~20keV) and 14 pitch angles (6 shown)
Negative fluxes reflect low count rates and background subtraction. The width of
lowest energy channel is variable.  Pitch angle coverage is NOT uniform. 
Conversion to velocity space density, calculations of density and other
operations involving division by a characteristic energy are limited in accuracy
by energy bands that are wide compared to the fall off of flux with energy.
Ion Energy, 15 channels ~0.01 to ~20 keV
The first (lowest) of the 15 energy channels has a variable lower limit and
center energy.  The variable Low_energy_cut_off specifies the lower limit of the
lowest energy channel. The remaining 14 energy channels have fixed lower,
center, and upper limits that are specified by DELTA_PLUS_VAR and
DELTA_MINUS_VAR Attribute E_delta. The value in this table (0.062 keV) is the
normal center energy for the lowest energy channel, i.e. when Low_energy_cut_off
= 0.01 keV.
Half of the instrumental Full EnergyWidth at Half Maximum Transmission, EXCEPT Low_energy_cut_off specifies the lower limit of the lowest energy channel. 
The first of the 15 energy channels has a variable lower limit and center
energy.   The remaining 14 energy channels have fixed lower, and upper limits
that are specified by Center_energy and the DELTA_PLUS_VAR and DELTA_MINUS_VAR
Attribute E_delta.
Pitch Angles at the center of 14 non uniformly spaced Bins. 
Variable width Pitch Angle Bins covering 0-7.5, 7.5-15, 15-30, 30-45, 45-60,
60-75 75-90, 90-105, 105-120, 120-135, 135-150, 150-165, 165-172.5, and
172.5-180 degrees.  This provides highest angular resolution along the magnetic
field direction.
ONE Standard deviation of H+ number fluxat 15 energy and 14 pitch angle bins.
Uncertainly estimated from the observed total signal counts.  The width of
lowest energy channel is variable.  Pitch angle coverage is NOT uniform.
O+ number flux, at 15 energies (~0.01 to ~20keV) and 14 pitch angles (6 shown)
Negative fluxes reflect low count rates and background subtraction. The width of
lowest energy channel is variable.  Pitch angle coverage is NOT uniform. 
Conversion to velocity space density, calculations of density and other
operations involving division by a characteristic energy are limited in accuracy
by energy bands that are wide compared to the fall off of flux with energy.
ONE Standard deviation of O+ number flux at 15 energy and 14 pitch angle bins.
Uncertainly estimated from the observed total signal counts.  The width of
lowest energy channel is variable.  Pitch angle coverage is NOT uniform.
He+ number flux, at 15 energies (~0.01 to ~20keV) and 14 pitch angles (6 shown)
Negative fluxes reflect low count rates and background subtraction. The width of
lowest energy channel is variable.  Pitch angle coverage is NOT uniform. 
Conversion to velocity space density, calculations of density and other
operations involving division by a characteristic energy are limited in accuracy
by energy bands that are wide compared to the fall off of flux with energy.
ONE Standard deviation of He+ number fluxat 15 energy and 14 pitch angle bins.
Uncertainly estimated from the observed total signal counts.  The width of
lowest energy channel is variable.  Pitch angle coverage is NOT uniform.
Background count rate interpolated to center time. scalar
Because the backgrounddoes, at times, vary rapidly on the 96 second averaging
period the background counting rate has been interpolated intime to reflect the
expected background counting rate at the center of the averaging interval.  The
ion flux may be time alised in regions of rapidly varying
INTERPOLATED_BACKGROUND.
One standard deviation of Interpolated Background. scalar
Determined from the total number ofbackground counts observed in the 96averaging
period.
Lowest Energy above the spacecraft potential accepted. scalar
The Center_energy of the lowest energy channel must be corrected for
Low_energy_cut_off above 0.015 keV
Bitwise combination of He_data,N_flag, C_flag, A_flag, Noisy_flag, Short_flag, and PA_coverage_flag. scalar
This variable is displayed as a bitwisespectrogram by the idl check_cdf.pro code
available from pete@willow.space.lockheed.com    Interpretation of Values: 0/1:
0=He+ data. 1=No He+ data 0/2: 0=NOT BCLIST N flag indicating that data are
missing or care must be taken in processing or interpreting them. 2= N flag on.
0/4: 0=NOT BCLIST C flag indicating that data in the lowest energy channel are
contaminated by extra counts from a EUV photoionization of residual gas in the
input aperture. 4=C flag on. 0/8: 0=NOT BCLIST A flag indicating that full
attitude are available in the full archived data file. Attitude data are not
required or available for the pitch angle organized data processed into the cdf
files here. 8= A flag on. 0/16: 0=Not NOISY data  Flag manually entered after
scan of summary spectrogram 16= Noisy flag on. 0/32: 0=NOT TOO SHORT. 
Interpretation of Noisy data and other problems was difficult from files
containing less than about 7 minutes of data.  This flag was manually set from
reading summary spectrograms. 32= Data interval too short.  0/64: 0=Complete
pitch angle coverage determined from visual inspection of summary spectrograms
64= Incomplete pitch angle coverage. 0/128:  See Q_FLAG_FILE_CORRUPTED variable
described below.
He+ data available flag 0=data for he+; 1=no he+ data 
He+ fluxes are available for approximately 50% of the data intervalsin this
archive.  He_data is set on a per record basis
Data valid flag 0=good; 1=Not available or use with caution
Some valid data may be included in the telemetry segment, but some of the data
in the segment are invalid and must not be includedin long term average data
sets.This is the N flag described in the EICSDATA.LIS file and other 
documentation accompanying the EICS_STAND_ALONE_TELEMETRY_FILE_SYSTEM from NSSDC
or on line on the DE project home page on the Space Physics Data System.  This
flag is set on a telemetryinterval (segment) basis.
Sun Pulse Flag0=good; 1=use data from the lowest energy channel with caution. 
Set to 1 when a visual examination of  color spectrogram showed the lowest
energy channel included a spurious count rate caused by the photoionization of
residual neutral gases in in the preacceleration region of the spectrometer as
described in Shelley et al. Geophys. Res. Lett. 9, p942, 1982. This is the C
data quality flag described in the EICSDATA.LIS file and other  documentation
accompanying the EICS_STAND_ALONE_TELEMETRY_FILE_SYSTEM from NSSDC or on line on
the DE project home page on the Space Physics Data System.
Attitude Available Flag 0: Source data CAN provide sensor orientation relative to the spacecraft velocity. 1: CAN NOT
Information variable. Does not apply to data in this CDF.  If set to 0
information about the direction of plasma motion with respect to the satellite
motion may be obtained from the the full resolution
EICS_STAND_ALONE_TELEMETRY_FILE_SYSTEM archived at NSSDC. This is the A data
quality flag described in the EICSDATA.LIS file and other  documentation
accompanying the EICS_STAND_ALONE_TELEMETRY_FILE_SYSTEM from NSSDC or on line on
the DE project home page on the Space Physics Data System.
Supplemental Data Valid Flag #1 0=good; 1= Telemetry interval contains unphysically high signal levels 
This flag is set on a telemetryinterval basis.  A visual examination of color
spectrograms indicated some 96 second dataintervals with extremely high counting
rates.  These intervals were identified by their characteristic patchyness on
energy-time and angle-time spectrograms.  Data from intervals where the
Noisy_flag=1 WERE NOT included in the large-scale statistical studies referenced
in the global attributes.Some valid data may be included in the telemetry
segment
Supplemental Data Valid Flag #2 0=good; 1=Too short to evaluate data quality. 
1 indicates that  a visual examination of color spectrograms was not possible
because the data interval was too short.  The data quality flags that depend on
visual examination are:  C_flag, A_flag, Noisy_flag, and PA_coverage_flag.
Pitch Angle Coverage Flag 0=good; 1=Incomplete PA coverage.
Data for some pitch angle ranges may contain fill indicating that the full pitch
angle range was notsampled.  This occurs when the magnetic field does not lie
within  the satellite spin plane.    The flag is set to 1 when a visual
examination of color spectrograms show that data are not available in all pitch
angle bins.  This flag is set on a telemetry segment basis.
Quality Flags Corrupted 0=OK ; 1= Information Lost
Quality flag information for DE/EICSwas created in a keyed file using
VMSspecific file management.  In the almost15 years this file has been
maintained records for some time intervals have become corrupted.  Some quality
informationcan be found in the data catalog available with the DE/EICS Stand
Alone Telemetry Files (SATF) from NSSDC
Geographic Position Altitude above the geoid, latitude and longitude. 
Values obtained from various sources.
Geomagnetic Position Magnetic local time, Invariant latitude and geomagnetic latitude. 
Values obtained from various sources.


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DMSP_R0_SSJ4
No TEXT global attribute.


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DN_K0_GBAY
Description
vlptm $Revision: 4.3


Modification History
skeleton table implemented 
new formats with all the DEPEND attrs set
ISTP KPGS Standard & Conventions version 1 implemented




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DN_K0_HANK
Description
vlptm $Revision: 4.5


Modification History
skeleton table implemented 
new formats with all the DEPEND attrs set
ISTP KPGS Standard & Conventions version 1 implemented




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DN_K0_ICEW
Description
vlptm $Revision: 4.3


Modification History
skeleton table implemented 
new formats with all the DEPEND attrs set
ISTP KPGS Standard & Conventions version 1 implemented




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DN_K0_KAPU
Description
vlptm $Revision: 4.3


Modification History
skeleton table implemented 
new formats with all the DEPEND attrs set
ISTP KPGS Standard & Conventions version 1 implemented




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DN_K0_PACE
Description
vlptm version 2.42
Ref1: Satellite Experiments Simultaneous with Antarctic Measurements (SESAME) 
to be submitted to Reviews of Geophysics (copy held by GGS group at NASA)
Ref2:Baker et al.,EOS 70,p785 1989. Ref3: Greenwald et al.,Radio Sci.20,p63 1985
Info:Keith Morrison,GGS Scientist,British AntarcticSurvey,Cambridge,CB3 0ET,UK
E-mail: 19989::MORRISON


Modification History
skeleton table implemented 
new formats with all the DEPEND attrs set
ISTP KPGS Standard & Conventions version 1 implemented




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DN_K0_PYKK
Description
vlptm $Revision: 4.5


Modification History
skeleton table implemented 
new formats with all the DEPEND attrs set
ISTP KPGS Standard & Conventions version 1 implemented




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DN_K0_SASK
Description
vlptm $Revision: 4.3


Modification History
skeleton table implemented 
new formats with all the DEPEND attrs set
ISTP KPGS Standard & Conventions version 1 implemented




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EQ_PP_3DA
Description
see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.4 3DA


Modification History
Produced in accordance with ESDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See also `TEXT' global attr. for Caveats file location




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EQ_PP_AUX
Description
see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.8 AUX


Modification History
Produced in accordance with ESDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See also `TEXT' global attr. for Caveats file location




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EQ_PP_EDI
Description
see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.2 EDI


Modification History
Produced in accordance with ESDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See also `TEXT' global attr. for Caveats file location




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EQ_PP_EPI
Description
see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.5 EPI


Modification History
Produced in accordance with ESDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See also `TEXT' global attr. for Caveats file location




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EQ_PP_ICI
Description
see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.3 ICI


Modification History
Produced in accordance with ESDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
none


Caveats
 This file has particularly bad background problems due to intense
 radiation belts after 16:00 UT.
 This file contains both onboard calculated moments (labeled 
 "raw" with an "*" in the name) and moments calculated on 
 the ground from 3D distributions (labeled "final").
 Quantitative analysis should be done with the "final" moments.  
 The raw data should only be used qualitatively for identifying
 regions and temporal variations.  It has large errors, particularly
 in Vz in spacecraft coordinates.
 O+ and He+ data should not be used in the magnetosheath or at low
 L-values, due to background problems.
 Contact the LI at Lynn.Kistler@unh.edu if the data you need
 is not available on-line.




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EQ_PP_MAM
Description
see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.1 MAM


Modification History
Produced in accordance with ESDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See also `TEXT' global attr. for Caveats file location




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EQ_PP_PCD
Description
see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.6 PCD


Modification History
Produced in accordance with ESDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See also `TEXT' global attr. for Caveats file location




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EQ_SP_3DA
Description
see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.4 3DA


Modification History
Produced in accordance with ESDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See also `TEXT' global attr. for Caveats file location




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EQ_SP_AUX
Description
see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.8 AUX


Modification History
Produced in accordance with ESDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See also `TEXT' global attr. for Caveats file location




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EQ_SP_EDI
Description
see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.2 EDI


Modification History
Produced in accordance with ESDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See also `TEXT' global attr. for Caveats file location




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EQ_SP_EPI
Description
see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.5 EPI


Modification History
Produced in accordance with ESDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See also `TEXT' global attr. for Caveats file location




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EQ_SP_ICI
Description
see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.3 ICI


Modification History
Produced in accordance with ESDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
none


Caveats
 This file has particularly bad background problems due to intense
 radiation belts after 16:00 UT.
 This file contains both onboard calculated moments (labeled 
 "raw" with an "*" in the name) and moments calculated on 
 the ground from 3D distributions (labeled "final").
 Quantitative analysis should be done with the "final" moments.  
 The raw data should only be used qualitatively for identifying
 regions and temporal variations.  It has large errors, particularly
 in Vz in spacecraft coordinates.
 O+ and He+ data should not be used in the magnetosheath or at low
 L-values, due to background problems.
 Contact the LI at Lynn.Kistler@unh.edu if the data you need
 is not available on-line.




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EQ_SP_MAM
Description
see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.1 MAM


Modification History
Produced in accordance with ESDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See also `TEXT' global attr. for Caveats file location




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EQ_SP_PCD
Description
see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.6 PCD


Modification History
Produced in accordance with ESDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See also `TEXT' global attr. for Caveats file location




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EQ_SP_SFD
Description
see EQS-MPE-EDC-01, Equator-S Data Center Manual, section 4.7 SFD


Modification History
Produced in accordance with ESDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003


Caveats
See also `TEXT' global attr. for Caveats file location




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FA_K0_ACF
Description
none yet


Modification History
none yet




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FA_K0_DCF
Description
none yet


Modification History
none yet




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FA_K0_EES
Description
Carlson et al., 1983, Adv. Space Res. 2(7), 67.
Data are derived from a pair of hemisperical electrostatic
analyzers with 180 degree radial FOVs that together form
a single 360 deg x 4.5 deg planar FOV in the spin 
spacecraft plane.  Sensors can deflect their FOV by
up to +/-10 deg to follow the magnetic field direction
which is within +/-6 deg of the spin plane for most
auroral crossings. Absolute geometric factors are the best
estimate at the time of key parameter data production
(20% uncertainty).  Key parameter data are averaged for
1 spin.  Any change in sensor configuration or onboard
data storage during a spin result in a rejection of the
spin average.
Electron Sensor Parameters:
Inner Hemisphere R = 3.75 cm
dR/R = 0.06
FOV = 360 deg x 4.5 (FWHM) deg 
Angular resolution = 11.25 deg x 4.5 deg
Energy range: 4 eV to 30 keV
dE/E = 0.15 (FWHM)
Geometric Factor = 0.0047 x E  (cm2-sr-eV)
Key Parameter Data:
Electron Energy-Time Spectrogram, 0-30 deg pitch angle
Electron Energy-Time Spectrogram, 60-120 deg pitch angle
Electron Energy-Time Spectrogram, 150-180 deg pitch angle
Electron Pitch Angle-Time Spectrogram, 0.1-1.0 keV
Electron Pitch Angle-Time Spectrogram, 1.0-30.0 keV
Electron Energy Flux mapped along B to 100 km altitude
Electron Number Flux mapped along B to 100 km altitude


Modification History
Initial version April 9, 1997




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FA_K0_IES
Description
Carlson et al., 1983, Adv. Space Res. 2(7), 67.
Data are derived from a pair of hemisperical electrostatic
analyzers with 180 degree radial FOVs that together form
a single 360 deg x 6.5 deg planar FOV in the spin 
spacecraft plane.  Sensors can deflect their FOV by
up to +/-10 deg to follow the magnetic field direction
which is within +/-6 deg of the spin plane for most
auroral crossings. Absolute geometric factors are the best
estimate at the time of key parameter data production
(20% uncertainty).  Key parameter data are averaged for
1 spin.  Any change in sensor configuration or onboard
data storage during a spin result in a rejection of the
spin average.
Ion Sensor Parameters:  
Inner Hemisphere R = 3.75 cm
dR/R = 0.075
FOV = 360 deg x 6.5 (FWHM) deg 
Angular resolution = 11.25 deg x 6.5 deg
Energy range: 3 eV to 25 keV
dE/E = 0.20 (FWHM)
Geometric Factor = 0.0136 x E  (cm2-sr-eV)
Key Parameter Data:
Ion Energy-Time Spectrogram, 0-30 deg pitch angle
Ion Energy-Time Spectrogram, 40-140 deg pitch angle
Ion Energy-Time Spectrogram, 150-180 deg pitch angle
Ion Pitch Angle-Time Spectrogram, 0.05-1.0 keV
Ion Pitch Angle-Time Spectrogram, 1.0-25.0 keV
Ion Energy Flux mapped along B to 100 km altitude
Ion Number Flux mapped along B to 100 km altitude


Modification History
Initial version April 9, 1997




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FA_K0_TMS
Description
The Time-of-Flight Energy, Angle, Mass Spectrograph 
(TEAMS) Experiment for FAST,  D. M. Klumpar, E. Moebius, 
L. M. Kistler, M. Popecki, E. G. Shelley, E. Hertzberg, 
K. Crocker, M. Granoff, Li Tang, C. W. Carlson, 
J. McFadden, B. Klecker, F. Eberl, E. Kuenneth, 
H. Kaestle, M. Ertl, W. K. Peterson, and D. Hovestadt, 
to be published, Space Science Reviews, 
D. Reidel Publishing Co., Dordrecht, Holland, 1997.
The 3-D Plasma Distribution Function Analyzers with 
Time-of-Flight Mass Discrimination for CLUSTER, FAST, 
and Equator-S, E. Moebius, L. M. Kistler, M. Popecki, 
K. Crocker, M. Granoff, Y. Jiang, E. Satori, V. Ye, 
H. Reme, J. A. Sauvaud, A. Cros, A. Aoustin, T. Camus, 
J. L. Medale, J. Rouzaud, C. W. Carlson, J. McFadden, 
D. Curtis, H. Heetdirks, J. Croyle, C. Ingraham, 
E. G. Shelley, D. M. Klumpar, E. Hertzberg, B. Klecker, 
M. Ertl, F. Eberl, H. Kaestle, E. Kuenneth, 
P. Laeverenz, E. Seidenschwang, G. Parks, M. McCarthy, 
A. Korth, B. Graeve, H. Balsiger, U. Schwab, and 
M. Steinacher, Measurement Techniques for Space Plasmas, 
J. Borovsky, R. Pfaff, D. Young, eds.,
American Geophysical Union, Washington, DC, in press, 1997.
Data are derived from a time-of-flight mass spectrograph 
that determines 3-dimensional distribution functions of 
individual ion species over the energy range 1 - 12000 eV, 
within 2.5 seconds (one-half spacecraft spin).  The 
instrument consists of a toroidal top-hat electrostatic 
analyzer with instantaneous acceptance of ions over 360 
degrees in polar angle in 16 sectors.  Ions passing 
through the electrostatic analyzer are postaccelerated by 
up to 25 kV and then analyzed for mass per charge in a 
foil-based time-of-flight analyzer.  The data used to 
construct CDF data products are derived from the Survey 
data.  Survey data consists of 
4 mass groups x 48 energies x 64 solid angle segments. 
The 4 mass groups are H+, O+, He+, and He++.  Only the 
16 equatorial angle segments are used for the CDF data set. 
Each equatorial solid angle segment contains 2 (4) samples 
at each energy in the 32 (64) sweep/spin mode.  The full 
angular range is covered in half a spin but the actual 
time resolution of the survey data product depends upon 
the telemetry mode.  In the highest TM rate modes H+ and O+ 
survey data read out every half spin.  In lowest TM rate 
mode these data are accumulated for 4 spins.  The minimum 
accumulation time included in the CDF is 1 spin, so if the 
actual accumulation time is a half spin, two data points 
are averaged.  Otherwise, the full resolution is included. 
In every mode He+ and He++ are accumulated twice as long 
as H+ and O+.  To force the H+, O+, and He+ to have an 
equal number of data points when H+ and O+ have twice the 
time resolution, each He+ data point is written twice 
consecutively in the file.


Modification History
none yet




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FM_K0_KILP
Description
Keograms are quick-look data of an all-sky camera at 
Kilpisjarvi (69.02 N, 20.79 E)  
 maintained and operated by the Finnish Meteorological Institute.
Keograms show the intensity along the middle meridian of the camera 
field-of-view as a function of time. The camera has a fish-eye lens 
of 180 degrees and narrow bandpass interference filters of wavelengths 
557.7 nm (green) and 630.0 nm (red). In standard operating mode, the sampling interval 
is 20 s and 60 s for the red and green images, respectively.
The exposure time is typically 1000 ms. The time resolution of keograms 
is 1 min and they are constructed using only the green images.
The size of a digital image is 512x512 pixels and intensity values 
vary between 0 and 255. At the altitude of 110 km the field-of-view 
(with reasonable spatial resolution) is a spherical area with the 
diameter of 600 km.  The keograms shown here are intensity versus latitude 
plots while the original keograms (available in http://www.geo.fmi.fi/MIRACLE 
are intensity versus zenith angle plots.
The conversion from zenith angle dependence to equidistant latitude grid 
causes occasionally artificial two-band structure to the keograms
(light bands below and above the darker zenith).
The artefact becomes visible especially during quiet periods, 
and the autoscaling color palette may even strengthen the effect.
Note that some keograms show also the Moon as a sphere or ellipsoid with 
very high, even saturating intensities.


Modification History
CDF created 31.05.1999 11:32:29 UTC.




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G0_K0_EP8
Description
The NOAA Geostationary Operational 
 Environmental Satellite (GOES) key
 parameters are obtained from the
 Energetic Particle Sensor (EPS)
 and the magnetometer (MAG).  The
 key parameters are a subset of the 
 data available from the GOES Space
 Environment Monitor (SEM) instruments.
The energetic particle fluxes are 
 given as five-minute averaged values
 and the vector magnetic field is given
 as one-minute average values.
Flux values for three integral electron
 channels (E >0.6 MeV, E >2.0 MeV,
 and E >4.0 MeV) and one differential
 proton channel(0.7 MeV < E <4 MeV)
 are provided. These data are used by
 NOAA Space Environment Center (SEC)
 for the real-time monitoring and
 prediction of the conditions in the
 Earth's space environment.  A new
 series of GOES spacecraft began
 with GOES-8 launched on 4/13/94,
 GOES-9 launched on 5/23/95, and
 GOES-10 launched on 4/25/97. Typically
 two satellites are maintained
 operational,one at about 135 degrees
 geographic west longitude and one at
 about 75 degrees geographic west
 longitude. The satellite inclination
 is typically within a few tenths of a
 degree of the geographic equator.
However, the satellites can be moved,
 especially during the six months to
 one year following launch, and the
 inclination can increase after years
 of satellite operation.
Instrument data quality flags are set
 from real-time telemetry, or, in
 the case of historically-processed
 data sets when telemetry is not
 available, fixed to a level-1
 instrument status flag for all data
Reference: Geostationary Operational
 Environmental Satellite GOES I-M
 System Description, compiled by John
 Savides, Space Systems/Loral, Palo
 Alto, California, December 1992.
 Dr. Terrance Onsager, NOAA/SEC,
 tonsager@sec.noaa.gov, 303-497-5713,
 Boulder CO 80303 USA,
 or Martin Black, NOAA/SEC,
 mblack@sec.noaa.gov, 303-497-7235,
 325 Broadway, Boulder CO 80303 USA


Modification History
 Version 2.0: 1st operational version,-db, 14 Jul 92
 Corrected S/C location error & added Geographic (not geodetic) & GEO S/C positions.  -db, 16 Feb 93
 Added unit_ptr to s/c position units fixed CATDES on SC_pos_sm, fixed GSn   -db, 20 Apr 93
Version 3.0: Major re-write, added  GOES-8 and GOES-9, -db 22 Feb 96.
Fixed 1-character xyz label problem,
   -db, 8 May 96
Minor text & label changes,
   -db, 29 Jul 96
Added global metadata, support_data  text, blank variable attrib. data  per Mona Kessel sample file,
-db, 5 Aug 96 
Added xyz GEO,GSE,GSM labels, 
 replacing 1 cartesian label  -db, 29 Aug 96 
Create 1 skeleton table for EPS for all GOES  preparing for the switch from GOES-9 to 10  -anewman,
22 Jul 1998 
Added GOES-10 launch date and replaced Ann Newman with me as contact person. -mblack, 18 Mar 1999




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G0_K0_MAG
Description
The NOAA Geostationary Operational 
 Environmental Satellite (GOES) key
 parameters are obtained from the
 Energetic Particle Sensor (EPS) and
 and the magnetometer (MAG).  The
 key parameters are a subset of the 
 data available from the GOES Space
 Environment Monitor (SEM) instruments.
The vector magnetic field is 
 given as one-minute averaged values
 in three coordinate systems:
 (1) Spacecraft (s/c) P,E,N,
 (2) GSM x,y,z, (3) GSE x,y,z
s/c mag. field is defined as:
 Hp, perpendicular to the satellite
 orbital plane or parallel to the
 Earths spin axis in the case of
 a zero degree inclination orbit;
 He, perpendicular to Hp and
 directed earthwards; and
 Hn, perpendicular to both Hp and
 directed eastwards.
These data are used by
 NOAA Space Environment Center (SEC)
 for the real-time monitoring and
 prediction of the conditions in the
 Earth's space environment.  A new
 series of GOES spacecraft began
 with GOES-8 launched on 4/13/94,
 GOES-9 launched on 5/23/95, and
 GOES-10 launched on 4/25/97.
Typically two satellites are
 operational,one at about 135 degrees
 geographic west longitude and one at
 about 75 degrees geographic west
 longitude. The satellite inclination
 is typically within a few tenths of a
 degree of the geographic equator.
 However, the satellites can be moved,
 especially during the six months to
 one year following launch, and the
 inclination can increase after years
 of satellite operation.
Instrument data quality flags are set
 from real-time telemetry, or, in
 the case of historically-processed
 data sets when telemetry is not
 available, fixed to a level-1
 instrument status flag for all data
Reference: Monitoring Space
 Weather with GOES Magnetometers,
 Singer, H.J, L. Matheson, R.Grubb
 A.Newman, and S.D.Bouwer, SPIE
 Proceedings, Volume 2812,
 4-9 Aug 1996.  For more info, contact:
Dr. Howard Singer, NOAA/SEC,
 hsinger@sec.noaa.gov, 303-497-6959,
 Boulder CO 80303 USA,
 or Martin Black, NOAA/SEC,
 mblack@sec.noaa.gov, 303-497-7235,
 325 Broadway, Boulder CO 80303 USA


Modification History
 Version 2.0: 1st operational version,-db, 15 Dec 92
 Corrected S/C location error & added  Geographic (not geodetic) & GEO S/C  positions 
 Fixed ADID_ref from 97 to 96    -db, 16 Feb 93
 Added unit_ptr to s/c position units, fixed CATDES on SC_pos_sm, fixed GSn    -db, 27 Apr 93
 Version 3.0, Major re-write of text, 
 corrected label_1 bug (now cartesian),
 added GOES-8 & 9 CDFs,-db,26 Jan 1996
 Corrected no. of elements on lines 
   477-479 (labels), -db 7 May 1996
 Minor text changes, -db 22 Jul 1996
Added global metadata, support_data  text, blank variable attrib. data  per Mona Kessel sample file,
-db, 5 Aug 96 
Added xyz GEO,GSE,GSM labels, 
 replacing 1 cartesian label  -db, 29 Aug 96 
Create 1 skeleton table for MAG for all GOES  preparing for the switch from GOES-9 to 10  -anewman,
22 Jul 1998 
Added GOES-10 launch data and replaced Ann Newman with Martin Black as contact person. -mblack, 18
Mar 1999




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G5_C9_G504
Description
Derived from G504 in CDAW9 DB.
Data for all CDAW9 events A-E.
If all three B-field components were equal to 0 for one input data point, the data were considered
to be fill data.
Location during events A through E:  285 deg E.


Modification History
Converted to CDAWeb Feb 2000




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G6_C9_G605
Description
Derived from G605 in CDAW9 DB.
Data for all CDAW9 events A-E.
If all three B-field components were equal to 0 for one input data point, the data were considered
to be fill data.
Location during events A through E: 252 deg E.


Modification History
Converted to CDAWeb Feb 2000




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G6_K0_EPS
Description
The NOAA GOES satellites include 2 sensors: an Energetic Particle Sensor (EPS), and a Magnetometer
(MAG).
The satellites are geostationary. For older satellites, inclination may be up to 15 deg.
Data sometimes contains errors. especially GOES-6 EPS & possibly both  GOES 6,7 magnetometers. 
The EPS data are 5-min. averages, the MAG data are 1-min. averages. 
The NOAA Space Environment Lab (SEL), Space Environ. Services Center (SESC) uses this data in real
time for forecasting and monitoring. 
Reference: GOES Spacecraft OperationsManual, Volume I, May 1980, Hughes RefNo. D5150 SCG 00169R
GOES-8, with 3 electron sensors should launch in early 93: the IE variables will be defined
post-launch.
For additional info., contact Dave Bouwer, NOAA/SEL, Mail Code R/E/SE, 325 Broadway, Boulder, CO
80303 USA (303)497-3899.
SELVAX::DBOUWER or dbouwer@selvax.sel.bldrdoc.gov


Modification History
 Version 2.0: 1st operational version,-db, 14 Jul 92
 Corrected S/C location error & added Geographic (not geodetic) & GEO S/C positions.  -db, 16 Feb 93
 Added unit_ptr to s/c position units fixed CATDES on SC_pos_sm, fixed GSn   -db, 20 Apr 93




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G6_K0_MAG
Description
The NOAA GOES satellites include 2 sensors: an Energetic Particle Sensor (EPS), and a Magnetometer
(MAG).
The satellites are geostationary. For older satellites, inclination may be up to 15 deg.
Data sometimes contains errors.
The EPS data are 5-min. averages, the MAG data are 1-min. averages. 
B s/c has undeterm. errors in x,y B field for GSM and GSE is missing while corrections are
developed.
The NOAA Space Environment Lab (SEL), Space Environ. Services Center (SESC) uses this data in real
time for forecasting and monitoring. 
Reference: GOES Spacecraft OperationsManual, Volume I, May 1980, Hughes RefNo. D5150 SCG 00169R
GOES-8, with 3 electron sensors should launch in early 93: the IE variables will be defined
post-launch.
For additional info., contact Dave Bouwer, NOAA/SEL, Mail Code R/E/SE, 325 Broadway, Boulder, CO
80303 USA (303)497-3899.
SELVAX::DBOUWER or dbouwer@selvax.sel.bldrdoc.gov


Modification History
 Version 2.0: 1st operational version,-db, 15 Dec 92


Variable Notes

Magnetic Field, Cartesian GSE components
This variable not available for GOES-6
Magnetic Field, Cartesian GSM components
This variable not available for GOES-6
Magnetic Field, local spacecraft coordinates
Spacecraft coordinates (PEN), P=north,  E=earth, N=normal


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G7_K0_EPS
Description
The NOAA GOES satellites include 2 sensors: an Energetic Particle Sensor (EPS), and a Magnetometer
(MAG).
The satellites are geostationary. For older satellites, inclination may be up to 15 deg.
Data sometimes contains errors. especially GOES-6 EPS & possibly both  GOES 6,7 magnetometers. 
The EPS data are 5-min. averages, the MAG data are 1-min. averages. 
The NOAA Space Environment Lab (SEL), Space Environ. Services Center (SESC) uses this data in real
time for forecasting and monitoring. 
Reference: GOES Spacecraft OperationsManual, Volume I, May 1980, Hughes RefNo. D5150 SCG 00169R
GOES-8, with 3 electron sensors should launch in early 93: the IE variables will be defined
post-launch.
For additional info., contact Dave Bouwer, NOAA/SEL, Mail Code R/E/SE, 325 Broadway, Boulder, CO
80303 USA (303)497-3899.
SELVAX::DBOUWER or dbouwer@selvax.sel.bldrdoc.gov


Modification History
 Version 2.0: 1st operational version,-db, 14 Jul 92
 Corrected S/C location error & added Geographic (not geodetic) & GEO S/C positions.  -db, 16 Feb 93
 Added unit_ptr to s/c position units fixed CATDES on SC_pos_sm, fixed GSn   -db, 20 Apr 93




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G7_K0_MAG
Description
The NOAA GOES satellites include 2 sensors: an Energetic Particle Sensor (EPS), and a Magnetometer
(MAG).
The satellites are geostationary. For older satellites, inclination may be up to 15 deg.
Data sometimes contains errors.
The EPS data are 5-min. averages, the MAG data are 1-min. averages. 
B s/c has undeterm. errors in x,y B field for GSM and GSE is missing while corrections are
developed.
The NOAA Space Environment Lab (SEL), Space Environ. Services Center (SESC) uses this data in real
time for forecasting and monitoring. 
Reference: GOES Spacecraft OperationsManual, Volume I, May 1980, Hughes RefNo. D5150 SCG 00169R
GOES-8, with 3 electron sensors should launch in early 93: the IE variables will be defined
post-launch.
For additional info., contact Dave Bouwer, NOAA/SEL, Mail Code R/E/SE, 325 Broadway, Boulder, CO
80303 USA (303)497-3899.
SELVAX::DBOUWER or dbouwer@selvax.sel.bldrdoc.gov


Modification History
 Version 2.0: 1st operational version,-db, 15 Dec 92


Variable Notes

Magnetic Field, Cartesian GSE components
This variable not available for GOES-6
Magnetic Field, Cartesian GSM components
This variable not available for GOES-6
Magnetic Field, local spacecraft coordinates
Spacecraft coordinates (PEN), P=north,  E=earth, N=normal


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G8_K0_EP8
Description
The NOAA Geostationary Operational 
Environmental Satellite (GOES) key
parameters are obtained from the
Energetic Particle Sensor (EPS)
and the magnetometer (MAG).  The
key parameters are a subset of the 
data available from the GOES Space
Environment Monitor (SEM) instruments.
The energetic particle fluxes are 
given as five-minute averaged values
and the vector magnetic field is given
as one-minute average values.
Flux values for three integral electron
channels (E >0.6 MeV, E >2.0 MeV,
and E >4.0 MeV) and one differential
proton channel(0.7 MeV < E <4 MeV)
are provided. These data are used by
NOAA Space Environment Center (SEC)
for the real-time monitoring and
prediction of the conditions in the
Earth's space environment.  A new
series of GOES spacecraft began
with GOES-8 launched on 4/13/94 and
GOES-9 launched on 5/23/95. Typically
two satellites are maintained
operational,one at about 135 degrees
geographic west longitude and one at
about 75 degrees geographic west
longitude. The satellite inclination
is typically within a few tenths of a
degree of the geographic equator.
However, the satellites can be moved,
especially during the six months to
one year following launch, and the
inclination can increase after years
of satellite operation.
Reference: Geostationary Operational
Environmental Satellite GOES I-M
System Description, compiled by John
Savides, Space Systems/Loral, Palo
Alto, California, December 1992.
Dr. Terrance Onsager, NOAA/SEC,
tonsager@sec.noaa.gov, 303-497-5713,
Boulder CO 80303 USA,
or Dave Bouwer, NOAA/SEC,
dbouwer@sel.noaa.gov, 303-497-3899,
325 Broadway, Boulder CO 80303 USA


Modification History
 Version 2.0: 1st operational version,-db, 14 Jul 92
 Corrected S/C location error & added Geographic (not geodetic) & GEO S/C positions.  -db, 16 Feb 93
 Added unit_ptr to s/c position units fixed CATDES on SC_pos_sm, fixed GSn   -db, 20 Apr 93
Version 3.0: Major re-write, added  GOES-8 and GOES-9, -db 22 Feb 96.
Fixed 1-character xyz label problem,
   -db, 8 May 96
Minor text & label changes,
   -db, 29 Jul 96
Added global metadata, support_data  text, blank variable attrib. data  per Mona Kessel sample file,
-db, 5 Aug 96 
Added xyz GEO,GSE,GSM labels, 
 replacing 1 cartesian label  -db, 29 Aug 96




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G8_K0_MAG
Description
The NOAA Geostationary Operational 
 Environmental Satellite (GOES) key
 parameters are obtained from the
 Energetic Particle Sensor (EPS) and
 and the magnetometer (MAG).  The
 key parameters are a subset of the 
 data available from the GOES Space
 Environment Monitor (SEM) instruments.
The vector magnetic field is 
 given as one-minute averaged values
 in three coordinate systems:
 (1) Spacecraft (s/c) P,E,N,
 (2) GSM x,y,z, (3) GSE x,y,z
s/c mag. field is defined as:
 Hp, perpendicular to the satellite
 orbital plane or parallel to the
 Earths spin axis in the case of
 a zero degree inclination orbit;
 He, perpendicular to Hp and
 directed earthwards; and
 Hn, perpendicular to both Hp and
 directed eastwards.
These data are used by
 NOAA Space Environment Center (SEC)
 for the real-time monitoring and
 prediction of the conditions in the
 Earth's space environment.  A new
 series of GOES spacecraft began
 with GOES-8 launched on 4/13/94 and
 GOES-9 launched on 5/23/95.
Typically two satellites are
 operational,one at about 135 degrees
 geographic west longitude and one at
 about 75 degrees geographic west
 longitude. The satellite inclination
 is typically within a few tenths of a
 degree of the geographic equator.
 However, the satellites can be moved,
 especially during the six months to
 one year following launch, and the
 inclination can increase after years
 of satellite operation.
Reference: Monitoring Space
 Weather with GOES Magnetometers,
 Singer, H.J, L. Matheson, R.Grubb
 A.Newman, and S.D.Bouwer, SPIE
 Proceedings, Volume 2812,
 4-9 Aug 1996.  For more info, contact:
Dr. Howard Singer, NOAA/SEC,
 hsinger@sec.noaa.gov, 303-497-6959,
 Boulder CO 80303 USA,
 or Dave Bouwer, NOAA/SEC,
 dbouwer@sec.noaa.gov, 303-497-3899,
 325 Broadway, Boulder CO 80303 USA


Modification History
 Version 2.0: 1st operational version,-db, 15 Dec 92
 Corrected S/C location error & added  Geographic (not geodetic) & GEO S/C  positions 
 Fixed ADID_ref from 97 to 96    -db, 16 Feb 93
 Added unit_ptr to s/c position units, fixed CATDES on SC_pos_sm, fixed GSn    -db, 27 Apr 93
 Version 3.0, Major re-write of text, 
 corrected label_1 bug (now cartesian),
 added GOES-8 & 9 CDFs,-db,26 Jan 1996
 Corrected no. of elements on lines 
   477-479 (labels), -db 7 May 1996
 Minor text changes, -db 22 Jul 1996
Added global metadata, support_data  text, blank variable attrib. data  per Mona Kessel sample file,
-db, 5 Aug 96 
Added xyz GEO,GSE,GSM labels, 
 replacing 1 cartesian label  -db, 29 Aug 96




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G9_K0_EP8
Description
The NOAA Geostationary Operational 
Environmental Satellite (GOES) key
parameters are obtained from the
Energetic Particle Sensor (EPS)
and the magnetometer (MAG).  The
key parameters are a subset of the 
data available from the GOES Space
Environment Monitor (SEM) instruments.
The energetic particle fluxes are 
given as five-minute averaged values
and the vector magnetic field is given
as one-minute average values.
Flux values for three integral electron
channels (E >0.6 MeV, E >2.0 MeV,
and E >4.0 MeV) and one differential
proton channel(0.7 MeV < E <4 MeV)
are provided. These data are used by
NOAA Space Environment Center (SEC)
for the real-time monitoring and
prediction of the conditions in the
Earth's space environment.  A new
series of GOES spacecraft began
with GOES-8 launched on 4/13/94 and
GOES-9 launched on 5/23/95. Typically
two satellites are maintained
operational,one at about 135 degrees
geographic west longitude and one at
about 75 degrees geographic west
longitude. The satellite inclination
is typically within a few tenths of a
degree of the geographic equator.
However, the satellites can be moved,
especially during the six months to
one year following launch, and the
inclination can increase after years
of satellite operation.
Reference: Geostationary Operational
Environmental Satellite GOES I-M
System Description, compiled by John
Savides, Space Systems/Loral, Palo
Alto, California, December 1992.
Dr. Terrance Onsager, NOAA/SEC,
tonsager@sec.noaa.gov, 303-497-5713,
Boulder CO 80303 USA,
or Dave Bouwer, NOAA/SEC,
dbouwer@sel.noaa.gov, 303-497-3899,
325 Broadway, Boulder CO 80303 USA


Modification History
 Version 2.0: 1st operational version,-db, 14 Jul 92
 Corrected S/C location error & added Geographic (not geodetic) & GEO S/C positions.  -db, 16 Feb 93
 Added unit_ptr to s/c position units fixed CATDES on SC_pos_sm, fixed GSn   -db, 20 Apr 93
Version 3.0: Major re-write, added  GOES-8 and GOES-9, -db 22 Feb 96.
Fixed 1-character xyz label problem,
   -db, 8 May 96
Minor text & label changes,
   -db, 29 Jul 96
Added global metadata, support_data  text, blank variable attrib. data  per Mona Kessel sample file,
-db, 5 Aug 96 
Added xyz GEO,GSE,GSM labels, 
 replacing 1 cartesian label  -db, 29 Aug 96




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G9_K0_MAG
Description
The NOAA Geostationary Operational 
 Environmental Satellite (GOES) key
 parameters are obtained from the
 Energetic Particle Sensor (EPS) and
 and the magnetometer (MAG).  The
 key parameters are a subset of the 
 data available from the GOES Space
 Environment Monitor (SEM) instruments.
The vector magnetic field is 
 given as one-minute averaged values
 in three coordinate systems:
 (1) Spacecraft (s/c) P,E,N,
 (2) GSM x,y,z, (3) GSE x,y,z
s/c mag. field is defined as:
 Hp, perpendicular to the satellite
 orbital plane or parallel to the
 Earths spin axis in the case of
 a zero degree inclination orbit;
 He, perpendicular to Hp and
 directed earthwards; and
 Hn, perpendicular to both Hp and
 directed eastwards.
These data are used by
 NOAA Space Environment Center (SEC)
 for the real-time monitoring and
 prediction of the conditions in the
 Earth's space environment.  A new
 series of GOES spacecraft began
 with GOES-8 launched on 4/13/94 and
 GOES-9 launched on 5/23/95.
Typically two satellites are
 operational,one at about 135 degrees
 geographic west longitude and one at
 about 75 degrees geographic west
 longitude. The satellite inclination
 is typically within a few tenths of a
 degree of the geographic equator.
 However, the satellites can be moved,
 especially during the six months to
 one year following launch, and the
 inclination can increase after years
 of satellite operation.
Reference: Monitoring Space
 Weather with GOES Magnetometers,
 Singer, H.J, L. Matheson, R.Grubb
 A.Newman, and S.D.Bouwer, SPIE
 Proceedings, Volume 2812,
 4-9 Aug 1996.  For more info, contact:
Dr. Howard Singer, NOAA/SEC,
 hsinger@sec.noaa.gov, 303-497-6959,
 Boulder CO 80303 USA,
 or Dave Bouwer, NOAA/SEC,
 dbouwer@sec.noaa.gov, 303-497-3899,
 325 Broadway, Boulder CO 80303 USA


Modification History
 Version 2.0: 1st operational version,-db, 15 Dec 92
 Corrected S/C location error & added  Geographic (not geodetic) & GEO S/C  positions 
 Fixed ADID_ref from 97 to 96    -db, 16 Feb 93
 Added unit_ptr to s/c position units, fixed CATDES on SC_pos_sm, fixed GSn    -db, 27 Apr 93
 Version 3.0, Major re-write of text, 
 corrected label_1 bug (now cartesian),
 added GOES-8 & 9 CDFs,-db,26 Jan 1996
 Corrected no. of elements on lines 
   477-479 (labels), -db 7 May 1996
 Minor text changes, -db 22 Jul 1996
Added global metadata, support_data  text, blank variable attrib. data  per Mona Kessel sample file,
-db, 5 Aug 96 
Added xyz GEO,GSE,GSM labels, 
 replacing 1 cartesian label  -db, 29 Aug 96




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GB_ED_FMI
Description
                                          Geographic No. Code  Station Name   
 Components  Latitude  Longitude  1  AMD   Amderma              X,Y,Z     69.46
    60.77         2  BLC   Baker Lake           X,Y,Z     64.33    -96.03 
 3  BRW   Barrow               X,Y,Z     71.30   -156.75       4  CBB   Cambridg
e Bay        X,Y,Z     69.10   -105.00       5  COL   College              X,Y,Z
     64.87   -147.83       6  CPS   Cape Schmidt         X,Y,Z     68.92   -179.
48       7  DIK   Dixon                X,Y,Z     73.55     80.57         8  ESK
  Eskdalemuir          X,Y,Z     55.32     -3.20         9  FCC   Fort Churchill
       X,Y,Z     58.80    -94.10       10  GDH   Godhavn              H,E,Z
69.23    -53.52       11  GLL   Glenlea              X,Y,Z     49.63    262.87
    12  MBC   Mould Bay            X,Y,Z     76.30   -119.40      13  MMK   Murm
ansk             X,Y,Z     68.25     33.08        14  NAQ   Narssarssuaq      
 H,E,Z     61.20    -45.40       15  OTT   Ottawa               X,Y,Z     45.40
   -75.55       16  PDB   Poste-de-la-Baleine  X,Y,Z     55.20    -77.70       1
7  RES   Resolute Bay         X,Y,Z     64.70    -94.90       18  SIT   Sitka
             X,Y,Z     57.10   -135.30      19  SOD   Sodankyla            X,Y,Z
     67.37     26.63        20  STJ   St. Johns            X,Y,Z     47.60    -5
2.60       21  THL   Thule/Qanaq          H,E,Z     77.48    -69.17       22  TI
K   Tixie Bay            X,Y,Z     71.58    129.00       23  VIC   Victoria  
        X,Y,Z     48.50   -123.40      24  YEK   Yellowknife          X,Y,Z
62.43   -114.40


Modification History
The data given for BLC are those of CBB and vice versa. In BLC (shown as CBB),
the X and  Y coordinates are also interchanged. This was reported for event B;
other events have not yet been checked. Data from SOD are given as (X,Y,Z)
coordinates but are thougthought to be in (HDZ), at least for Event B.




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GE_AT_DEF
Description
TBS


Modification History
6/13/91 - Original Implementation
9/18/91 - Modified for new attitude file format changes.  ICCR 881
2/11/92 - Used the variable name TIME and type CDF_INT4 and size 3 instead of 
EPOCH, CDF_EPOCH and 1 for the time tags.  CCR 490
6/1/92 - Added global attributes TITLE, PROJECT, DISCIPLINE, SOURCE_NAME, 
DATA_VERSION, and MODS; added variable attributes VALIDMIN, VALIDMAX, 
LABL_PTR_1, and MONOTON; added variables EPOCH and LABEL_TIME; 
changed variable name TIME to TIME_PB5.  CCR 1066
11/07/92 - use cdf variable Epoch and Time_PB5
6/8/93 - Added global attributes ADID_ref and Logical_file_id.  CCR 1092
7/5/94 - CCR ISTP 1852, updated CDHF skeleton to CDF standards - JT
9/20/94 - Added global attributes GCI_RA_ERR and GCI_DECL_ERR.  CCR 1932
11/7/94 - Merged CCR 1852 changes and corrected errors 
made in CCR 1852.  ICCR 1884
12/7/94 - Modified MODS and LABLAXIS to follow ISTP standards.  ICCR 1885




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GE_AT_PRE
Description
TBS


Modification History
6/13/91 - Original Implementation
9/18/91 - Modified for new attitude file format changes.  ICCR 881
2/11/92 - Used the variable name TIME and type CDF_INT4 and size 3 instead of 
EPOCH, CDF_EPOCH and 1 for the time tags.  CCR 490
6/1/92 - Added global attributes TITLE, PROJECT, DISCIPLINE, SOURCE_NAME, 
DATA_VERSION, and MODS; added variable attributes VALIDMIN, VALIDMAX, 
LABL_PTR_1, and MONOTON; added variables EPOCH and LABEL_TIME; 
changed variable name TIME to TIME_PB5.  CCR 1066
11/07/92 - use cdf variable Epoch and Time_PB5
6/8/93 - Added global attributes ADID_ref and Logical_file_id.  CCR 1092
7/5/94 - CCR ISTP 1852, updated CDHF skeleton to CDF standards - JT
9/20/94 - Added global attributes GCI_RA_ERR and GCI_DECL_ERR.  CCR 1932
11/7/94 - Merged CCR 1852 changes and corrected errors 
made in CCR 1852.  ICCR 1884
12/7/94 - Modified MODS and LABLAXIS to follow ISTP standards.  ICCR 1885




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GE_ED_MGF
Description
Kokubun et al., Geotail Prelaunch Report, ISAS, 58-70, 1992


Modification History
Created on 7/26/95, Adapted from MGF KP skeleton table




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GE_H0_CPI
Description
GEOTAIL Prelaunch Report
 April 1992, SES-TD-92-007SY
 CPI-SW Solar Wind Analyzer
   Key Parameters
      Ion number density
      Average proton energy
      Bulk flow velocity
 CPI-HP Hot Plasma Analyzer
   Key Parameters
      Ion number density
      Average proton energy
      Average electron energy
      Bulk flow velocity
      Plasma pressure
 CPI-IC Ion Composition Analyzer
   Key Parameters
      Principal Species
        H+
        He++
        He+
        O+
 CPI Survey Data will be made available
 via the World Wide Web as image files
 for the mission operation periods in a
 compressed time resolution for viewing
 and/or downloading with a WWW browser
 from the URL
 http://www-pi.physics.uiowa.edu/


Modification History
made from ASCII files at University of IOWA, see URL: http://www-pi.physics.uiowa.edu/www/cpi/


Variable Notes

Ion bulk flow velocity, 3 GSE cartesian components (SWA)
From 5 deg angular bins
Kinetic Temperature of Hydrogen component of solar wind, scalar
calculated by integrating the distribution function
Ion number density (Solar Wind Analyzer), scalar
Assuming no helium (0.3 - several hundred) if the density is less than 0.3/cc
the higher moments (VEL,TEMP) shall not be used because of the poor counting
statistics.
Ion Pressure (assuming protons measured and adding 5% alphas - Solar Wind Analyzer), scalar
Assuming Vp = Va, P = C * Np * mp * Vp*Vp * [1 + 4(.05)]. mp = 1.67 * 10^(-27),
C = 10^(21), Np in #/cc, Vp in km/s. Pressure not provided for density less than
0.3/cc because of the poor counting statistics.
Label for 3 comp velocity
Theta: polar angle in GSE coordinates -- 0 = flow toward north ecliptic pole
(positive vz), 90 = flow in spin plane (within 2 degrees of ecliptic), 180 =
flow toward south pole (negative vz).    Phi: azimuthal angle -- 0 = flow toward
sun  (positive vx), 90 = flow toward dusk  (positive vy), 180 = flow away from
sun  (negative vx), 270 = flow toward dawn   (negative vy)


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GE_H0_LEP
Description
J.Geomag.Geoelectr.,46,669,1994


Modification History
created Oct 1994
Modified by JT Oct. 28, 1994
Adapted by D Batchelor Apr. 8, 1996




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GE_H0_MGF
Description
Kokubun et al., Geotail Prelaunch Report, ISAS, 58-70, 1992


Modification History
Created by S.-H. Chen on 6/18/97; Adapted from GE_FO_MGF


Variable Notes

Magnetic field magnitude (1 min)
Average of the magnitudes (F1)
RMS magnitude (1 min)
RMS of the magnitudes (F1 RMS)
Magnetic field magnitude (3 sec)
Average of the magnitudes (F1)
RMS magnitude (3 sec)
RMS of the magnitudes (F1 RMS)


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GE_H1_CPI
Description
 GEOTAIL Prelaunch Report 
  April 1992, SES-TD-92-007SY 
  
 CPI/HPA  Hot Plasma Analyzer 
    High Time Resolution Moments 
       Ion Number density 
       Ion Average Temperature 
       Ion Bulk Flow Velocity 
       Electron Number Density 
       Electron Average Temperature 
  
 CPI Survey Data will be made available 
 via the World Wide Web as image files 
 for the mission operation periods in a 
 compressed time resolution for viewing 
 and/or downloading with a WWW browser 
 from the URL: 
     http://www-pi.physics.uiowa.edu/www/cpi/


Modification History
First Delivery version, 29-JUL-1998
Final Delivery version, 17-AUG-1998


Variable Notes

Kinetic Temperature of Hot Plasma Ions, scalar
calculated by integrating the distribution function
Kinetic Temperature of Hot Plasma Electrons, scalar
Calculated by integrating the distribution function


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GE_H1_MGF
Description
Kokubun et al., Geotail Prelaunch Report, ISAS, 58-70, 1992


Modification History
Created by R.L. Kessel in July 2000
Revised by R.L. Kessel on 31 Dec 2000 to update global metadata
Revised by R.L. Kessel on 28 Feb 2001 to add minute data




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GE_H2_CPI
Description
      GEOTAIL Prelaunch Report April 1992, SES-TD-92-007SY
 
The Solar Wind Analyzer of the Comprehensive Plasma Instrumentation
(CPI-SW) is described by Frank et al., [J. Geomagn. Geoelect., Volume 46,
pp. 23-37, 1994].  See also .http://www-pi.physics.uiowa.edu/www/cpi/. 
 
Three dimensional ion velocity distributions, f(v), are given at
approximately 2.4 minute intervals.  Ion values of f(v) are tabulated in:
 
  (12 detector fields of view) * (21 Spin Sectors) * (64 E/Q Passbands)
 
Thus there are 16,128 samples for ions given approximately once each
2.4 minutes.  The values of f(v) are in log(base10) with units (s**3/cm**6)
computed with the assumption that the ions are protons.  Angles are
specified in right-handed spacecraft coordinates with Z along the spin
axis and X toward the sun.  If the response is less than the one-count
threshold of the sensors the value given for f(v) is -31.0.
 
The 12 detector fields-of-view (FOV) include particles with velocity
vectors directed into the following ranges of Theta and Phi.
 
              Angular Coverage, Ions
              ______________________
    Detector    Theta         Phi
     FOV        Range        Range
              (degrees)    (degrees)
    _______   _________    _________
      1        60 -  66    -8  -  7
      2        65 -  71    -7  -  6
      3        70 -  76    -6  -  5
      4        75 -  81    -5  -  4
      5        79 -  86    -4  -  3
      6        84 -  91    -3  -  2
      7        89 -  96    -3  -  2
      8        94 - 101    -4  -  3
      9        99 - 105    -5  -  4
     10       104 - 110    -6  -  5
     11       109 - 115    -7  -  6
     12       114 - 120    -8  -  7
 
The azimuth angles of particle velocity vectors are the Phi angles listed
above offset by the rotation angles of the 21 spin sectors.
 
     Spin    Rotation Angle
    Sector   Range (degrees)
    ______   ______________
       1        114.50
       2        120.74
       3        126.97
       4        137.00
       5        143.24
       6        149.47
       7        159.50
       8        165.74
       9        171.97
      10        182.00
      11        188.24
      12        194.47
      13        204.50
      14        210.74
      15        216.97
      16        227.00
      17        233.24
      18        239.47
      19        249.50
      20        255.74
      21        261.97
 
The 64 E/Q passbands used to sample f(v) are centered on the E/Q
values listed below.  Each passband has (Delta E)/E approximately 0.1.
 
    Passband    E/Q (Volts)             Passband    E/Q (Volts)
    ________    ___________             ________    ___________
        1          144.3                   33          1023.1
        2          153.4                   34          1087.7
        3          163.0                   35          1156.4
        4          173.3                   36          1229.4
        5          184.3                   37          1307.0
        6          195.9                   38          1389.5
        7          208.3                   39          1477.2
        8          221.4                   40          1570.5
        9          235.4                   41          1669.7
       10          250.3                   42          1775.1
       11          266.1                   43          1887.1
       12          282.9                   44          2006.3
       13          300.7                   45          2132.9
       14          319.7                   46          2267.6
       15          339.9                   47          2410.8
       16          361.4                   48          2563.0
       17          384.2                   49          2724.8
       18          408.4                   50          2896.8
       19          434.2                   51          3079.7
       20          461.6                   52          3274.1
       21          490.8                   53          3480.8
       22          521.8                   54          3700.5
       23          554.7                   55          3934.2
       24          589.7                   56          4182.5
       25          626.9                   57          4446.6
       26          666.5                   58          4727.3
       27          708.6                   59          5025.8
       28          753.3                   60          5343.1
       29          800.9                   61          5680.4
       30          851.5                   62          6039.0
       31          905.2                   63          6420.3
       32          962.4                   64          6825.6


Modification History
First Delivery version, 29-JUL-1998
Final Delivery version, 18-AUG-1998


Variable Notes

Analyzer's Polar Detector Center Angle
See TEXT description for full angular definitions
Analyzer's Azimuthal Sector Center Angle
See TEXT description for full angular definitions


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GE_H3_CPI
Description
          GEOTAIL Prelaunch Report April 1992, SES-TD-92-007SY
 
The Hot Plasma Analyzer of the Comprehensive Plasma Instrumentation
(CPI-HP) is described by Frank et al., [J. Geomagn. Geoelect., Volume 46,
pp.  23-37, 1994].  See also .http://www-pi.physics.uiowa.edu/www/cpi/. 
 
Three dimensional ion and electron velocity distributions, f(v), are
given at approximately one minute intervals.  For both ions and electrons
values of f(v) are tabulated in:
 
    (9 detector fields of view)*(16 Spin Sectors)*(24 E/Q Passbands) 
 
Thus there are 3456 samples for ions and 3456 samples for electrons given
approximately once each minute.  The values of f(v) are in MKS units
(s**3/m**6) computed with the assumption that the ions are protons.
Angles are specified in right-handed spacecraft coordinates with Z along
the spin axis and X toward the sun.  If the response is less than the
one-count threshold of the sensors the value given for f(v) is zero.
 
The 9 detector fields-of-view (FOV) include particles with velocity
vectors directed into the following ranges of Theta and Phi.
 
              Angular Coverage, Ions
              ______________________
    Detector    Theta         Phi
     FOV        Range        Range
              (degrees)    (degrees)
    _______   _________    _________
      1         4 -  35    -66 to 81
      2        22 -  48    -19 to 44
      3        42 -  66    -33 to 22
      4        57 -  84    -22 to 10
      5        74 - 106    -12 to 4
      6        96 - 123    -22 to 10
      7       114 - 138    -33 to 22
      8       132 - 158    -19 to 44
      9       145 - 176    -66 to 81
 
         Angular Coverage, Electrons
              ______________________
    Detector    Theta         Phi
     FOV        Range        Range
              (degrees)    (degrees)
    _______   _________    _________
      1         4 -  38    -31 to 81
      2        22 -  48    -20 to 45
      3        42 -  66    -33 to 23
      4        57 -  84    -22 to 11
      5        74 - 106    -12 to 5
      6        96 - 123    -22 to 11
      7       114 - 138    -33 to 23
      8       132 - 158    -20 to 45
      9       142 - 176    -31 to 81
 
The azimuth angles of particle velocity vectors are the Phi angles listed
above offset by the rotation angles of the 16 spin sectors.
 
     Spin    Rotation Angle
    Sector   Range (degrees)
    ______   ______________
      1         0.0 -  22.5
      2        22.5 -  45.0
      3        45.0 -  67.5
      4        67.5 -  90.0
      5        90.0 - 112.5
      6       112.5 - 135.0
      7       135.0 - 157.5
      8       157.5 - 180.0
      9       180.0 - 202.5
     10       202.5 - 225.0
     11       225.0 - 247.5
     12       247.5 - 270.0
     13       270.0 - 292.5
     14       292.5 - 315.0
     15       315.0 - 337.5
     16       337.5 - 360.0
 
The 24 E/Q passbands used to sample f(v) are a subset of 64 possible
passbands and are centered on the E/Q values listed below.  Each passband
has (Delta E)/E approximately 0.1. 
 
    Passband    E/Q (Volts)
    ________    ___________
      17            22
      19            31
      21            43
      23            61
      25            85
      27           118
      29           165
      31           230
      33           322
      35           449
      37           627
      39           876
      41          1220
      43          1710
      45          2390
      47          3330
      49          4650
      51          6500
      53          9080
      55         12700
      57         17700
      59         24700
      61         34500
      63         48200
 
A quality flag is set for each record using a simple automated procedure
that checks densities and temperatures of electrons and ions.  If the
densities of these species differ significantly then it is likely that
for some reason one or both charge species are poorly resolved.  Also, if
the electron temperature is found to be less than 3.5E5 K then the
spacecraft is probably in the solar wind and the ions and possibly the
electrons are not well resolved.  According to these criteria the quality
flag is set to indicate:
 
    Flag = 1    Probably Good
    Flag = 2    Possibly Poor


Modification History
First Delivery version, 29-JUL-1998
Final Delivery version, 18-AUG-1998


Variable Notes

Quality Flag for CPI/HPA Moments
 Flag=1 Probaby Good, Flag=2 Probably Poor
Analyzer's Polar Detector Center Angle
See TEXT description for full angular definitions
Analyzer's Azimuthal Sector Center Angle
See TEXT description for full angular definitions


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GE_K0_CPI
Description
GEOTAIL Prelaunch Report
 April 1992, SES-TD-92-007SY
 CPI-SW Solar Wind Analyzer
   Key Parameters
      Ion number density
      Average proton energy
      Bulk flow velocity
 CPI-HP Hot Plasma Analyzer
   Key Parameters
      Ion number density
      Average proton energy
      Average electron energy
      Bulk flow velocity
      Plasma pressure
 CPI-IC Ion Composition Analyzer
   Key Parameters
      Principal Species
        H+
        He++
        He+
        O+
 CPI Survey Data will be made available
 via the World Wide Web as image files
 for the mission operation periods in a
 compressed time resolution for viewing
 and/or downloading with a WWW browser
 from the URL
 http://www-pi.physics.uiowa.edu/ 



SPDF/SPOF Supplementary Information and Notes:


Modification History
First Delivery version, 7-OCT-1993
v2.0, 12-APR-1994, RLD
     Changed dimensions to 3 and 2 at
     recommendation of Mona Kessel
     With help of Jeff Love (CDFSUPPORT)
     have cleaned up dim problems
v2.1, 20-JUL-1994, RLD
     Change VALIDMIN dates for CPI data
     be 1 Oct 92
     Added items to TEXT field to
     include all KPs and defined
     coordinate system used for velocities
v2.2, 24-JAN-1995, RLD
     Added some new comments to the
     description section
v2.3, 19-MAY-1995, RLD
     Added SW_V Z-component
v2.31, 8-Jun-95, RLD
     Corrected dependent variables
     to differentiate between CDF's
     2-D size 2 & 3 (i.e., 2 & 3-
     dimensional velocities
v2.4, 28-Sep-95, RLD
     Updated text & variable
     min/max values for consistency
v2.41, 21-DEC-1995, RLD
     Updated for KPGS v2.3 delivery
     Official version of ST is v04


Variable Notes

Ion number density (Solar Wind Analyzer), scalar
From 5 deg angular bins
Ion bulk flow velocity, 3 ~GSE cartesian components (SWA)
From 5 deg angular bins
CPI Post Gap Flag (0: no gap immediately prior to this record, scalar
CPI Post Gap Flag (0:  no gap immediately prior to this record; 1:  gap due to
inst mode;  2:  gap due to missing SIRIUS data;  3:  gap due to noisy SIRIUS
data;  20: gap due to missing Minor Frame(s)), scalar


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GE_K0_EFD
Description
Geotail Prelaunch Report, April 1992



The sensor providing data here (called EFD-P in report above) measures the difference of electric
potential between two electrodes (probes) immersed in the plasma.
There are two sperical probes and two wire antennas each of which is extended by 50 meters from the
satellite in its rotational plane.
 The two sperical probes are opposite each other (100 meters tip-to-tip) as are the two wire
antennas. The probe pairs are orthogonal to each other.
Diving the potential difference by the distance between the probes or the centers of the conducting
portion of the wire antennas gives the electric field component along the probe extension.
The measurement of the electric field in the satellite rotational plane gives the vector electric
field when the electric field along the magnetic field is much smaller than the perpendicular
component.


Modification History
Version 1.0 Jan. 12, 1993
Modified on 7/18/94 and 7/29/94 by JT
Modified on 9/9/94 by JT - KPGS CCR 0039




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GE_K0_EPI
Description
EPIC Instrument Description: 
 A) Supra-Thermal Ion Composition Spectrometer (STICS) Subsystem: 
    1) Ion Head/Telescope Coverage 
       Apperature Width:  53.4 polar deg 
       Apperature Center: Spacecraft spin plane
 B) Ion Composition Spectrometer (ICS) Subsystem: 
    1) Ion Head Coverage 
       Apperature Width:  60.0 polar deg excluding center 16.0 deg 
       Apperature Center: Spacecraft spin plane
    2) Electron Detector Coverage 
       Apperature Width:  60.0 polar deg 
       Apperature Center: Spacecraft spin plane
    3) Caution 
       ICS Ion channels can change between two sets of energy pass 
       bands from record to record; consult the associated energy 
       information to determine what the current values are.
Anisotropy Calculation Qualification: 
 A) a1, a2, phi1 and phi2 are not
    calculated when the count rate
    is below a threshhold, currently
    8 counts/96 seconds.


Modification History
v1.0 19-Sep-1991
v1.3 11-Mar-1992
v2.0 13-Jan-1993 changes for Standards and Convensions v1.1
v3.0 25-May-1994 a) corrected PDiffI_S_Eminus    dimen variance FTFF -> TFFF
 b) changed LABL_PTR_1 to LABLAXIS    for 3 variables
 c) removed several DEPEND1 attributes d) corrected indexing for M8/P2
 e) corrected anisotropy min/max    values from [0,2pi] to
    [-pi,+pi] for phi1 and to    [-pi/2,+pi/2] for phi2
 f) changed ratio SCALETYP from    linear to log
 g) narrowed several SCALEMIN/MAX    ranges
v3.1 16-Sep-1994 a) shortened TEXT entries to max of     80 char
 b) removed several DEPEND0/1 attributes
 c) removed value for Logical_file_id    entry


Variable Notes

9-212 keV/e H Anis. param. (a0/a1/a2/phi1/phi2 from Fourier fit to H flux , EPIC/STICS)
9-212 keV/e H Anisotropy parameters (a0/a1/a2/phi1/phi2 from Fourier fit   a0*(1
+ a1*cos(theta-phi1) +a2*cos2(theta-phi2))   to H flux , EPIC/STICS)
9-212 keV/e H Anis. param. (a0/a1/a2/phi1/phi2 from Fourier fit to H flux , EPIC/STICS), with error bars
9-212 keV/e H Anisotropy parameters (a0/a1/a2/phi1/phi2 from Fourier fit   a0*(1
+ a1*cos(theta-phi1) +a2*cos2(theta-phi2))   to H flux , EPIC/STICS)


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GE_K0_LEP
Description
J.Geomag.Geoelectr.,46,669,1994


Modification History
created Oct 1994
Modified by JT Oct. 28, 1994




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GE_K0_MGF
Description
Kokubun et al., Geotail Prelaunch Report, ISAS, 58-70, 1992


Modification History
Created on 8/7/92, Modified on 1/25/93, 
Modified on 2/19/93, Modified on 3/8/93, 
Modified on 4/16/93, Modified on 7/18/94 by JT




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GE_K0_PWI
Description
Text description of the experiment need to be defined by the developer


Modification History
7/24/92
4/4/94




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GE_K0_SPHA
Description
Geotail Prelaunch Report April 1992


Modification History
4/6/92 - Original Implementation, CCR 935
6/12/92 - Added global attributes TITLE, PROJECT, 
DISCIPLINE, SOURCE_NAME, DATA_VERSION, and MODS;
added variable attributes VALIDMIN, VALIDMAX, LABL_PTR_1, and MONOTON;
added variables EPOCH and LABEL_TIME; 
changed variable name TIME to TIME_PB5. CCR 935
9/23/92 - Changed descriptor value from SPAH to SPHA. ICCR 1387
2/22/93 - Changed VALIDMAX of FAULT. CCR 1361
6/10/93 - Added ADID_ref and Logical_file_id. CCR 1092
6/14/94 - CCR ISTP 1852, updated CDHF skeleton to CDF standards - JT
11/9/94 - Correct errors made in ccr 1852.  ICCR 1884




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GE_K1_MGF
Description
Kokubun et al., Geotail Prelaunch Report, ISAS, 58-70, 1992


Modification History
Created by R.L. Kessel on 11/7/2000,




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GE_OR_DEF
Description
TBS


Modification History
Originated Monday, May 13, 1991
Modified June 13, 1991 for version 2.1
Modified October 2,1991 for new global attributes, incr sizes
Modified 11/11/91 Add sun vector, replace space id with support id
Modified 1992 Feb 11 to use the variable name TIME and type CDF_INT4 instead of 
EPOCH and CDF_EPOCH for the time tags CCR 490
Modified 6/2/92 add project, discipline, source_name, data_version, title, and 
mods to global section; add validmin, validmax, labl_ptr_1 and monoton 
attributes to some variables; put epoch time back in, rename time to 
time_pb5; add label_time to variables
Modified 11/07/92 to use Epoch and Time_PB5 variable name
Modified 6/2/93 add ADID_ref and Logical_file_id
7/5/94 - CCR ISTP 1852 updated CDHF skeleton to CDF standards - JT
9/21/94 - Added 24 new global attributes to log the ephemeris 
comparison summary report from the definitive FDF orbit file.  CCR 1932
11/7/94 - Merged CCR 1852 changes and corrected errors 
made in CCR 1852.  ICCR 1884
12/7/94 - Modified MODS to follow ISTP standards.  ICCR 1885
01/05/95 - add heliocentric coordinate system.  CCR 1889
2/28/95 - added COMMENT1 and COMMENT2 for CCR




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GE_OR_PRE
Description
TBS


Modification History
Originated Monday, May 13, 1991
Modified June 13, 1991 for version 2.1
Modified October 2,1991 for new global attributes, incr sizes
Modified 11/11/91 Add sun vector, replace space id with support id
Modified 1992 Feb 11 to use the variable name TIME and type CDF_INT4 instead of 
EPOCH and CDF_EPOCH for the time tags CCR 490
Modified 6/2/92 add project, discipline, source_name, data_version, title, and 
mods to global section; add validmin, validmax, labl_ptr_1 and monoton 
attributes to some variables; put epoch time back in, rename time to 
time_pb5; add label_time to variables
Modified 11/07/92 to use Epoch and Time_PB5 variable name
Modified 6/2/93 add ADID_ref and Logical_file_id
7/5/94 - CCR ISTP 1852 updated CDHF skeleton to CDF standards - JT
9/21/94 - Added 24 new global attributes to log the ephemeris 
comparison summary report from the definitive FDF orbit file.  CCR 1932
11/7/94 - Merged CCR 1852 changes and corrected errors 
made in CCR 1852.  ICCR 1884
12/7/94 - Modified MODS to follow ISTP standards.  ICCR 1885
01/05/95 - add heliocentric coordinate system.  CCR 1889
2/28/95 - added COMMENT1 and COMMENT2 for CCR




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GE_Y0_PRE
Description
GROUP 1    Satellite   Resolution   Factor
            geotail       720         1
                                          
                                          
           Start Time           Stop Time 
           1999 360 00:00       1999 360 23:60   
                                          
                                          
Coord/            Min/Max   Range Filter       Filter
Component   Output Markers  Minimum  Maximum   Mins/Maxes 
GEO Lat      YES      -        -        -           -        -           -   
GEO Lon      YES      -        -        -           -        -           -   
                                          
                                          
Addtnl             Min/Max   Range Filter       Filter
Options     Output Markers  Minimum  Maximum   Mins/Maxes
dEarth       YES      -        -        -           -   
MagStrgth    YES      -        -        -           -   
                                          
                                          
Magnetic field model:                          
    Internal: IGRF
    External: Tsyganenko 89C     Kp:  3-,3,3+
    Stop trace altitude (km):   100.00
                                          
Formats and units:                          
    Day/Time format: YYYY DDD HH:MM
    Degrees/Hemisphere format: Decimal degrees with 2 place(s).
        Longitude 0 to 360, latitude -90 to 90.
    Distance format: Earth radii with 2 place(s).


Modification History
Originated 03/14/96




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GM_C9_GM30
Description
Derived from CDAW-9 DB GM30.
Data for all CDAW-9 events A-E.


Modification History
Converted to CDAWeb Feb 2000




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GM_C9_GM32
Description
Derived from GM32 in CDAW9 DB.
Data for all CDAW9 events A-E.
The channel for this data set is nominally designed for protons with energies of 0.8 - 4 MeV. 
However, there are a lot of electron counts and proton counts are almost always masked.  There are
often injection events in the dawn side in this data set so that we assume that particles are mainly
electrons with energies less than 500 KeV.  There is one channel for electrons with energies greater
than 2 MeV but it is not available during the CDAW 9 periods.  
Non-zero values of the CALB parameter imply the CDF contains  calibration data at those points.


Modification History
Converted to CDAWeb Feb 2000




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GM_C9_GMMD
Description
 Data derived from CDAW9 GMMD dataset
Data for all CDAW9 events A-E.
Data derived by S. Kayser


Modification History
Converted to CDAWeb Feb 2000




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HEL1_H0_CRP
Description
The objext of experiment (E6) was to study high-energy, charged, cosmic-reay particles of solar,
planetary, and galactic origin in interplanetary space.




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HK_H0_MAG
Description
Gurnett, D. A., and L. A. Frank, A region of intense plasma wave turbulences on auroral field lines,
JGR, 69, 1031, 1977
Farrell, W. M., and J. A. Van Allen, Observations of the Earth"s  polar cleft at large radial
distances with Hawkeye 1 magnetometer, JGR, 95, 20, 945, 1990


Modification History
Created by S. Chen on 2-5-97
Modified by R. Kessel on 13 June 2000


Variable Notes

Despin Method (0:not despun; 1 optical aspect; 2:sun pulse; 3:array voltage; 4 mag field model; 4/5 - solar array method)
0 - not despun; 1 - optical aspect  system; 2 - lepedea method; 3 - magnetometer
method; 4/5 -  solar array method - interpolated
Estimate of the angular uncertainty in Mag Field direction (set to zero for despin = 1 or 2), scalar
may be pessimistic estimate
magnetometer range indicator
B field measurement range setting= 0: +/- 150 nT; 1: +/-450 nT; 2: +/- 1500 nT;
3: +/1 25000 nT.


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HK_H0_VLF
Description
BUILD_DATE:                     1974-01-01
INSTRUMENT_MASS:         0.23 (LESS BOOMS) kg
INSTRUMENT_HEIGHT:       0.058 mt
INSTRUMENT_LENGTH:       0.140 mt
INSTRUMENT_WIDTH:         0.140 mt
INSTRUMENT_MANUFACTURER_NAME:   UNIV IOWA
INSTRUMENT_SERIAL_NUMBER:     VLF-05
                         Electric Antenna
The electric antenna on HAWKEYE consisted of two extendible beryllium copper elements 0.025 inch in
diameter which could be extended to a maximum tip-to-tip length of 42.7 m. Except for the outermost
6.1 m of each element, which had a conducting surface, the antenna was coated with Pyre-ML to
electrically insulate the antenna from the surrounding plasma. The insulating coating was required
to insulate the antenna from the perturbing effects of the plasma sheath surrounding the spacecraft
body. At high altitudes, the thickness of the plasma sheath surrounding  the spacecraft body was
quit large, on the order of 9 m. Since the conducting portion of the antenna must extend beyond the
plasma sheath, it was necessary that the antenna be rather long, at least 30 m. tip-to-tip. The
antenna mechanism used on HAWKEYE was the Dual-Tee extendible antenna manufactured by Fairchild
Industries. The antenna length was 42.49 meters after final deployment until the last orbit, when an
attempt was made to retract the antenna to reduce the spacecraft drag.
                   Magnetic Antenna
 The magnetic antenna for this experiment consisted of a search coil with a high permeability core
mounted on a boom approximately 1.5 m. from the centerline of the spacecraft body. The boom was a
three element telescoping device developed at the University of Iowa. The boom supporting the flux
gate magnetometer on the opposite side of the spacecraft was the same type. Both booms were extended
simultaneously by an electric motor.
           The search coil core was .305 m. long and was wound with approximately 20,000 turns of
copper wire. The axis of the search coil was parallel to the spin axis of the spacecraft. A
preamplifier was located with the sensor to provide low-impedance signals to the main electronics
package in the spacecraft body. The frequency range of the search coil antenna was from 1.0 Hz to
10.0 kHz.
                         Electronics
 The potential difference between the electric antenna elements was amplified by a high input
impedance differential amplifier to provide a 0 to 5 volt analog voltage, V-Diff, to the spacecraft
encoder. As the spacecraft rotated the potential difference between the antenna elements  varied
sinusoidally at the spacecraft rotation rate, with an amplitude proportional to the electric field
strength and a phase determined by the direction of the electric field. The frequency response of
the differential amplifier was 0.05 Hz to 10 Hz and included the entire range of spin rates expected
as the antenna was deployed. The V-Diff signal was sampled 6 times each frame by the encoder. The
gain of the differential amplifier could be controlled by command to provide dynamic ranges of
+/-0.5 and +/-8.0 volts for the antenna potential difference measurements.
           Signals from the electric antenna in the frequency range from 10 kHz to 200 kHz were
analyzed by the narrow band step frequency receiver. The primary purpose of this receiver was to
provide very good frequency resolution in the neighborhood of the electron plasma frequency and
upper hybrid resonance frequency. The step frequency receiver consisted of 8 narrow band filters
(+/-5% band-width) which were sequentially switched into a log compressor. The  log compressor
provided a 0 to 5 volt analog voltage, SFR, to the spacecraft encoder. The switch (S4) position was
controlled by clock lines from the spacecraft encoder and was stepped through 8 frequencies, 13.3,
17.8, 23.7, 31.1, 42.2, 56.2, 100, and 178 kHz, at a rate of four frequencies per telemetry frame
(5.76 seconds). The log compressor provided a 0 to 5 volt analog voltage, SFR, to the spacecraft
encoder which was proportional to the logarithm of the signal strength over a dynamic range of 100
db.
           The 8-channel spectrum analyzer  provided relatively coarse frequency spectrum
measurements of both electric and magnetic fields over a broad frequency range of 1.0 Hz to 10.0
kHz. The primary purpose of the 8-channel spectrum analyzer was to provide field strength
measurements to complement the high-resolution frequency-time spectra from the wide-band receiver.
           Switches S1 and S2 were controlled by clock lines from the spacecraft encoder and
commutate the filter outputs to two log compressors which provided field strength measurements SA-1
and SA-2 (0 to 5 volts) to the spacecraft encoder. These outputs were sampled twice per telemetry
frame. Switch S3, which was controlled by a clock line, commutates the electric and magnetic field
signals to the 8-channel spectrum analyzer.
          Approximately every 5 minutes the impedance of the electric antenna was determined at a
frequency of 17 Hz by driving a small AC current into the antennas and measuring the resultant
voltage on the antennas with the 8-channel spectrum analyzer. The 17 Hz oscillator was gated on for
1 frame out of every 64 frames by a clock line.
           Immediately following the impedance measurement the pulser circuit produced a 10 volt
pulse with a duration of 20 micro- seconds. This pulse was to stimulate local plasma resonances,
such as plasma oscillation, from which the electron density could be determined. A pulse of +10
volts was applied to one antenna element and a -10 volt pulse was applied to the opposite antenna
element. The pulser was switched on by command. The pulser was on when the experiment was in VLF45
mode and off when the experiment was in the VLF10 mode. The pulser voltage was coupled to the
antenna through a 220 pf capacitor which would have allowed some meaningful data to be obtained from
the experiment even if the pulser output were to short to ground. The pulse was applied at the end
of the impedance measurement frame.
 The potential difference between the electric antenna elements was amplified by a high input
impedance differential amplifier to provide a 0 to 5 volt analog voltage, V-Diff, to the spacecraft
encoder. As the spacecraft rotated the potential difference between the antenna elements  varied
sinusoidally at the spacecraft rotation rate, with an amplitude proportional to the electric field
strength and a phase determined by the direction of the electric field. The frequency response of
the differential amplifier was 0.05 Hz to 10 Hz and included the entire range of spin rates expected
as the antenna was deployed. The V-Diff signal was sampled 6 times each frame by the encoder. The
gain of the differential amplifier could be controlled by command to provide dynamic ranges of
+/-0.5 and +/-8.0 volts for the antenna potential difference measurements.
           Signals from the electric antenna in the frequency range from 10 kHz to 200 kHz were
analyzed by the narrow band step frequency receiver. The primary purpose of this receiver was to
provide very good frequency resolution in the neighborhood of the electron plasma frequency and
upper hybrid resonance frequency. The step frequency receiver consisted of 8 narrow band filters
(+/-5% band-width) which were sequentially switched into a log compressor. The  log compressor
provided a 0 to 5 volt analog voltage, SFR, to the spacecraft encoder. The switch (S4) position was
controlled by clock lines from the spacecraft encoder and was stepped through 8 frequencies, 13.3,
17.8, 23.7, 31.1, 42.2, 56.2, 100, and 178 kHz, at a rate of four frequencies per telemetry frame
(5.76 seconds). The log compressor provided a 0 to 5 volt analog voltage, SFR, to the spacecraft
encoder which was proportional to the logarithm of the signal strength over a dynamic range of 100
db.
           The 8-channel spectrum analyzer  provided relatively coarse frequency spectrum
measurements of both electric and magnetic fields over a broad frequency range of 1.0 Hz to 10.0
kHz. The primary purpose of the 8-channel spectrum analyzer was to provide field strength
measurements to complement the high-resolution frequency-time spectra from the wide-band receiver.
           Switches S1 and S2 were controlled by clock lines from the spacecraft encoder and
commutate the filter outputs to two log compressors which provided field strength measurements SA-1
and SA-2 (0 to 5 volts) to the spacecraft encoder. These outputs were sampled twice per telemetry
frame. Switch S3, which was controlled by a clock line, commutates the electric and magnetic field
signals to the 8-channel spectrum analyzer.
          Approximately every 5 minutes the impedance of the electric antenna was determined at a
frequency of 17 Hz by driving a small AC current into the antennas and measuring the resultant
voltage on the antennas with the 8-channel spectrum analyzer. The 17 Hz oscillator was gated on for
1 frame out of every 64 frames by a clock line.
           Immediately following the impedance measurement the pulser circuit produced a 10 volt
pulse with a duration of 20 micro- seconds. This pulse was to stimulate local plasma resonances,
such as plasma oscillation, from which the electron density could be determined. A pulse of +10
volts was applied to one antenna element and a -10 volt pulse was applied to the opposite antenna
element. The pulser was switched on by command. The pulser was on when the experiment was in VLF45
mode and off when the experiment was in the VLF10 mode. The pulser voltage was coupled to the
antenna through a 220 pf capacitor which would have allowed some meaningful data to be obtained from
the experiment even if the pulser output were to short to ground. The pulse was applied at the end
of the impedance measurement frame.


Modification History
CDF created Jan 1999 by Mona Kessel
modified Aug 1999 by Mona Kessel, Carolyn Ng
modified Oct 1999 by Mona Kessel
modified Nov 1999 by Mona Kessel, final for archiving


Variable Notes

Active (=1) vs Passive (=0) Indicator
Active emissions only affect the Electric Field measurements at 17.8 Hz and 56.8
Hz


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I1_AV_ACN
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_ADL
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_SNT
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_ULA
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_AME
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_BRZ
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_BUR
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_BRZ
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_CNA
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_ULA
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_BUR
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_KER
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_KRU
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_KSH
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_KWA
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_LAU
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_LIM
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_ODG
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_ORR
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_OTT
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_QUI
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_RES
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_SNT
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_SOD
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_SOL
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_SYO
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_TRO
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_TRO
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_ULA
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_AV_WNK
Description
This ionogram was digitized from the original ISIS 1 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1998


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I1_C9_I100
Description
Derived from I100 in CDAW9 DB
Data for all CDAW9 events A-E.


Modification History
Converted from CDAWeb Feb 2000




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I1_C9_I102
Description
Derived from I102 in CDAW9 DB.
Data for all CDAW9 events A-E.
Spin period is 3.041 sec.3
The Electron Spectrometer produces a distribution function every 0.5 sec at the top data rate, from
which moments such as density and temperature are calculated.


Modification History
Converted from CDAWeb Feb 2000




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I1_C9_I103
Description
Derived from i103 in CDAW9 DB.
Data for all CDAW9 events A-E.
Proton plasma parameters were obtained as moments of the distribution function every 128 s.  For
densities below 0.1/cc, higher-order moments are not always reliable.  To convert temperature values
from eV to K, multiply by 1.1605E+4.


Modification History
Converted from CDAWeb Feb 2000




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I1_C9_I104
Description
Derived from i104 in CDAW9 DB.
Data for all CDAW9 events A-E.
The data points are 4 seconds apart, but they are averages over 12 seconds.     
There are a few bad data points for the GSM coordinate values in event A.


Modification History
Converted to CDAWeb Feb 2000




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I1_C9_I110
Description
Derived from i110 in CDAW9 DB.
Data for all CDAW9 events A-E.
Spin period is 3.041 sec. 
Measurements of energetic particles were made by essentially identical instrumentation on the ISEE-1
and -2 Mother/Daughter spacecraft.  Four fixed voltage electrostatic analyzers measure ~1.5 keV and
~6 keV electrons and protons (2e, 2p, 6e, 6p), and two semiconductor telescopes measure e and p
fluxes above 15 keV.   
One of these telescopes (FT) has a thin foil cover to stop low energy protons; the open telescope
(OT) counts both electrons and protons.   
The detectors' view directions are along the spin axis (nominally normal to the ecliptic plane),
except for the FT which looks 15 deg from the spin axis.  This minimizes spin modulation effects
that could confuse comparison of features seen at both spacecraft.


Modification History
Converted to CDAWeb Feb 2000




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I1_C9_I1MD
Description
Data derived from CDAW9 I1MD dataset.
Data for all CDAW9 events A-E.


Modification History
Converted to CDAWeb Feb 2000




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I2_AV_ACN
Description
This ionogram was digitized from the original ISIS 2 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.


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I2_AV_ADL
Description
A 7-track ISIS 2 analog telemetry tape from Ottawa (#561) has been 
digitized using the GSFC facilities of the Data Evaluation Laboratory 
(DEL) within the Mission Operations and Data Systems Directorate (Code 
500) at Goddard.  The digitization was performed using an A/D 
converter board and software device driver compatible with the OS/2 
operating system used by the 486-based Programmable Telemetry 
Processor (PTP) associated software has been installed on their PTP 
and de-bugged so that we now have a working system for making digital 
ISIS ionograms directly from the telemetry tapes.  Earlier, we 
successfully digitized the PCM and NASA 36 bit time-code data from 
this same tape. The ionograms were digitized at the rate of 40,000 
16-bit samples/sec. This sample rate is higher than the Nyquist 
frequency of 30 kHz appropriate for the post-detection ISIS 2 
sounder-receiver video output which extends from DC to 15 kHz (see p. 
50 of the 1971 ISIS 2 report by Daniels).  The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (ct/2) interval of 3.747 km.  With the ISIS 2 prf of 45 
sounder pulses/s, there are (1/45)/(2.5**(-5)) = 888.89 samples 
between each of the approximately 1015 sounder pulses per ionogram 
(including the fixed-frequency portion) or nearly 10**6 16-bit 
samples/ionogram (approximately 1.8 MBytes) for just the 
sounder-receiver video data. Adding header information, and the pcm 
data containing data from the other instruments, yields about 2 MBytes 
of data for the 22.5 s period corresponding to one ionogram. Two steps 
were taken in order to reduce this large volume of nearly 2 
MBytes/ionogram.  First, every four 25 microsecond samples following 
the sounder pulse were averaged.  Second, the 16 bit samples were 
reduced to 8 bit samples.  The first step decreased the apparent-range 
resolution to 15 km, but yielded high-quality ionograms because of the 
improved S/N due to the averaging.


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I2_AV_AME
Description
This ionogram was digitized from the original ISIS 2 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.


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I2_AV_BRZ
Description
A 7-track ISIS 2 analog telemetry tape from Ottawa (#561) has been 
digitized using the GSFC facilities of the Data Evaluation Laboratory 
(DEL) within the Mission Operations and Data Systems Directorate (Code 
500) at Goddard.  The digitization was performed using an A/D 
converter board and software device driver compatible with the OS/2 
operating system used by the 486-based Programmable Telemetry 
Processor (PTP) associated software has been installed on their PTP 
and de-bugged so that we now have a working system for making digital 
ISIS ionograms directly from the telemetry tapes.  Earlier, we 
successfully digitized the PCM and NASA 36 bit time-code data from 
this same tape. The ionograms were digitized at the rate of 40,000 
16-bit samples/sec. This sample rate is higher than the Nyquist 
frequency of 30 kHz appropriate for the post-detection ISIS 2 
sounder-receiver video output which extends from DC to 15 kHz (see p. 
50 of the 1971 ISIS 2 report by Daniels).  The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (ct/2) interval of 3.747 km.  With the ISIS 2 prf of 45 
sounder pulses/s, there are (1/45)/(2.5**(-5)) = 888.89 samples 
between each of the approximately 1015 sounder pulses per ionogram 
(including the fixed-frequency portion) or nearly 10**6 16-bit 
samples/ionogram (approximately 1.8 MBytes) for just the 
sounder-receiver video data. Adding header information, and the pcm 
data containing data from the other instruments, yields about 2 MBytes 
of data for the 22.5 s period corresponding to one ionogram. Two steps 
were taken in order to reduce this large volume of nearly 2 
MBytes/ionogram.  First, every four 25 microsecond samples following 
the sounder pulse were averaged.  Second, the 16 bit samples were 
reduced to 8 bit samples.  The first step decreased the apparent-range 
resolution to 15 km, but yielded high-quality ionograms because of the 
improved S/N due to the averaging.


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I2_AV_BUR
Description
A 7-track ISIS 2 analog telemetry tape from Ottawa (#561) has been 
digitized using the GSFC facilities of the Data Evaluation Laboratory 
(DEL) within the Mission Operations and Data Systems Directorate (Code 
500) at Goddard.  The digitization was performed using an A/D 
converter board and software device driver compatible with the OS/2 
operating system used by the 486-based Programmable Telemetry 
Processor (PTP) associated software has been installed on their PTP 
and de-bugged so that we now have a working system for making digital 
ISIS ionograms directly from the telemetry tapes.  Earlier, we 
successfully digitized the PCM and NASA 36 bit time-code data from 
this same tape. The ionograms were digitized at the rate of 40,000 
16-bit samples/sec. This sample rate is higher than the Nyquist 
frequency of 30 kHz appropriate for the post-detection ISIS 2 
sounder-receiver video output which extends from DC to 15 kHz (see p. 
50 of the 1971 ISIS 2 report by Daniels).  The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (ct/2) interval of 3.747 km.  With the ISIS 2 prf of 45 
sounder pulses/s, there are (1/45)/(2.5**(-5)) = 888.89 samples 
between each of the approximately 1015 sounder pulses per ionogram 
(including the fixed-frequency portion) or nearly 10**6 16-bit 
samples/ionogram (approximately 1.8 MBytes) for just the 
sounder-receiver video data. Adding header information, and the pcm 
data containing data from the other instruments, yields about 2 MBytes 
of data for the 22.5 s period corresponding to one ionogram. Two steps 
were taken in order to reduce this large volume of nearly 2 
MBytes/ionogram.  First, every four 25 microsecond samples following 
the sounder pulse were averaged.  Second, the 16 bit samples were 
reduced to 8 bit samples.  The first step decreased the apparent-range 
resolution to 15 km, but yielded high-quality ionograms because of the 
improved S/N due to the averaging.


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I2_AV_CNA
Description
A 7-track ISIS 2 analog telemetry tape from Ottawa (#561) has been 
digitized using the GSFC facilities of the Data Evaluation Laboratory 
(DEL) within the Mission Operations and Data Systems Directorate (Code 
500) at Goddard.  The digitization was performed using an A/D 
converter board and software device driver compatible with the OS/2 
operating system used by the 486-based Programmable Telemetry 
Processor (PTP) associated software has been installed on their PTP 
and de-bugged so that we now have a working system for making digital 
ISIS ionograms directly from the telemetry tapes.  Earlier, we 
successfully digitized the PCM and NASA 36 bit time-code data from 
this same tape. The ionograms were digitized at the rate of 40,000 
16-bit samples/sec. This sample rate is higher than the Nyquist 
frequency of 30 kHz appropriate for the post-detection ISIS 2 
sounder-receiver video output which extends from DC to 15 kHz (see p. 
50 of the 1971 ISIS 2 report by Daniels).  The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (ct/2) interval of 3.747 km.  With the ISIS 2 prf of 45 
sounder pulses/s, there are (1/45)/(2.5**(-5)) = 888.89 samples 
between each of the approximately 1015 sounder pulses per ionogram 
(including the fixed-frequency portion) or nearly 10**6 16-bit 
samples/ionogram (approximately 1.8 MBytes) for just the 
sounder-receiver video data. Adding header information, and the pcm 
data containing data from the other instruments, yields about 2 MBytes 
of data for the 22.5 s period corresponding to one ionogram. Two steps 
were taken in order to reduce this large volume of nearly 2 
MBytes/ionogram.  First, every four 25 microsecond samples following 
the sounder pulse were averaged.  Second, the 16 bit samples were 
reduced to 8 bit samples.  The first step decreased the apparent-range 
resolution to 15 km, but yielded high-quality ionograms because of the 
improved S/N due to the averaging.


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I2_AV_KER
Description
A 7-track ISIS 2 analog telemetry tape from Ottawa (#561) has been 
digitized using the GSFC facilities of the Data Evaluation Laboratory 
(DEL) within the Mission Operations and Data Systems Directorate (Code 
500) at Goddard.  The digitization was performed using an A/D 
converter board and software device driver compatible with the OS/2 
operating system used by the 486-based Programmable Telemetry 
Processor (PTP) associated software has been installed on their PTP 
and de-bugged so that we now have a working system for making digital 
ISIS ionograms directly from the telemetry tapes.  Earlier, we 
successfully digitized the PCM and NASA 36 bit time-code data from 
this same tape. The ionograms were digitized at the rate of 40,000 
16-bit samples/sec. This sample rate is higher than the Nyquist 
frequency of 30 kHz appropriate for the post-detection ISIS 2 
sounder-receiver video output which extends from DC to 15 kHz (see p. 
50 of the 1971 ISIS 2 report by Daniels).  The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (ct/2) interval of 3.747 km.  With the ISIS 2 prf of 45 
sounder pulses/s, there are (1/45)/(2.5**(-5)) = 888.89 samples 
between each of the approximately 1015 sounder pulses per ionogram 
(including the fixed-frequency portion) or nearly 10**6 16-bit 
samples/ionogram (approximately 1.8 MBytes) for just the 
sounder-receiver video data. Adding header information, and the pcm 
data containing data from the other instruments, yields about 2 MBytes 
of data for the 22.5 s period corresponding to one ionogram. Two steps 
were taken in order to reduce this large volume of nearly 2 
MBytes/ionogram.  First, every four 25 microsecond samples following 
the sounder pulse were averaged.  Second, the 16 bit samples were 
reduced to 8 bit samples.  The first step decreased the apparent-range 
resolution to 15 km, but yielded high-quality ionograms because of the 
improved S/N due to the averaging.


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I2_AV_KRU
Description
A 7-track ISIS 2 analog telemetry tape from Ottawa (#561) has been 
digitized using the GSFC facilities of the Data Evaluation Laboratory 
(DEL) within the Mission Operations and Data Systems Directorate (Code 
500) at Goddard.  The digitization was performed using an A/D 
converter board and software device driver compatible with the OS/2 
operating system used by the 486-based Programmable Telemetry 
Processor (PTP) associated software has been installed on their PTP 
and de-bugged so that we now have a working system for making digital 
ISIS ionograms directly from the telemetry tapes.  Earlier, we 
successfully digitized the PCM and NASA 36 bit time-code data from 
this same tape. The ionograms were digitized at the rate of 40,000 
16-bit samples/sec. This sample rate is higher than the Nyquist 
frequency of 30 kHz appropriate for the post-detection ISIS 2 
sounder-receiver video output which extends from DC to 15 kHz (see p. 
50 of the 1971 ISIS 2 report by Daniels).  The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (ct/2) interval of 3.747 km.  With the ISIS 2 prf of 45 
sounder pulses/s, there are (1/45)/(2.5**(-5)) = 888.89 samples 
between each of the approximately 1015 sounder pulses per ionogram 
(including the fixed-frequency portion) or nearly 10**6 16-bit 
samples/ionogram (approximately 1.8 MBytes) for just the 
sounder-receiver video data. Adding header information, and the pcm 
data containing data from the other instruments, yields about 2 MBytes 
of data for the 22.5 s period corresponding to one ionogram. Two steps 
were taken in order to reduce this large volume of nearly 2 
MBytes/ionogram.  First, every four 25 microsecond samples following 
the sounder pulse were averaged.  Second, the 16 bit samples were 
reduced to 8 bit samples.  The first step decreased the apparent-range 
resolution to 15 km, but yielded high-quality ionograms because of the 
improved S/N due to the averaging.


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I2_AV_KSH
Description
A 7-track ISIS 2 analog telemetry tape from Ottawa (#561) has been 
digitized using the GSFC facilities of the Data Evaluation Laboratory 
(DEL) within the Mission Operations and Data Systems Directorate (Code 
500) at Goddard.  The digitization was performed using an A/D 
converter board and software device driver compatible with the OS/2 
operating system used by the 486-based Programmable Telemetry 
Processor (PTP) associated software has been installed on their PTP 
and de-bugged so that we now have a working system for making digital 
ISIS ionograms directly from the telemetry tapes.  Earlier, we 
successfully digitized the PCM and NASA 36 bit time-code data from 
this same tape. The ionograms were digitized at the rate of 40,000 
16-bit samples/sec. This sample rate is higher than the Nyquist 
frequency of 30 kHz appropriate for the post-detection ISIS 2 
sounder-receiver video output which extends from DC to 15 kHz (see p. 
50 of the 1971 ISIS 2 report by Daniels).  The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (ct/2) interval of 3.747 km.  With the ISIS 2 prf of 45 
sounder pulses/s, there are (1/45)/(2.5**(-5)) = 888.89 samples 
between each of the approximately 1015 sounder pulses per ionogram 
(including the fixed-frequency portion) or nearly 10**6 16-bit 
samples/ionogram (approximately 1.8 MBytes) for just the 
sounder-receiver video data. Adding header information, and the pcm 
data containing data from the other instruments, yields about 2 MBytes 
of data for the 22.5 s period corresponding to one ionogram. Two steps 
were taken in order to reduce this large volume of nearly 2 
MBytes/ionogram.  First, every four 25 microsecond samples following 
the sounder pulse were averaged.  Second, the 16 bit samples were 
reduced to 8 bit samples.  The first step decreased the apparent-range 
resolution to 15 km, but yielded high-quality ionograms because of the 
improved S/N due to the averaging.


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I2_AV_KWA
Description
This ionogram was digitized from the original ISIS 2 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.


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I2_AV_LAU
Description
A 7-track ISIS 2 analog telemetry tape from Ottawa (#561) has been 
digitized using the GSFC facilities of the Data Evaluation Laboratory 
(DEL) within the Mission Operations and Data Systems Directorate (Code 
500) at Goddard.  The digitization was performed using an A/D 
converter board and software device driver compatible with the OS/2 
operating system used by the 486-based Programmable Telemetry 
Processor (PTP) associated software has been installed on their PTP 
and de-bugged so that we now have a working system for making digital 
ISIS ionograms directly from the telemetry tapes.  Earlier, we 
successfully digitized the PCM and NASA 36 bit time-code data from 
this same tape. The ionograms were digitized at the rate of 40,000 
16-bit samples/sec. This sample rate is higher than the Nyquist 
frequency of 30 kHz appropriate for the post-detection ISIS 2 
sounder-receiver video output which extends from DC to 15 kHz (see p. 
50 of the 1971 ISIS 2 report by Daniels).  The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (ct/2) interval of 3.747 km.  With the ISIS 2 prf of 45 
sounder pulses/s, there are (1/45)/(2.5**(-5)) = 888.89 samples 
between each of the approximately 1015 sounder pulses per ionogram 
(including the fixed-frequency portion) or nearly 10**6 16-bit 
samples/ionogram (approximately 1.8 MBytes) for just the 
sounder-receiver video data. Adding header information, and the pcm 
data containing data from the other instruments, yields about 2 MBytes 
of data for the 22.5 s period corresponding to one ionogram. Two steps 
were taken in order to reduce this large volume of nearly 2 
MBytes/ionogram.  First, every four 25 microsecond samples following 
the sounder pulse were averaged.  Second, the 16 bit samples were 
reduced to 8 bit samples.  The first step decreased the apparent-range 
resolution to 15 km, but yielded high-quality ionograms because of the 
improved S/N due to the averaging.


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I2_AV_LIM
Description
This ionogram was digitized from the original ISIS 2 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.


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I2_AV_ODG
Description
A 7-track ISIS 2 analog telemetry tape from Ottawa (#561) has been 
digitized using the GSFC facilities of the Data Evaluation Laboratory 
(DEL) within the Mission Operations and Data Systems Directorate (Code 
500) at Goddard.  The digitization was performed using an A/D 
converter board and software device driver compatible with the OS/2 
operating system used by the 486-based Programmable Telemetry 
Processor (PTP) associated software has been installed on their PTP 
and de-bugged so that we now have a working system for making digital 
ISIS ionograms directly from the telemetry tapes.  Earlier, we 
successfully digitized the PCM and NASA 36 bit time-code data from 
this same tape. The ionograms were digitized at the rate of 40,000 
16-bit samples/sec. This sample rate is higher than the Nyquist 
frequency of 30 kHz appropriate for the post-detection ISIS 2 
sounder-receiver video output which extends from DC to 15 kHz (see p. 
50 of the 1971 ISIS 2 report by Daniels).  The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (ct/2) interval of 3.747 km.  With the ISIS 2 prf of 45 
sounder pulses/s, there are (1/45)/(2.5**(-5)) = 888.89 samples 
between each of the approximately 1015 sounder pulses per ionogram 
(including the fixed-frequency portion) or nearly 10**6 16-bit 
samples/ionogram (approximately 1.8 MBytes) for just the 
sounder-receiver video data. Adding header information, and the pcm 
data containing data from the other instruments, yields about 2 MBytes 
of data for the 22.5 s period corresponding to one ionogram. Two steps 
were taken in order to reduce this large volume of nearly 2 
MBytes/ionogram.  First, every four 25 microsecond samples following 
the sounder pulse were averaged.  Second, the 16 bit samples were 
reduced to 8 bit samples.  The first step decreased the apparent-range 
resolution to 15 km, but yielded high-quality ionograms because of the 
improved S/N due to the averaging.


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I2_AV_ORR
Description
A 7-track ISIS 2 analog telemetry tape from Ottawa (#561) has been 
digitized using the GSFC facilities of the Data Evaluation Laboratory 
(DEL) within the Mission Operations and Data Systems Directorate (Code 
500) at Goddard.  The digitization was performed using an A/D 
converter board and software device driver compatible with the OS/2 
operating system used by the 486-based Programmable Telemetry 
Processor (PTP) associated software has been installed on their PTP 
and de-bugged so that we now have a working system for making digital 
ISIS ionograms directly from the telemetry tapes.  Earlier, we 
successfully digitized the PCM and NASA 36 bit time-code data from 
this same tape. The ionograms were digitized at the rate of 40,000 
16-bit samples/sec. This sample rate is higher than the Nyquist 
frequency of 30 kHz appropriate for the post-detection ISIS 2 
sounder-receiver video output which extends from DC to 15 kHz (see p. 
50 of the 1971 ISIS 2 report by Daniels).  The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (ct/2) interval of 3.747 km.  With the ISIS 2 prf of 45 
sounder pulses/s, there are (1/45)/(2.5**(-5)) = 888.89 samples 
between each of the approximately 1015 sounder pulses per ionogram 
(including the fixed-frequency portion) or nearly 10**6 16-bit 
samples/ionogram (approximately 1.8 MBytes) for just the 
sounder-receiver video data. Adding header information, and the pcm 
data containing data from the other instruments, yields about 2 MBytes 
of data for the 22.5 s period corresponding to one ionogram. Two steps 
were taken in order to reduce this large volume of nearly 2 
MBytes/ionogram.  First, every four 25 microsecond samples following 
the sounder pulse were averaged.  Second, the 16 bit samples were 
reduced to 8 bit samples.  The first step decreased the apparent-range 
resolution to 15 km, but yielded high-quality ionograms because of the 
improved S/N due to the averaging.


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I2_AV_OTT
Description
A 7-track ISIS 2 analog telemetry tape from Ottawa (#561) has been 
digitized using the GSFC facilities of the Data Evaluation Laboratory 
(DEL) within the Mission Operations and Data Systems Directorate (Code 
500) at Goddard.  The digitization was performed using an A/D 
converter board and software device driver compatible with the OS/2 
operating system used by the 486-based Programmable Telemetry 
Processor (PTP) associated software has been installed on their PTP 
and de-bugged so that we now have a working system for making digital 
ISIS ionograms directly from the telemetry tapes.  Earlier, we 
successfully digitized the PCM and NASA 36 bit time-code data from 
this same tape. The ionograms were digitized at the rate of 40,000 
16-bit samples/sec. This sample rate is higher than the Nyquist 
frequency of 30 kHz appropriate for the post-detection ISIS 2 
sounder-receiver video output which extends from DC to 15 kHz (see p. 
50 of the 1971 ISIS 2 report by Daniels).  The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (ct/2) interval of 3.747 km.  With the ISIS 2 prf of 45 
sounder pulses/s, there are (1/45)/(2.5**(-5)) = 888.89 samples 
between each of the approximately 1015 sounder pulses per ionogram 
(including the fixed-frequency portion) or nearly 10**6 16-bit 
samples/ionogram (approximately 1.8 MBytes) for just the 
sounder-receiver video data. Adding header information, and the pcm 
data containing data from the other instruments, yields about 2 MBytes 
of data for the 22.5 s period corresponding to one ionogram. Two steps 
were taken in order to reduce this large volume of nearly 2 
MBytes/ionogram.  First, every four 25 microsecond samples following 
the sounder pulse were averaged.  Second, the 16 bit samples were 
reduced to 8 bit samples.  The first step decreased the apparent-range 
resolution to 15 km, but yielded high-quality ionograms because of the 
improved S/N due to the averaging.


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I2_AV_QUI
Description
A 7-track ISIS 2 analog telemetry tape from Ottawa (#561) has been 
digitized using the GSFC facilities of the Data Evaluation Laboratory 
(DEL) within the Mission Operations and Data Systems Directorate (Code 
500) at Goddard.  The digitization was performed using an A/D 
converter board and software device driver compatible with the OS/2 
operating system used by the 486-based Programmable Telemetry 
Processor (PTP) associated software has been installed on their PTP 
and de-bugged so that we now have a working system for making digital 
ISIS ionograms directly from the telemetry tapes.  Earlier, we 
successfully digitized the PCM and NASA 36 bit time-code data from 
this same tape. The ionograms were digitized at the rate of 40,000 
16-bit samples/sec. This sample rate is higher than the Nyquist 
frequency of 30 kHz appropriate for the post-detection ISIS 2 
sounder-receiver video output which extends from DC to 15 kHz (see p. 
50 of the 1971 ISIS 2 report by Daniels).  The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (ct/2) interval of 3.747 km.  With the ISIS 2 prf of 45 
sounder pulses/s, there are (1/45)/(2.5**(-5)) = 888.89 samples 
between each of the approximately 1015 sounder pulses per ionogram 
(including the fixed-frequency portion) or nearly 10**6 16-bit 
samples/ionogram (approximately 1.8 MBytes) for just the 
sounder-receiver video data. Adding header information, and the pcm 
data containing data from the other instruments, yields about 2 MBytes 
of data for the 22.5 s period corresponding to one ionogram. Two steps 
were taken in order to reduce this large volume of nearly 2 
MBytes/ionogram.  First, every four 25 microsecond samples following 
the sounder pulse were averaged.  Second, the 16 bit samples were 
reduced to 8 bit samples.  The first step decreased the apparent-range 
resolution to 15 km, but yielded high-quality ionograms because of the 
improved S/N due to the averaging.


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I2_AV_RES
Description
A 7-track ISIS 2 analog telemetry tape from Ottawa (#561) has been 
digitized using the GSFC facilities of the Data Evaluation Laboratory 
(DEL) within the Mission Operations and Data Systems Directorate (Code 
500) at Goddard.  The digitization was performed using an A/D 
converter board and software device driver compatible with the OS/2 
operating system used by the 486-based Programmable Telemetry 
Processor (PTP) associated software has been installed on their PTP 
and de-bugged so that we now have a working system for making digital 
ISIS ionograms directly from the telemetry tapes.  Earlier, we 
successfully digitized the PCM and NASA 36 bit time-code data from 
this same tape. The ionograms were digitized at the rate of 40,000 
16-bit samples/sec. This sample rate is higher than the Nyquist 
frequency of 30 kHz appropriate for the post-detection ISIS 2 
sounder-receiver video output which extends from DC to 15 kHz (see p. 
50 of the 1971 ISIS 2 report by Daniels).  The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (ct/2) interval of 3.747 km.  With the ISIS 2 prf of 45 
sounder pulses/s, there are (1/45)/(2.5**(-5)) = 888.89 samples 
between each of the approximately 1015 sounder pulses per ionogram 
(including the fixed-frequency portion) or nearly 10**6 16-bit 
samples/ionogram (approximately 1.8 MBytes) for just the 
sounder-receiver video data. Adding header information, and the pcm 
data containing data from the other instruments, yields about 2 MBytes 
of data for the 22.5 s period corresponding to one ionogram. Two steps 
were taken in order to reduce this large volume of nearly 2 
MBytes/ionogram.  First, every four 25 microsecond samples following 
the sounder pulse were averaged.  Second, the 16 bit samples were 
reduced to 8 bit samples.  The first step decreased the apparent-range 
resolution to 15 km, but yielded high-quality ionograms because of the 
improved S/N due to the averaging.


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I2_AV_SNT
Description
This ionogram was digitized from the original ISIS 2 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.


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I2_AV_SOD
Description
This ionogram was digitized from the original ISIS 2 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.


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I2_AV_SOL
Description
This ionogram was digitized from the original ISIS 2 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.


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I2_AV_SYO
Description
A 7-track ISIS 2 analog telemetry tape from Ottawa (#561) has been 
digitized using the GSFC facilities of the Data Evaluation Laboratory 
(DEL) within the Mission Operations and Data Systems Directorate (Code 
500) at Goddard.  The digitization was performed using an A/D 
converter board and software device driver compatible with the OS/2 
operating system used by the 486-based Programmable Telemetry 
Processor (PTP) associated software has been installed on their PTP 
and de-bugged so that we now have a working system for making digital 
ISIS ionograms directly from the telemetry tapes.  Earlier, we 
successfully digitized the PCM and NASA 36 bit time-code data from 
this same tape. The ionograms were digitized at the rate of 40,000 
16-bit samples/sec. This sample rate is higher than the Nyquist 
frequency of 30 kHz appropriate for the post-detection ISIS 2 
sounder-receiver video output which extends from DC to 15 kHz (see p. 
50 of the 1971 ISIS 2 report by Daniels).  The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (ct/2) interval of 3.747 km.  With the ISIS 2 prf of 45 
sounder pulses/s, there are (1/45)/(2.5**(-5)) = 888.89 samples 
between each of the approximately 1015 sounder pulses per ionogram 
(including the fixed-frequency portion) or nearly 10**6 16-bit 
samples/ionogram (approximately 1.8 MBytes) for just the 
sounder-receiver video data. Adding header information, and the pcm 
data containing data from the other instruments, yields about 2 MBytes 
of data for the 22.5 s period corresponding to one ionogram. Two steps 
were taken in order to reduce this large volume of nearly 2 
MBytes/ionogram.  First, every four 25 microsecond samples following 
the sounder pulse were averaged.  Second, the 16 bit samples were 
reduced to 8 bit samples.  The first step decreased the apparent-range 
resolution to 15 km, but yielded high-quality ionograms because of the 
improved S/N due to the averaging.


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
Interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.
Altitude
Virtual variable.


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I2_AV_TRO
Description
This ionogram was digitized from the original ISIS 2 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.


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I2_AV_ULA
Description
This ionogram was digitized from the original ISIS 2 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.


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I2_AV_WNK
Description
This ionogram was digitized from the original ISIS 2 analog 
telemetry data on 7-track tape using the facilities of the Data 
Evaluation Laboratory at GSFC (Code 500). This data restoration 
project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were 
digitized at the rate of 40,000 16-bit samples/sec. This sample rate is 
higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 
kHz provides a measurement every 25 microseconds corresponding to an 
apparent range (c*t/2) interval of 3.747 km. Each ionogram consists 
of a fixed-frequency and and a swept-frequency portion. The time 
resolution is typically 24 seconds. More information can be found 
at http://nssdc/space/isis/isis-status.html


Modification History
created April 1995


Variable Notes

scan line number of start of swept portion
seperates the fixed and swept portions
msec after frame sync
time of frequency markers
interpolated fixed & sweep frequencies
This variable could be used as x-axis on amplitude spectrograms if fixed part is
subtracted.


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I2_C9_I204
Description
Derived from i204 in CDAW9 DB.
Data for all CDAW9 events A-E.
The data points are 4 seconds apart, but they are averages over 12 seconds.     
There are a few bad data points for the GSM coordinate values in event A.


Modification History
Converted to CDAWeb Feb 2000




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I2_C9_I208
Description
Derived from i208 in CDAW9 DB.
Data from all CDAW9 events A-E.
Spin period is 3.019 sec. 
Measurements of energetic particles were made by essentially identical instrumentation on the ISEE-1
and -2 Mother/Daughter spacecraft.  Four fixed voltage electrostatic analyzers measure ~1.5 keV and
~6 keV electrons and protons (2e, 2p, 6e, 6p), and two semiconductor telescopes measure e and p
fluxes above 15 keV.  One of these telescopes (FT) has a thin foil cover to stop low energy protons;
the open telescope (OT) counts both electrons and protons.
The detectors' view directions are along the spin axis (nominally normal to the ecliptic plane),
except for the FT which looks 15 deg from the spin axis.  This minimizes spin modulation effects
that could confuse comparison of features seen at both spacecraft.


Modification History
Converted to CDAWeb Feb 2000




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I8_ED_M3
Description
These CDFs contain the IMP-8 magnetic field values in both the GSE and GSM coord
inate systems, in both polar and cartesian coordinates.  The variances and s/c p
osition coordinates are also provided. The IMP-8 s/c is in the solar wind for Ev
ents A, B, and E, and in the magnetosphere for Event C.  During Event D, IMP-8 c
rossed the bow shock from the magnetosheath into the solar wind at 14 h UT.


Modification History
Null




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I8_ED_PA
Description
These CDFs contain the IMP-8 proton plasma data.  Temperatures are expressed as 
thermal velocity; to convert to Kelvin, multiply (value in km/sec) squared, by 6
0.1.  Flow angles are with respect to the s/c axes. The IMP-8 s/c is in the sola
r wind for Events A, B, and E, and in the magnetosphere for Event C.  During Eve
nt D, IMP-8 crossed the bow shock from the magnetosheath into the solar wind at 
14 h UT.


Modification History




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I8_ED_PLA
Description
Time resolution: approx 1 min


Modification History
Data for 9/8/92 to 7/31/96 created at the NSSDC from ASCII files provided by the PI, July, 1996
MIT software Version 3; non-linear, least squares analysis, May, 1994
MIT software Version 5; minor fixes, position in Re, July, 1994
MIT software Version 6; minor fixes to previously sent files




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I8_H0_GME
Description
30-min avg flex I8 GME


Modification History
v0.1 (vv01) May/Aug97  orig 30-min design V0.2 (vv02) Nov97  split protons into  two vars by
energies  (not needed virvars) V0.3 (vv03) Jul/Aug98  cleaned up var names & set up for virvars V0.4
(vv04) Aug98  defined virvars for  alternate views




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I8_H0_MAG
Description
This data set was converted to CDF format at NSSDC from the intermediate
 ASCII version (called MAG15_ASCII in NSSDC's near-line NDADS interfaces
), which itself was created at NSSDC by converting the PI-provided 15.36
-sec binary data set (73-078A-01A) to ASCII and simultaneously rejecting
 many little-used data words. With one exception (the number of detail p
oints is omitted), the parameters in this CDF are exactly those included
 in the ASCII data set, which are: time, number of sequences, spacecraft
 position (GSE and GSM), field magnitude, field cartesian components (GS
E and GSM), and the variances and covariances of the GSE field component
 averages. 
 
Unlike the original binary source data set (73-078A-01A), this CDF data 
set and its ASCII version both use a common January 1 = day 1 convention
 throughout. The ASCII version of this data set is accessible from NDADS
 via the SPyCAT interface at: http://nssdc.gsfc.nasa.gov/space/ndads/spy 
cat.html 
 
In making this CDF, an intermediate data file was generated first, which
 duplicates the X components of the position and of the B vector, and in
serts the new values explicitly in the GSM coordinate versions, so that 
the input to the CDF has all three components explicitly given for the G
SM coordinates.


Modification History
Master CDF made 10/19/99 by H. K. Hills, NSSDC.


Variable Notes

Variances; SQRT of diagonal elements Bxx, Byy, Bzz; GSE coordinates 
..


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I8_H1_GME
Description
6-hour avg flex I8 GME


Modification History
v0.1 from H0 Mar02




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I8_K0_MAG
Description
Data: 1.024 minute averages
References: 1. Mish, W. H., and R. P. Lepping, 
Magnetic field experiment data processing systems: 
Explorers 47 and 50, NASA/GSFC, X-694-76-158, Aug. 1976.
2. Ness, N.F., A proposal for the magnetic field experiment for IMPs H and J, 
NASA/GSFC, X-612-66-461, Sept. 1966
3. Scearce, C. S., C. V. Moyer, R. P. Lepping, and N. F. Ness, 
GSFC magnetic field experiments, Explorers 47 and 50, NASA/GSFC, X-695-76-191, 
Oct. 1976, revision in preparation, 1992.
4. Schonstedt, E. O., Saturable measuring device and magnetic core therefor, 
U. S. patent 2916696 (December 1959) and U. S. Patent 2981885 (Apr. 1961)
5. Lepping, R. P., Lazarus, A. J., Moriarty, L. J., Milligan, P., 
Kennon, R. S., McGuire, R. E., and Mish, W. H.
IMP-8 Solar Wind Magnetic Field and Plasma Data in Support of 
Ulysses-Jupiter Encounter: 13-31 Jan. 1992, Oct. 1992


Modification History
Ver. 1.3 oct 92 change by bz components sign change for SC flip 
fixing theta/phi problem.
V1.4 4 Dec 92 changesa)mona5.skt b)c function nadj_hopas called fromj1main to 
temporary fix the sun angle counts to avoid obvious bad values, some negative
V1.5, 5 Mar. 1993 changes SC position vector and distance not averaged but the 
value of first sample, rms vector and scalar based on the four 15.36 sec. 
data values, time of 1 min. avg. mid time of period, field lat-lon values 
based on 1 min avg of field vector (4 samples)
V1.6, 2 June 1993 changessdfu comment containing zerolevels used added, 
zero levels retrieved from calibration file, loop change in nadj_hopas.c 
to prevent infinite loop when hopas array all bad, lib$int_over 
inserted in togama to obviate bad data integer overflow hardcoded 
V1.7, 2 Sep 1993 changes paysta- no data saved when pseudo seq count=0, 
times generated from the page milliseconds of day 
no one min avg if only one sample-STAT15
V1.8, 4 Mar 1994 changes spin2-new default spin topay-spike correction 
j1main- read z corr. and correct sfdu comment togama- subtract z corr. 
new cal. w/ z-corr.
Modified on June 16, 1994 by JT




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I8_K0_PLA
Description
Time resolution: approx 1 min


Modification History
Data for 9/8/92 to 7/31/96 created at the NSSDC from ASCII files provided by the PI, July, 1996
MIT software Version 3; non-linear, least squares analysis, May, 1994
MIT software Version 5; minor fixes, position in Re, July, 1994
MIT software Version 6; minor fixes to previously sent files




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I8_Y0_PRE
Description
GROUP 1    Satellite   Resolution   Factor
            imp8          720         1
                                          
                                          
           Start Time           Stop Time 
           1999 362 00:00       1999 362 23:60   
                                          
                                          
Coord/            Min/Max   Range Filter       Filter
Component   Output Markers  Minimum  Maximum   Mins/Maxes 
GEO Lat      YES      -        -        -           -        -           -   
GEO Lon      YES      -        -        -           -        -           -   
                                          
                                          
Addtnl             Min/Max   Range Filter       Filter
Options     Output Markers  Minimum  Maximum   Mins/Maxes
dEarth       YES      -        -        -           -   
dMagPause    YES      -        -        -           -   
                                          
                                          
Formats and units:                          
    Day/Time format: YYYY DDD HH:MM
    Degrees/Hemisphere format: Decimal degrees with 2 place(s).
        Longitude 0 to 360, latitude -90 to 90.
    Distance format: Earth radii with 2 place(s).


Modification History
Originated 03/14/96




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IA_K0_EPI
No TEXT global attribute. 
Energetic particle fluxesin three energy rangesfrom several sensors. Data areaveraged in 2
min.intervals Status flags show instrument mode.
Full description: http://www.iki.rssi.ru/interball.html


Modification History
created Apr 1997


Variable Notes

Electron Flux, 26-29 keV (DOK-2 firstelectron sensor, fixed)
sensor offset at an angle 180 deg withrespect to the sunward directed spacecraft
spin axis
Electron Flux, 25-28 keV (DOK-2 firstelectron sensor, fixed)
sensor offset at an angle 180 deg withrespect to the sunward directed spacecraft
spin axis
Proton Flux, 18-24 keV (DOK-2 first proton sensor, fixed)
sensor offset at an angle 180 deg withrespect to the sunward directed spacecraft
spin axis
Proton Flux, 20-26 keV (DOK-2 second proton sensor, scan)
The value is taken from the sensorthat can scan the angle's interval 45-180deg
or can be fixed at angles 45, 90,135, 180 deg. with respect to the sunward
directed spacecraft spin axis
Status Flag: energy and positioncoded, see description
Standard flags are used in the case ofdata absence. SFs are set to 11-15
and21-25 for all valid data values ofeach parameter. Most significant digit (1-
low or 2 - high) indicates level of the energy threshold. Higher energy
threshold will be used only in case ofdegradation of a sensor. Less significant
digit indicates sensor orientation ( 1, 2, 3, 4, 5 correspondrespectively to 45,
90, 135, 180 deg.and scan)
Status Flag: energy and positioncoded, see description
Standard flags are used in the case ofdata absence. SFs are set to 11-15
and21-25 for all valid data values ofeach parameter. Most significant digit (1-
low or 2 - high) indicates level of the energy threshold. Higher energy
threshold will be used only in case ofdegradation of a sensor. Less significant
digit indicates sensor orientation ( 1, 2, 3, 4, 5 correspondrespectively to 45,
90, 135, 180 deg.and scan)
Status Flag: energy and position coded, see description
Standard flags are used in the case ofdata absence. SFs are set to 11-15
and21-25 for all valid data values of each parameter. Most significant digit (1-
low or 2 - high) indicates level of the energy threshold. Higher energy
threshold will be used only in case ofdegradation of a sensor. Less significant
digit indicates sensor orientation ( 1, 2, 3, 4, 5 correspondrespectively to 45,
90, 135, 180 deg.and scan)
Status Flag: energy and position coded, see description
Standard flags are used in the case ofdata absence. SFs are set to 11-15
and21-25 for all valid data values of each parameter. Most significant digit (1-
low or 2 - high) indicates level of the energy threshold. Higher energy
threshold will be used only in case ofdegradation of a sensor. Less significant
digit indicates sensor orientation ( 1, 2, 3, 4, 5 correspondrespectively to 45,
90, 135, 180 deg.and scan)


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IA_K0_MFI
No TEXT global attribute. 
Full description: http://www.iki.rssi.ru/interball.html


Modification History
created May 1997


Variable Notes

Magnetic Field average of magnitudes, scalar
2 min. average, IMAP
Magnetic Field Index 
2 min average


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IA_OR_DEF
No TEXT global attribute. 
Full description: http://www.iki.rssi.ru/interball.html


Modification History
created May 1997
edited global attributes Apr 1996




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IG_K0_PCI
Description
References:     1.Troshichev O.A. et al, Planet.Space Sci.,   36, 1095, 1988. 
2.Vennerstrom S. et al,  Report UAG-103, World Data Center A for STP, Boulder, April 1994 



PC-index is an empirical magnetic activity index based on data from single near-pole station (Thule
or Vostok for N or S hemispheres, respectively).
Its derivation procedure is optimized to achieve the best correlation of  PC-index with the solar
wind electric field (SWEF) magnitude ( v*B*sin(teta/2)**2 ). 
The averaged horizontal magnetic disturbance vector (quiet  value subtracted) is projected onto the
optimal direction (defined  empirically for each UT hour and each season based on the best
correlation  with the SWEF) and, after normalization to the equivalent value  of SWEF, it gives the
PC-index (expressed in mV/m). 
Although PC-index is  formally expressed in mV/m, it actually represents the  measure of magnetic
activity, the normalization procedure (to SWEF)  helps to reduce the seasonal/diurnal effects to
facilitate the intercomparison.
The resolution of the northern cap PC-index is 5 min and of the one from southern cap - 15 min.
However, one time scale with the 5 min step is used for both indices and each  15 min averaged value
of southern index is, hence, repeated for three times. 
Full description: http://www.iki.rssi.ru/interball.html


Modification History
created Mar 1996


Variable Notes

Southern Polar Cap magnetic activity index, 'Vostok'
15 min averaged value of southern index is repeated for three times.
Nothern Polar Cap magnetic activity index, 'Thule'
5 min. resolution


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IJ_C9_IJ00
Description
Derived from ij00 dataset in CDAW9 DB.
Data for all CDAW9 events A-E.


Modification History
Converted to CDAWeb Feb 2000




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IJ_C9_IJ01
Description
Derived from ij01 in CDAW9 DB.
Data for all CDAW9 event A-E.
These CDFs contain the IMP-8 magnetic field values in both the GSE and GSM coordinate systems, in
both polar and cartesian coordinates.  The variances and s/c position coordinates are also provided.
 
The IMP-8 s/c is in the solar wind for Events A, B, and E, and in the magnetosphere for Event C. 
During Event D, IMP-8 crossed the bow shock from the magnetosheath into the solar wind at 14 h UT.


Modification History
Converted to CDAWeb Feb 2000.




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IJ_C9_IJ02
Description
Derived from IJ02 CDAW9 dataset.
Data for CDAW9 events A,B,D,E


Modification History
Converted to CDAWeb Feb 2000




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IJ_C9_IJ05
Description
Derived from ij05 in CDAW9 DB.
Data for all CDAW9 events A-E.
The fluxes in this CDF are dimensioned with respect to the azimuthal sector angle parameter, SANG. 
There are 16 22.5-degree azimuthal sectors.  They increase in a counter-clockwise direction and the
values of the beginning edges of the sectors are given in SANG.


Modification History
Converted to CDAWeb Feb 2000




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IJ_C9_IJ08
Description
Derived from IJ08 in CDAW9 DB.
Data for CDAW9 event C only.
sector 1 tailward; contact Lui for validity of electron data.  
Energetic electron fluxes appeared abnormal in some sectors; contact investigator for validity.


Modification History
Converted to CDAWeb Feb 2000




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IJ_C9_IJMD
Description
Derived from IJMD dataset in CDAW9.
Data for all CDAW9 events A-E.


Modification History
 Converted to CDAWeb Feb 2000




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IM_HK_ADS
Description
tbs


Modification History
tbs




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IM_HK_AST
Description
tbs


Modification History
tbs




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IM_HK_COM
Description
tbs


Modification History
tbs




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IM_HK_FSW
Description
tbs


Modification History
tbs




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IM_HK_PWR
Description
tbs


Modification History
tbs




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IM_HK_TML
Description
tbs


Modification History
tbs




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IM_K0_EUV
Description
The logical_file_id stores the name of the CDF file using the ISTP naming convention (source_name /
data_type / descriptor / date / data_version).im_l1_euv_00000000_v01


Variable Notes

Image Time
The time in EPOCH refers to the center of the image in IMAGE. The times shown
here are the actual time of exposure.
---> EUV ion images, as above (movie)
This is a virtual variable computed in read_myCDF
Roll Angle to Magnetic North
Counter-clockwise defined to be the positive direction.  Represents the angle of
rotation of the image field necessary to orient the North magnetic field at the
top of the user's perspective.
IMAGE Position in GEO (geographic) coordinates, 3 components
Geo = geographic coordinates
IMAGE Position in GSM coordinates, 3 components
GSM = geocentric solar magnetospheric coordinates


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IM_K0_GEO
Description
REM - not clear "sun senor" variables should be Z360 dependent - more likely to be scalars
REM - Various orbit parameters should probably be 1d size 3 (for the three components) rather than
size 360 



SKT version 2-December-1999 
Mende et al: Far Ultraviolet Imaging from the IMAGE Spacecraft,Space Sciences Review 1999


Variable Notes

Visible Sun Sensor 1
REM- not clear why this should be a dimensional variable rather than scalar -
may be problem in structure - same note to all other sun sensors
oriention direction cosine
direction of true spin axis at WIC Snapshot Time - REM - should not be 1-d size
360?
oriention direction cosine
direction of true spin axis at WIC Snapshot Time
oriention direction cosine
direction of true spin axis at WIC Snapshot Time
IMAGE geocentric inertial (GCI) position (X-component)
Spacecraft Position at Snapshot Time - REM - incorrectly structured, should not
be dimension 360? - should be one  1-d variable of size 3 for three components
IMAGE geocentric inertial (GCI)position (Y-component)
Spacecraft Position at Snapshot Time
geocentric position
Spacecraft Position at Snapshot Time
azimuth angle
(Phi) flight software uses 315, analysis uses 45
co-elevation angle
(Theta)
roll angle
(Omega)


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IM_K0_HENA
No TEXT global attribute.


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IM_L1_LEN
Description
The logical_file_id stores the name of the CDF file using the ISTP naming convention (source_name /
data_type / descriptor / date / data_version).im_l1_len_00000000_v01


Variable Notes

Image Time
The time in EPOCH refers to the center of IMAGE.
Spacecraft Position in SM, 3 comp.
SM = solar magnetic coordinates
Spacecraft Position in Geo, 3 comp.
Geo = geographic coordinates
Spacecraft Position in GSM, 3 comp.
GSM = gencentric solar magnetospheric coordinates
Spin_Phase
The time during the image at which the camera is pointed toward the center of
the earth.  This time is relative to Epoch.
The start of the image, measured from EPOCH.
The beginning time of the image is specified in msec relative to the time in
EPOCH by IMG_MINUS_MSEC.
The end of the image, measured from EPOCH.
The ending time of the image is specified in msec relative to the time in EPOCH
by IMG_PLUS_MSEC.


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IM_K0_LENA
No TEXT global attribute.


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IM_K0_MENA
No TEXT global attribute.


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IM_K0_RPI
Description
TBD


Modification History
Master with plasmagram vv's re-integrated with data CDFs 12/6/00 REM; 
SKTEditor review and corrections applied to master 12/6/00 REM;


Variable Notes

Plasmagram Time
The time in EPOCH refers to the beginning of the plasmagram. Use Duration_ms to
obtain stop time of the run.
Program Specifications
TBD
Offset from Epoch time to the end of the measurement run.
Time in ms between start and stop of the measurement run.
Nadir crossing MET is the reference MET that uniquely identifies all RPI measurements.
MET of the last Nadir crossing before  the measurement starts.
Measurement start MET.
Start MET is derived using the Nadir crossing MET and the time offset from the
first packet header. Might not be unique due to telemetry losses.
Operating Mode Name
values: Calibration, Sounding, Thermal Noise, Relaxation, Whistler, Test
Pattern; time-varying character data
Number of Dopplers
TBD
Pulse Repetition Rate
0.5 pps (1 pulse every 2 sec), 1 pps, 2 pps, 4 pps, 10 pps, 20 pps, 50 pps.
Xmtr Antenna Setting Name
values (numbers sequence only):  1= Radio Silence (no Tx), 2= X antenna only, 3=
Y antenna only, 4= X+Y Linearly polarized, 5= X+Y Right Circularly Polarized, 6=
X+Y Left Circularly Polarized, 7= X+Y Right/Left Alternated, 8= X+Y Lin/Lin90
Alternated.; time-varying character data
Coupler Mode Name
values (numbers sequence only):  0= OFF (untuned), 1= ON (tuned)
Waveform Operating Mode Name
values (numbers sequence only):  1= 16-chip complementary, 2= FM Chirp, 3=
Staggered Pulse Sequence, 4= Long Pulse, 5= Short Pulse, 6= 0.5 s Pulse7= 1.95 s
Pulse, 8= 8-chip complementary9= 4-chip complementary.
Base Gain
TBD
Gain Control Name
0= Fixed Gain, 1= Auto Gain.
Search of quiet frequencies enabled
0= Search of quiet frequencies disabled, 1= Search of quiet frequencies enabled.
Peak Power Constraint
Total RPI Peak Power Consumption Constraint.
Actual number of frequencies being measured
Detailed plasmagram picture has the original number of frequencies as specified
by RPI measurement parameters. Frequency axis varies from plasmagram to
plasmagram. Plasmagram *thumbnails* have a fixed frequency axis. The original
plasmagram data often requires transformation into thumbnail format by
averaging.
Measured frequency values
TBD
Measured frequency values
TBD
Actual mumber of ranges being measured
Number of Ranges, depending on program setting and processing.
Measured range values
Range readings
Echo Amplitude images (x=range, y=frequency, no scales)
TBD
---> Echo Amplitude image movie (x=range, y=frequency, no scales)
TBD
Echo Amplitude images (x=frequency, y=range, no scales)
TBD
---> Echo Amplitude image movie (x=frequency, y=range, no scales)
TBD
Echo Amplitude Image [nV] - Plasmagram - linear (range vs frequency)
TBD
---> Echo Amplitude Image [nV] - Plasmagram movie - linear (range vs. frequency)
TBD
Echo Amplitude Image [nV] - Plasmagram - linear (frequency vs. range)
TBD
---> Echo Amplitude Image [nV] - Plasmagram movie - linear (frequency vs. range)
TBD
Echo Amplitude Image [nV] - Plasmagram - log (range vs. frequency)
TBD
---> Echo Amplitude Image [nV] - Plasmagram movie - log (range vs. frequency)
TBD
Echo Amplitude Image [nV] - Plasmagram - log (frequency vs. range)
TBD
---> Echo Amplitude Image [nV] - Plasmagram movie - log (frequency vs. range)
TBD
Most Probable Amplitude
Most probable amplitude
Echo Azimuth angle images (x=range, y=frequency, no scales)
Values 0 to 254 cover 0 to 360 degrees
Echo Doppler Number image (x=range, y=frequency, no scales)
TBD
Doppler Number to frequency translation
Translates Doppler Number to an actual Doppler Frequency. The entries are 
calculated from program parameters.


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IM_K0_SIE
Description
electrons



SKT version 24-July-2000 
Mende et al: Far Ultraviolet Imaging from the IMAGE Spacecraft,Space Sciences Review 1999


Variable Notes

oriention direction cosine
direction of true spin axis at WIC Snapshot Time
oriention direction cosine
direction of true spin axis at WIC Snapshot Time
oriention direction cosine
direction of true spin axis at WIC Snapshot Time
geocentric position - GCI X
Spacecraft Position at Snapshot Time
geocentric position GCI Y
Spacecraft Position at Snapshot Time
geocentric position GCI Z
Spacecraft Position at Snapshot Time
angle
(Phi) flight software uses 315, analysis uses 45
angle
(Theta)
angle
(Omega)


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IM_K0_SIP
Description
Protons



SKT version 24-July-2000
Mende et al: Far Ultraviolet Imaging from the IMAGE Spacecraft,Space Sciences Review 1999


Variable Notes

oriention direction cosine
direction of true spin axis at WIC Snapshot Time
oriention direction cosine
direction of true spin axis at WIC Snapshot Time
oriention direction cosine
direction of true spin axis at WIC Snapshot Time
geocentric position GCI X
Spacecraft Position at Snapshot Time
geocentric position GCI Y
Spacecraft Position at Snapshot Time
geocentric position GCI Z
Spacecraft Position at Snapshot Time
angle
(Phi) flight software uses 315, analysis uses 45
angle
(Theta)
angle
(Omega)


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IM_K0_WIC
Description
 



SKT version 15-December-1999 
Mende et al: Far Ultraviolet Imaging from the IMAGE Spacecraft,Space Sciences Review 1999


Variable Notes

FUV/WIC LBH Auroral Images (raw cnts/14 bits, no grid, small format, linear scale)
REM - reset validmin to 250 on 11/29/00; LBH=Lyman-Birge-Hopfield
---> FUV/WIC LBH Auroral Images, as above (large format)
REM - reset validmin to 250 on 11/29/00
FUV/WIC LBH Auroral Mapped Images (raw cnts/14 bits, large format, linear scale)
REM - reset validmin to 250 on 11/29/00; LBH=Lyman-Birge-Hopfield
---> FUV/WIC LBH Auroral Mapped images, as above (movie format)
REM - reset validmin to 250 on 11/29/00
orientation direction cosine X (direction of true spin axis at WIC Snapshot Time)
direction of true spin axis at WIC Snapshot Time
oriention direction cosine Y (direction of true spin axis at WIC Snapshot Time)
direction of true spin axis at WIC Snapshot Time
oriention direction cosine Z
direction of true spin axis at WIC Snapshot Time
IMAGE GCI position X
Spacecraft Position at Snapshot Time
IMAGE GCI position Y
Spacecraft Position at Snapshot Time
IMAGE GCI position Z
Spacecraft Position at Snapshot Time
WIC azimuthal offset
(Phi) flight software uses 315, analysis uses 45
WIC vertical angular offset
(Theta)
WIC third Euler angle
(Omega)


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IM_K1_RPI
Description
TBD


Variable Notes

Measurement Time
The time in EPOCH refers to the beginning of the thermal noise measurement. Use
Duration_ms to obtain stop time of the run.
Program Specifications
TBD
Measurement duration, offset from Epoch time to the end of the measurement run.
Time in ms between start and stop of the measurement run.
Nadir crossing MET is the reference MET that uniquely identifies all RPI measurements.
MET of the last Nadir crossing before  the measurement starts.
Measurement start MET.
Start MET is derived using the Nadir crossing MET and the time offset from the
first packet header. Might not be unique due to telemetry losses.
Number of repetitions
2**N, where N is RPI control parameter
Base Gain
valid codes 1-16
Freq Search
values (numbers for sequence only): 0= Fixed Gain, 1= Auto Gain.
Number of frequencies measured
Detailed plasmagram picture has the original number of frequencies as specified
by RPI measurement parameters. Frequency axis varies from plasmagram to
plasmagram. Plasmagram *thumbnails* have a fixed frequency axis. The original
plasmagram data often requires transformation into thumbnail format by
averaging.
Frequency
TBD
Thermal Noise Amplitude, Antenna X
TBD
Thermal Noise Amplitude, Antenna Y
TBD
Thermal Noise Amplitude, Antenna Z
TBD
Thermal Noise Amplitude, antennas XY summary
TBD


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IM_K2_RPI
Description
The logical_file_id stores the name of the CDF file using the ISTP naming convention (source_name /
data_type / descriptor / date / data_version).im_k2_rpi_00000000_v01


Modification History
Master with plasmagram vv's re-integrated with data CDFs 12/6/00 REM; 
SKTEditor review and corrections applied to master 12/6/00 REM;
New version to match newly formatted data files also corrected Amplitude2 display_type - vars are
case sensitive. TJK 11/22/2002


Variable Notes

Plasmagram Time
The time in EPOCH refers to the beginning of the plasmagram. Use Duration_ms to
obtain stop time of the run.
ProgramSpecs
TBD
Offset from Epoch time to the end of the measurement run.
Time in ms between start and stop of the measurement run.
Nadir crossing MET is the reference MET that uniquely identifies all RPI measurements.
MET of the last Nadir crossing before  the measurement starts.
Measurement start MET.
Start MET is derived using the Nadir crossing MET and the time offset from the
first packet header. Might not be unique due to telemetry losses.
Operating Mode Name
values: Calibration, Sounding, Thermal Noise, Relaxation, Whistler, Test
Pattern; time-varying character data
NumDopplers
TBD
RepetitionRate
0.5 pps (1 pulse every 2 sec), 1 pps, 2 pps, 4 pps, 10 pps, 20 pps, 50 pps.
Xmtr Antenna Setting Name
values (numbers sequence only):  1= Radio Silence (no Tx), 2= X antenna only, 3=
Y antenna only, 4= X+Y Linearly polarized, 5= X+Y Right Circularly Polarized, 6=
X+Y Left Circularly Polarized, 7= X+Y Right/Left Alternated, 8= X+Y Lin/Lin90
Alternated.; time-varying character data
Coupler Mode Name
values (numbers sequence only):  0= OFF (untuned), 1= ON (tuned)
Waveform Operating Mode Name
values (numbers sequence only):  1= 16-chip complementary, 2= FM Chirp, 3=
Staggered Pulse Sequence, 4= Long Pulse, 5= Short Pulse, 6= 0.5 s Pulse7= 1.95 s
Pulse, 8= 8-chip complementary9= 4-chip complementary.
Base Gain
TBD
Gain Control Name
0= Fixed Gain, 1= Auto Gain.
Search of quiet frequencies enabled
0= Search of quiet frequencies disabled, 1= Search of quiet frequencies enabled.
Peak Power Constraint
Total RPI Peak Power Consumption Constraint.
Actual Number of Times
Actual number of times the measurements were made.
Actual number of frequencies being measured
Detailed plasmagram picture has the original number of frequencies as specified
by RPI measurement parameters. Frequency axis varies from plasmagram to
plasmagram. Plasmagram *thumbnails* have a fixed frequency axis. The original
plasmagram data often requires transformation into thumbnail format by
averaging.
Frequency
Sounding frequency in kHz
Actual sounding times measured
Time since the measurement start in seconds
Actual number of ranges being measured
Number of Ranges, depending on program setting and processing.
Measured range values
Range readings
Echo Amplitude Images [nV] (x=Time, y=Range, no scales)
TBD
[DO NOT USE - UNDER DEVELOPMENT] Echo Amplitude Images [nV] - Plasmagram (x=Time, y=Range, no scales)
TBD
[DO NOT USE - UNDER DEVELOPMENT] Echo Amplitude Images [nV] - Plasmagram Movie (x=Time, y=Range, no scales)
TBD
MPA
Most probable amplitude
Echo Azimuth angle
Values 0 to 254 cover 0 to 360 degrees
Echo Doppler Number
TBD
DopplerTranslation
Translates Doppler Number to an actual Doppler Frequency. The entries are 
calculated from program parameters.


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IM_OR_DEF
Description
tbs


Modification History
tbs




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IM_OR_PRE
Description
tbs


Modification History
tbs




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IR_C9_IR00
Description
Derived from IR00 dataset in CDAW9
Data for all CDAW9 events A-E


Modification History
Converted to CDAWeb Feb 2000




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IR_C9_IR04
Description
Derived from IR04 in CDAW9 DB.
Data for CDAW9 event B only.


Modification History
Converted to CDAWeb Feb 2000.




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IR_C9_IR23
Description
Derived from IR23 in CDAW9 DB.
Data for CDAW9 event B only.
Times are for midpoint of 30-s averages.  Angles are in GSE coords.             
AMPTE/IRM 30-s averages of plasma data (for protons) and magnetic field data are available only for
the interval 0:30 - 2:30 on 860403.  Angles are expressed in the GSE system.  The UT times are for
the midpoints of each interval.


Modification History
Converted to CDAWeb Feb 2000




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IR_C9_IRMD
Description
 Derived from IRMD in CDAW9 DB.
Data for all CDAW9 events A-E.


Modification History
 Converted to CDAWeb Feb 2000




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ISEE1_H0_FE
Description
This enhanced CDF master was generated by NSSDC, with input from R. Fitzenreiter, to make useable a
bare-bones CDF data set provided earlier to NSSDC. This current CDF master version, Nov. 4, 2002, is
used for making a CDF by selecting only certain variables from those available in the original
bare-bones CDF.


Variable Notes

Harvey Experiment Status (0 = Off)
Active Harvey experiment causes spikes in electron data.
Mozer Experiment Status (0 = Off)
Active Mozer experiment cause spikes in elecgtron data.
Electron distribution function: 6 values taken during one spin. 
Electron density is obtained 6 times during a spacecraft spin period. The six
measurements are separately averaged to make the six elements of this array. We
still need to know the delta t from Epoch to the first of these 6 densities.
Electron Density
Electron Density
Electron Temperature = 1/3 trace of the diagonalized pressure tensor.
Electron Temperatue is 1/3 trace of diagonalized pressure tensor. Electron
Temperature = (1/3) (parallel temp + two perpendicular eigenvalues)


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IT_H0_MFI
Description
               Magnetic field measurements on the  Interball- Tail  satellites are carried out by
IZMIRAN and Space Research Institute RAS  (SRI)   
       since 1995.  Satellite has  the orbits  with  apogee 200000 (30 Re)  and perigee 500 km. and
provides measurements in the solar wind and in the different
       regions of the magnetosphere at the same time with Geotail, Polar and Interbal-A working in
the magnetosphere and  Wind, ACE in the solar wind. 
        Magnetic field measurements on-board the Interball  Tail Probe are carried out by the FM-3I
and MFI instruments. FM-3I consists of two flux-gate
       magnetometers M1 and  M2  covering two  different  ranges:  200  nT  and  1000  nT.  The   M2
instrument is mostly  used to perform the  attitude 
       control of  the INTERBALL TAIL spacecraft.   M1 magnetometer data are transmitted to the
scientific SSNI  telemetry  system at rates  0.125-16 vectors/s
       depending on the instrument  operating mode. The magnetic field data from the M2 magnetometer
are transmitted at the  rate 1 vectors per 6 sec. to  the
       BNS attitude  control  system.  MFI magnetometer has the next parameters: measured range
0.3-37.5 nT, frequency range 0-2  Hz, sampling rate  from 1/4
       to 8 measurements per second. FM-3 M2 magnetometer failed in February 1996, FM-3 M1 and MFI
are working until now. 
                  Data presented here are the  combination of the data of all magnetometers. First
of all   FM-3 M1 data are used,  if they are absent, used MFI data
       and if data of both magnetometer are absent, FM-3 M2 data presented. In case of FM-3 M1 and
MFI, data are averaged for 6 seconds intervals.


Modification History
created CDF August 2000 by Mona Kessel, data provided by
Dr. Valery G. Petrov ZMIRAN, 
       Troitsk, Moscow region, 
       142092, Russia 
http://antares.izmiran.rssi.ru/projects/PROGNOZ-MF/




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IT_H0_SCA1
Description
Vaisber et al., Complex Plasma Spectrometer SKA-1, in Interball Mission and Payload, IKI-RSA-CNES,
P. 170, 1995.


Modification History
created Nov 1997




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IT_H0_SCA1
Description
Vaisber et al., Complex Plasma Spectrometer SKA-1, in Interball Mission and Payload, IKI-RSA-CNES,
P. 170, 1995.


Modification History
created Nov 1997


Variable Notes

8 azimuthal angles (0-360)deg
angle acceptance is 45 degrees in azimuth


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IT_K0_AKR
Description
Radioemission flux measured in 100, 252, 500 kHz ranges, the passband 10 kHz. Loop antenna with 1.5
m2 area is used.
Full description: http://www.iki.rssi.ru/interball.html


Modification History
created May 1996


Variable Notes

Radioemission flux at 3 freq (100, 252, 500 kHz)
2 min average of spectral amplitudes  in three ranges, AKR-X instrument
3 Frequencies for AKR spectrum
middle frequencies given, passbands are 10 kHz


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IT_K0_COR
No TEXT global attribute. 
Ion moments measured measured in the 25 eV - 25 keV range. Solar and antisolar directions not
covered.
Full description: http://www.iki.rssi.ru/interball.html


Modification History
created July 1996


Variable Notes

Ion Number Density, CORALL
2 min. resolution
Ion temperature, CORALL
2 min. resolution
Ion velocity, GSE cartesian vector, CORALL
2 min resolution
Ion velocity, GSM cartesian vector, CORALL
2 min resolution
Status flag, quality coded, see description
Standard flags are used in case of data absence. For the valid data SF is in the
range 10-12. 10 - good quality data. 11 - data in the spacecraft frame
preliminary data.


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IT_K0_ELE
No TEXT global attribute. 
Density and mean energy integrated from spectrum, measured by one plate and averaged over a spin
period 
Ne and Te - integration over full energy range, Ne1, Te1 - integration, excluding lowest energies
with dominating photoelectrons (up to 20-40 eV, see description)
Top Hat Electrostatic Analyser
Full description: http://www.iki.rssi.ru/interball.html


Modification History
created Mar 1996


Variable Notes

Electron Number Density, full energy range
2 min. resolution
Electron mean energy, full energy range
2 min. resolution
Electron Density, lowest energies cut off
2 min. resolution
Electron mean energy, lowest energies cut off
2 min. resolution
Status flag, mode coded, see description
Standard flags are used in case of data absence. For the valid data SF is in the
range 10-38. Most significant digit (1-3) shows energy range used. Least
significant digit shows number of the plate, data from which are used.


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IT_K0_EPI
No TEXT global attribute. 
Energetic particle fluxes in three energy ranges from several sensors. Data are averaged in 2 min.
intervals Status flags show instrument mode.
Full description: http://www.iki.rssi.ru/interball.html


Modification History
created Mar 1996


Variable Notes

Electron Flux, 21-26 keV (DOK-2 first electron sensor, fixed)
sensor offset at an angle 180 deg with respect to the sunward directed
spacecraft spin axis
Electron Flux, 76-95 keV (DOK-2 first electron sensor, fixed)
sensor offset at an angle 180 deg with respect to the sunward directed
spacecraft spin axis
Proton Flux, 22-28 keV (DOK-2 first proton sensor, fixed)
sensor offset at an angle 180 deg with respect to the sunward directed
spacecraft spin axis
Proton Flux, 21-27 keV (DOK-2 second proton sensor, scan)
The value is taken from the sensor that can scan the angle's interval 45-180 deg
or can be fixed at angles 45, 90, 135, 180 deg. with respect to the sunward
directed spacecraft spin axis
Electron Flux, 150-500 keV (SKA-2 electron sensor)
Electron and proton sensors of EV-3 subsystem are offset at an angle 135 deg
with respect to the sunward directed spacecraft spin axis
Proton Flux, 1-3 MeV (SKA-2 proton sensor)
Electron and proton sensors of EV-3 subsystem are offset at an angle 135 deg
with respect to the sunward directed spacecraft spin axis
Status Flag: energy and position coded, see description
Standard flags are used in the case of data absence. SFs are set to 11-15 and
21-25 for all valid data values of each parameter. Most significant digit (1 -
low or 2 - high) indicates level of the energy threshold. Higher energy
threshold will be used only in case of degradation of a sensor. Less significant
digit indicates sensor orientation ( 1, 2, 3, 4, 5 correspond respectively to
45, 90, 135, 180 deg. and scan)
Status Flag: energy and position coded, see description
Standard flags are used in the case of data absence. SFs are set to 11-15 and
21-25 for all valid data values of each parameter. Most significant digit (1 -
low or 2 - high) indicates level of the energy threshold. Higher energy
threshold will be used only in case of degradation of a sensor. Less significant
digit indicates sensor orientation ( 1, 2, 3, 4, 5 correspond respectively to
45, 90, 135, 180 deg. and scan)
Status Flag: energy and position coded, see description
Standard flags are used in the case of data absence. SFs are set to 11-15 and
21-25 for all valid data values of each parameter. Most significant digit (1 -
low or 2 - high) indicates level of the energy threshold. Higher energy
threshold will be used only in case of degradation of a sensor. Less significant
digit indicates sensor orientation ( 1, 2, 3, 4, 5 correspond respectively to
45, 90, 135, 180 deg. and scan)
Status Flag: energy and position coded, see description
Standard flags are used in the case of data absence. SFs are set to 11-15 and
21-25 for all valid data values of each parameter. Most significant digit (1 -
low or 2 - high) indicates level of the energy threshold. Higher energy
threshold will be used only in case of degradation of a sensor. Less significant
digit indicates sensor orientation ( 1, 2, 3, 4, 5 correspond respectively to
45, 90, 135, 180 deg. and scan)
Status Flag: standard values, see description
Standard flags are used in the case of data absence. SFs are set to 11-15 and
21-25 for all valid data values of each parameter. Most significant digit (1 -
low or 2 - high) indicates level of the energy threshold. Higher energy
threshold will be used only in case of degradation of a sensor. Less significant
digit indicates sensor orientation ( 1, 2, 3, 4, 5 correspond respectively to
45, 90, 135, 180 deg. and scan)


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IT_K0_ICD
Description
Count rate of H+, O+ ions in 2 min, three directions, (1-30 keV) Status flag shows instrument mode.
Data description:  http://www.iki.rssi.ru/interball.html


Modification History
created Feb 1996




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IT_K0_MFI
No TEXT global attribute. 
Magnetic field vector is averaged from 4 Hz or 1 Hz data.  Fill values are used instead of Y, Z
components if attitude data are absent 
Spectral amplitudes in ranges 1-4 Hz and 600-850 Hz are measured with the use of filter bank by
fluxgate and search-coil sensors
Full description: http://www.iki.rssi.ru/interball.html


Modification History
created Feb 1996


Variable Notes

Magnetic Field, 3 coord cartesian GSE
2 min. average, ASPI MIF-M/PRAM magnetometer
Magnetic Field, 3 coord cartesian GSM
2 min. average, ASPI MIF-M/PRAM magnetometer
Magnetic Field absolute value, scalar
2 min. average, ASPI MIF-M/PRAM magnetometer
Magnetic Field Fluctuations at 2 freq (2 and 725 Hz)
2 min average of spectral amplitudes  in two ranges, ASPI MIF-M/PRAM
magnetometer
Status of PRAM experiment
Standard values used, see description
PRAM mode coded
Flag values: 10 - data OK, 11 - mode with no amplitude values available
2 Frequencies for B spectrum (1-4, 600-850 Hz)
middle frequencies given, real ranges are 1-4, 600-850 Hz


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IT_K0_VDP
No TEXT global attribute. 
Total antisunward ion flux, measured by the Sun-oriented Faraday cup with the grid potential -170 V
In the solar wind and flank magnetosheath full ion flux is measured. In the front-side magnetosheath
up to 30% of flux is out of instrument's field of view. 
All measurements with negative currents (high energy electron contamination inside the
magnetosphere) are excluded
Full description: http://www.iki.rssi.ru/interball.html


Modification History
created Feb 1997


Variable Notes

Total antisunward ion flux
2 min. resolution


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IT_K0_WAV
Description
Magnetic field averages and variance are computed from 4 Hz or 1 Hz data 
Mf1 magnetic field AC amplitudes are measured by fluxgate sensor.
Mf2 magnetic field AC amplitudes are measured by search-coil.
Mf3 plasma wave AC amplitudesare measured by Langmuir splitprobe.
Full description: http://www.iki.rssi.ru/interball.html


Modification History
created Jan 1998


Variable Notes

Magnetic Field Fluctuations at 2 freq.
2 min average of spectral amplitudes  in two ranges, ASPI MIF-M/PRAM fluxgate
Magnetic Field Fluctuations at 5 freq.
2 min average of spectral amplitudes  in five ranges, ASPI MIF-M/PRAM
search-coil
Electric Current Fluctuations at 5 freq.
2 min average of spectral amplitudes  in five ranges, ASPI MIF-M/PRAM split
Langmuir probe
PRAM mode coded
Flag values: 10 -  magnetic field data in MF2, 11 - plasma current datain MF3, 2
- no filter data.
Frequencies for spectrum 1-40 Hz
middle frequencies given, real ranges are in label_Mf
Frequencies for spectrum 1-2000 Hz
middle frequencies given, real ranges are in label_Mf
Magnetic Field average of magnitudes, scalar
2 min. average, ASPI MIF-M/PRAM magnetometer
Magnetic Field variance of magnitudes, scalar
2 min. average, ASPI MIF-M/PRAM magnetometer
Magnetic Field GSE Bx, scalar
2 min. average, ASPI MIF-M/PRAM magnetometer
Magnetic Field variance of GSE Bx (spin axis), scalar
2 min. average, ASPI MIF-M/PRAM magnetometer


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IT_OR_DEF
No TEXT global attribute. 
Full description: http://www.iki.rssi.ru/interball.html


Modification History
created Mar 1996




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L0_H0_MPA
No TEXT global attribute.


Modification History
Created OCT 1998




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L0_K0_MPA
Description
This file contains numerical moments computed from measurements of the 
Los Alamos Magnetospheric Plasma Analyzer (MPA) [Bame et al., 
Rev. Sci. Inst., in press 1993]. 
The moments are presented in s/c coordinates: the z-axis is aligned with 
the spin axis, which points radially toward the center of the Earth; 
the x-axis is in the plane containing the spacecraft spin axis and the spin 
axis of the Earth, with +X generally northward; and the y-axis points 
generally eastward. Polar angles are measured relative to the spin axis 
(+Z), and azimuthal angles are measured around the z-axis, with zero along 
the +X direction. The moments are computed for three 'species': 
lop (low-ener. ions, ~1eV/e-~130eV/e); hip (hi-ener. ions, ~130eV/e-~45keV/e);
 alle (electrons, ~30eV - ~45keV ). The electron measurements are obtained 
21.5 secs after the ion measurements. Epoch is the measurement time 
appropriate for the ions. The moments are computed after the fluxes are 
corrected for background and s/c potential. Algorithms for these corrections
 are relatively unsophisticated, so the moments are suspect during times of 
high background and/or high spacecraft potential. Because the determined  
spacecraft potential is not very precise, the magnitude of the low-energy 
ion flow velocity is probably not accurate, but the flow direction is well 
determined.  Tperp and Tpara are obtained from diagonalization of the  
3-dimensional temperature matrix, with the parallel direction assigned 
to the eigenvalue which is most different from the other two. 
The corresponding eigenvector is the symmetry axis of the distribution and 
should be equivalent to the magnetic field direction. The eigenvalue ratio 
Tperp/Tmid, which is provided for each species, is a measure of the symmetry 
of the distribution and should be ~1.0 for a good determination. Several of  
the parameters have a fairly high daily dynamic range and for survey purposes 
are best displayed logarithmically. These parameters are indicated by  
non-zero 'SCALEMIN' values in this file. A quality flag value of 1  
indicates that the values are  preliminary and have not been checked 
in detail.


Modification History
Created SEP 1992 Modified JAN 1993 
Electron time tags removed Mag Latitude added 
Local time added Post Gap flag added 
Ratio variables changed Modified SEP 1994 
Changes noted in mail message from M.Kessel


Variable Notes

[Computed 3-min vector] S/C position, GCI coordinates (X, Y, Z)
This is a virtual variable generated by read_myCDF w/ useof the data in the
sc_pos_geo variable and a conversion routinespecified in the function attribute,
namely conv_pos
[Computed 3-min vector] S/C position, GEO coordinates (Radius, Lat, Lon)
This is a virtual variable generated by read_myCDF w/ useof the data in the
sc_pos_geo variable and a conversion routinespecified in the function attribute,
namely conv_pos


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L0_K0_SPA
Description
     Electron, proton and helium measurements are taken every 160 ms from one 
of the three telescopes according to the following sequence:  T1, T2, T3, 
T2, T1, T2 etc.  Heavy ion data accumulated from each of the three telescopes 
again according to the timing and sequence above and summed for 10.24 seconds
which is approximately one spacecraft rotation.  SOPA Key Parameters are 
normally averaged over three telescopes for ~ 1 minute (6 - 10.24 second
data accumulation cycles) giving an average over much of the sky.  The time 
associated with each set of Key Parameters is determined by using the time 
(in minutes of the day) at the start of each data collection cycle as an index
into an array of 1440 time slots dividing the day into 1440 one minute 
intervals.  The time reported is the midpoint of each interval.  
     We provide six fluxes:
        Low energy Protons:  50 keV to 400 keV
        High energy Protons: 1.2 MeV to 5 MeV
        Low energy Electrons:  50 keV to 225 keV
        High energy Electrons: 315 keV to 1.5 MeV
        Helium      : ~0.9 MeV to ~1.3 Mev
        Heavy Ions  : ~5 MeV to ~15 MeV (includes carbon, nitrogen,
                       and oxygen
     We also compute two electron temperatures and densities and two proton
temperatures and densities.  These are based on approximately the same energy
ranges as the fluxes given in above and are determined for relativistic
Maxwellian distributions.  
 
Status of SOPA Instrument 1990-095:  Loss of all ion data as of July 1992
All three thin, front, D1 detectors have failed, having become intolerably
noisy.  The net result of this failure is the complete loss of proton, 
helium, carbon, nitrogen, oxygen and other high Z Key Parameter data from
the instrument.  Since all three thick, back D2 detectors are still 
operating normally, the electron measurements remain only insignificantly 
affected.
   
   
Data is flagged with a data quality flag as follows:
   +1 Data is Good
    0 Data is Suspect
   -1 Data is Unusable
References:   Belian, R. D., Gisler, G. R., Cayton, T. E., Christensen, R. A.,
High-Z Energetic Particles at Geosynchronous Orbit During The Great Solar 
Proton Event Series of October 1989, J. Geophys. Res., 97, 16897, 1992


Modification History
created 30-Nov-1992 
added text to describe instrument 04-Feb-1993


Variable Notes

Electron temperature in 2 energy bands (50-225 keV, 315-1500 keV)
Electron temperature determined from relativistic Maxwellian distributions and
averaged over 3 11deg telescopes (separated by  30deg) rotating with spacecraft
Protron temperature in 2 energy bands (50-400 keV, 1.2-5.0 MeV)
Protron temperature determined from relativistic Maxwellian distributions and
averaged over 3 11deg telescopes (separated by  30deg) rotating with spacecraft
Partial electron densities in 2 energy bands (50-225 keV, 315-1500 keV)
Partial electron densities determined from relativistic Maxwellian distributions
and averaged over 3 11deg telescopes (separated by  30deg) rotating with
spacecraft
Partial protron densities in 2 energy bands (50-400 keV, 1.2-5.0 MeV)
Partial protron densities determined from relativistic Maxwellian distributions
and averaged over 3 11deg telescopes (separated by  30deg) rotating with
spacecraft
alpha flux (Helium) from ~0.9 MeV to ~1.3 Mev
alpha flux (Helium) averaged over 3 11deg telescopes (separated by  30deg)
rotating with spacecraft
Heavy Ion flux at ~5 MeV to ~15 MeV (includes carbon, nitrogen, and oxygen
Heavy Ion flux averaged over 3 11deg telescopes (separated by  30deg) rotating
with spacecraft
Electron flux in 2 energy bands (50-225 keV, 315-1500 keV)
Electron flux is averaged over 3 11deg telescopes (separated by  30deg) rotating
with spacecraft
protron flux in 2 energy bands (50-400 keV, 1.2-5.0 MeV)
protron flux averaged over 3 11deg telescopes (separated by  30deg) rotating
with spacecraft


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L1_H0_MPA
No TEXT global attribute.


Modification History
Created OCT 1998




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L1_K0_MPA
Description
This file contains numerical moments computed from measurements of the 
Los Alamos Magnetospheric Plasma Analyzer (MPA) [Bame et al., 
Rev. Sci. Inst., in press 1993]. 
The moments are presented in s/c coordinates: the z-axis is aligned with 
the spin axis, which points radially toward the center of the Earth; 
the x-axis is in the plane containing the spacecraft spin axis and the spin 
axis of the Earth, with +X generally northward; and the y-axis points 
generally eastward. Polar angles are measured relative to the spin axis 
(+Z), and azimuthal angles are measured around the z-axis, with zero along 
the +X direction. The moments are computed for three 'species': 
lop (low-ener. ions, ~1eV/e-~130eV/e); hip (hi-ener. ions, ~130eV/e-~45keV/e);
 alle (electrons, ~30eV - ~45keV ). The electron measurements are obtained 
21.5 secs after the ion measurements. Epoch is the measurement time 
appropriate for the ions. The moments are computed after the fluxes are 
corrected for background and s/c potential. Algorithms for these corrections
 are relatively unsophisticated, so the moments are suspect during times of 
high background and/or high spacecraft potential. Because the determined  
spacecraft potential is not very precise, the magnitude of the low-energy 
ion flow velocity is probably not accurate, but the flow direction is well 
determined.  Tperp and Tpara are obtained from diagonalization of the  
3-dimensional temperature matrix, with the parallel direction assigned 
to the eigenvalue which is most different from the other two. 
The corresponding eigenvector is the symmetry axis of the distribution and 
should be equivalent to the magnetic field direction. The eigenvalue ratio 
Tperp/Tmid, which is provided for each species, is a measure of the symmetry 
of the distribution and should be ~1.0 for a good determination. Several of  
the parameters have a fairly high daily dynamic range and for survey purposes 
are best displayed logarithmically. These parameters are indicated by  
non-zero 'SCALEMIN' values in this file. A quality flag value of 1  
indicates that the values are  preliminary and have not been checked 
in detail.


Modification History
Created SEP 1992 Modified JAN 1993 
Electron time tags removed Mag Latitude added 
Local time added Post Gap flag added 
Ratio variables changed Modified SEP 1994 
Changes noted in mail message from M.Kessel


Variable Notes

[Computed 3-min vector] S/C position, GCI coordinates (X, Y, Z)
This is a virtual variable generated by read_myCDF w/ useof the data in the
sc_pos_geo variable and a conversion routinespecified in the function attribute,
namely conv_pos
[Computed 3-min vector] S/C position, GEO coordinates (Radius, Lat, Lon)
This is a virtual variable generated by read_myCDF w/ useof the data in the
sc_pos_geo variable and a conversion routinespecified in the function attribute,
namely conv_pos


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L1_K0_SPA
Description
     Electron, proton and helium measurements are taken every 160 ms from one 
of the three telescopes according to the following sequence:  T1, T2, T3, 
T2, T1, T2 etc.  Heavy ion data accumulated from each of the three telescopes 
again according to the timing and sequence above and summed for 10.24 seconds
which is approximately one spacecraft rotation.  SOPA Key Parameters are 
normally averaged over three telescopes for ~ 1 minute (6 - 10.24 second
data accumulation cycles) giving an average over much of the sky.  The time 
associated with each set of Key Parameters is determined by using the time 
(in minutes of the day) at the start of each data collection cycle as an index
into an array of 1440 time slots dividing the day into 1440 one minute 
intervals.  The time reported is the midpoint of each interval.  
     We provide six fluxes:
        Low energy Protons:  50 keV to 400 keV
        High energy Protons: 1.2 MeV to 5 MeV
        Low energy Electrons:  50 keV to 225 keV
        High energy Electrons: 315 keV to 1.5 MeV
        Helium      : ~0.9 MeV to ~1.3 Mev
        Heavy Ions  : ~5 MeV to ~15 MeV (includes carbon, nitrogen,
                       and oxygen
     We also compute two electron temperatures and densities and two proton
temperatures and densities.  These are based on approximately the same energy
ranges as the fluxes given in above and are determined for relativistic
Maxwellian distributions.  
 
Status of SOPA Instrument 1991-080:  Operating normally as of 01-Feb-1993
with the following exception.  Detector D1 on Telescope 2 is becoming noisy.
This affects proton and ion data from that telescope.  Bad data is disabled 
thru software in the ground processing and is NOT averaged into the Key 
parameter data.  Therefore, the parameters given are good but do not cover 
the same percentage of the sky.
   
Data is flagged with a data quality flag as follows:
   +1 Data is Good
    0 Data is Suspect
   -1 Data is Unusable
LANL personnel should be contacted before using any data tagged as suspect.
References:   Belian, R. D., Gisler, G. R., Cayton, T. E., Christensen, R. A.,
High-Z Energetic Particles at Geosynchronous Orbit During The Great Solar 
Proton Event Series of October 1989, J. Geophys. Res., 97, 16897, 1992


Modification History
created 30-Nov-1992 
added text to describe instrument 04-Feb-1993


Variable Notes

Electron temperature in 2 energy bands (50-225 keV, 315-1500 keV)
Electron temperature determined from relativistic Maxwellian distributions and
averaged over 3 11deg telescopes (separated by  30deg) rotating with spacecraft
Protron temperature in 2 energy bands (50-400 keV, 1.2-5.0 MeV)
Protron temperature determined from relativistic Maxwellian distributions and
averaged over 3 11deg telescopes (separated by  30deg) rotating with spacecraft
Partial electron densities in 2 energy bands (50-225 keV, 315-1500 keV)
Partial electron densities determined from relativistic Maxwellian distributions
and averaged over 3 11deg telescopes (separated by  30deg) rotating with
spacecraft
Partial protron densities in 2 energy bands (50-400 keV, 1.2-5.0 MeV)
Partial protron densities determined from relativistic Maxwellian distributions
and averaged over 3 11deg telescopes (separated by  30deg) rotating with
spacecraft
alpha flux (Helium) from ~0.9 MeV to ~1.3 Mev
alpha flux (Helium) averaged over 3 11deg telescopes (separated by  30deg)
rotating with spacecraft
Heavy Ion flux at ~5 MeV to ~15 MeV (includes carbon, nitrogen, and oxygen
Heavy Ion flux averaged over 3 11deg telescopes (separated by  30deg) rotating
with spacecraft
Electron flux in 2 energy bands (50-225 keV, 315-1500 keV)
Electron flux is averaged over 3 11deg telescopes (separated by  30deg) rotating
with spacecraft
protron flux in 2 energy bands (50-400 keV, 1.2-5.0 MeV)
protron flux averaged over 3 11deg telescopes (separated by  30deg) rotating
with spacecraft


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L4_H0_MPA
No TEXT global attribute.


Modification History
Created OCT 1998




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L4_K0_MPA
Description
This file contains numerical moments computed from measurements of the 
Los Alamos Magnetospheric Plasma Analyzer (MPA) [Bame et al., 
Rev. Sci. Inst., in press 1993]. 
The moments are presented in s/c coordinates: the z-axis is aligned with 
the spin axis, which points radially toward the center of the Earth; 
the x-axis is in the plane containing the spacecraft spin axis and the spin 
axis of the Earth, with +X generally northward; and the y-axis points 
generally eastward. Polar angles are measured relative to the spin axis 
(+Z), and azimuthal angles are measured around the z-axis, with zero along 
the +X direction. The moments are computed for three 'species': 
lop (low-ener. ions, ~1eV/e-~130eV/e); hip (hi-ener. ions, ~130eV/e-~45keV/e);
 alle (electrons, ~30eV - ~45keV ). The electron measurements are obtained 
21.5 secs after the ion measurements. Epoch is the measurement time 
appropriate for the ions. The moments are computed after the fluxes are 
corrected for background and s/c potential. Algorithms for these corrections
 are relatively unsophisticated, so the moments are suspect during times of 
high background and/or high spacecraft potential. Because the determined  
spacecraft potential is not very precise, the magnitude of the low-energy 
ion flow velocity is probably not accurate, but the flow direction is well 
determined.  Tperp and Tpara are obtained from diagonalization of the  
3-dimensional temperature matrix, with the parallel direction assigned 
to the eigenvalue which is most different from the other two. 
The corresponding eigenvector is the symmetry axis of the distribution and 
should be equivalent to the magnetic field direction. The eigenvalue ratio 
Tperp/Tmid, which is provided for each species, is a measure of the symmetry 
of the distribution and should be ~1.0 for a good determination. Several of  
the parameters have a fairly high daily dynamic range and for survey purposes 
are best displayed logarithmically. These parameters are indicated by  
non-zero 'SCALEMIN' values in this file. A quality flag value of 1  
indicates that the values are  preliminary and have not been checked 
in detail.


Modification History
Created SEP 1992 Modified JAN 1993 
Electron time tags removed Mag Latitude added 
Local time added Post Gap flag added 
Ratio variables changed Modified SEP 1994 
Changes noted in mail message from M.Kessel


Variable Notes

[Computed 3-min vector] S/C position, GCI coordinates (X, Y, Z)
This is a virtual variable generated by read_myCDF w/ useof the data in the
sc_pos_geo variable and a conversion routinespecified in the function attribute,
namely conv_pos
[Computed 3-min vector] S/C position, GEO coordinates (Radius, Lat, Lon)
This is a virtual variable generated by read_myCDF w/ useof the data in the
sc_pos_geo variable and a conversion routinespecified in the function attribute,
namely conv_pos


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L4_K0_SPA
Description
     Electron, proton and helium measurements are taken every 160 ms from one 
of the three telescopes according to the following sequence:  T1, T2, T3, 
T2, T1, T2 etc.  Heavy ion data accumulated from each of the three telescopes 
again according to the timing and sequence above and summed for 10.24 seconds
which is approximately one spacecraft rotation.  SOPA Key Parameters are 
normally averaged over three telescopes for ~ 1 minute (6 - 10.24 second
data accumulation cycles) giving an average over much of the sky.  The time 
associated with each set of Key Parameters is determined by using the time 
(in minutes of the day) at the start of each data collection cycle as an index
into an array of 1440 time slots dividing the day into 1440 one minute 
intervals.  The time reported is the midpoint of each interval.  
     We provide six fluxes:
        Low energy Protons:  50 keV to 400 keV
        High energy Protons: 1.2 MeV to 5 MeV
        Low energy Electrons:  50 keV to 225 keV
        High energy Electrons: 315 keV to 1.5 MeV
        Helium      : ~0.9 MeV to ~1.3 Mev
        Heavy Ions  : ~5 MeV to ~15 MeV (includes carbon, nitrogen,
                       and oxygen
     We also compute two electron temperatures and densities and two proton
temperatures and densities.  These are based on approximately the same energy
ranges as the fluxes given in above and are determined for relativistic
Maxwellian distributions.  
 
Status of SOPA Instrument 1994-084:  Operating normally as of 01-Jan-1996
   
Data is flagged with a data quality flag as follows:
   +1 Data is Good
    0 Data is Suspect
   -1 Data is Unusable
LANL personnel should be contacted before using any data tagged as suspect.
References:   Belian, R. D., Gisler, G. R., Cayton, T. E., Christensen, R. A.,
High-Z Energetic Particles at Geosynchronous Orbit During The Great Solar 
Proton Event Series of October 1989, J. Geophys. Res., 97, 16897, 1992


Modification History
created 30-Nov-1992 
added text to describe instrument 04-Feb-1993


Variable Notes

Electron temperature in 2 energy bands (50-225 keV, 315-1500 keV)
Electron temperature determined from relativistic Maxwellian distributions and
averaged over 3 11deg telescopes (separated by  30deg) rotating with spacecraft
Protron temperature in 2 energy bands (50-400 keV, 1.2-5.0 MeV)
Protron temperature determined from relativistic Maxwellian distributions and
averaged over 3 11deg telescopes (separated by  30deg) rotating with spacecraft
Partial electron densities in 2 energy bands (50-225 keV, 315-1500 keV)
Partial electron densities determined from relativistic Maxwellian distributions
and averaged over 3 11deg telescopes (separated by  30deg) rotating with
spacecraft
Partial protron densities in 2 energy bands (50-400 keV, 1.2-5.0 MeV)
Partial protron densities determined from relativistic Maxwellian distributions
and averaged over 3 11deg telescopes (separated by  30deg) rotating with
spacecraft
alpha flux (Helium) from ~0.9 MeV to ~1.3 Mev
alpha flux (Helium) averaged over 3 11deg telescopes (separated by  30deg)
rotating with spacecraft
Heavy Ion flux at ~5 MeV to ~15 MeV (includes carbon, nitrogen, and oxygen
Heavy Ion flux averaged over 3 11deg telescopes (separated by  30deg) rotating
with spacecraft
Electron flux in 2 energy bands (50-225 keV, 315-1500 keV)
Electron flux is averaged over 3 11deg telescopes (separated by  30deg) rotating
with spacecraft
protron flux in 2 energy bands (50-400 keV, 1.2-5.0 MeV)
protron flux averaged over 3 11deg telescopes (separated by  30deg) rotating
with spacecraft


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L7_H0_MPA
No TEXT global attribute.


Modification History
Created OCT 1998




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L7_K0_MPA
Description
This file contains numerical moments computed from measurements of the 
Los Alamos Magnetospheric Plasma Analyzer (MPA) [Bame et al., 
Rev. Sci. Inst., in press 1993]. 
The moments are presented in s/c coordinates: the z-axis is aligned with 
the spin axis, which points radially toward the center of the Earth; 
the x-axis is in the plane containing the spacecraft spin axis and the spin 
axis of the Earth, with +X generally northward; and the y-axis points 
generally eastward. Polar angles are measured relative to the spin axis 
(+Z), and azimuthal angles are measured around the z-axis, with zero along 
the +X direction. The moments are computed for three 'species': 
lop (low-ener. ions, ~1eV/e-~130eV/e); hip (hi-ener. ions, ~130eV/e-~45keV/e);
 alle (electrons, ~30eV - ~45keV ). The electron measurements are obtained 
21.5 secs after the ion measurements. Epoch is the measurement time 
appropriate for the ions. The moments are computed after the fluxes are 
corrected for background and s/c potential. Algorithms for these corrections
 are relatively unsophisticated, so the moments are suspect during times of 
high background and/or high spacecraft potential. Because the determined  
spacecraft potential is not very precise, the magnitude of the low-energy 
ion flow velocity is probably not accurate, but the flow direction is well 
determined.  Tperp and Tpara are obtained from diagonalization of the  
3-dimensional temperature matrix, with the parallel direction assigned 
to the eigenvalue which is most different from the other two. 
The corresponding eigenvector is the symmetry axis of the distribution and 
should be equivalent to the magnetic field direction. The eigenvalue ratio 
Tperp/Tmid, which is provided for each species, is a measure of the symmetry 
of the distribution and should be ~1.0 for a good determination. Several of  
the parameters have a fairly high daily dynamic range and for survey purposes 
are best displayed logarithmically. These parameters are indicated by  
non-zero 'SCALEMIN' values in this file. A quality flag value of 1  
indicates that the values are  preliminary and have not been checked 
in detail.


Modification History
Created SEP 1992 Modified JAN 1993 
Electron time tags removed Mag Latitude added 
Local time added Post Gap flag added 
Ratio variables changed Modified SEP 1994 
Changes noted in mail message from M.Kessel


Variable Notes

[Computed 3-min vector] S/C position, GCI coordinates (X, Y, Z)
This is a virtual variable generated by read_myCDF w/ useof the data in the
sc_pos_geo variable and a conversion routinespecified in the function attribute,
namely conv_pos
[Computed 3-min vector] S/C position, GEO coordinates (Radius, Lat, Lon)
This is a virtual variable generated by read_myCDF w/ useof the data in the
sc_pos_geo variable and a conversion routinespecified in the function attribute,
namely conv_pos


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L7_K0_SPA
Description
     Electron, proton and helium measurements are taken every 160 ms from one 
of the three telescopes according to the following sequence:  T1, T2, T3, 
T2, T1, T2 etc.  Heavy ion data accumulated from each of the three telescopes 
again according to the timing and sequence above and summed for 10.24 seconds
which is approximately one spacecraft rotation.  SOPA Key Parameters are 
normally averaged over three telescopes for ~ 1 minute (6 - 10.24 second
data accumulation cycles) giving an average over much of the sky.  The time 
associated with each set of Key Parameters is determined by using the time 
(in minutes of the day) at the start of each data collection cycle as an index
into an array of 1440 time slots dividing the day into 1440 one minute 
intervals.  The time reported is the midpoint of each interval.  
     We provide six fluxes:
        Low energy Protons:  50 keV to 400 keV
        High energy Protons: 1.2 MeV to 5 MeV
        Low energy Electrons:  50 keV to 225 keV
        High energy Electrons: 315 keV to 1.5 MeV
        Helium      : ~0.9 MeV to ~1.3 Mev
        Heavy Ions  : ~5 MeV to ~15 MeV (includes carbon, nitrogen,
                       and oxygen
     We also compute two electron temperatures and densities and two proton
temperatures and densities.  These are based on approximately the same energy
ranges as the fluxes given in above and are determined for relativistic
Maxwellian distributions.  
 
Status of SOPA Instrument LANL-97A:  Operating normally as of 01-Jul-1997
   
Data is flagged with a data quality flag as follows:
   +1 Data is Good
    0 Data is Suspect
   -1 Data is Unusable
LANL personnel should be contacted before using any data tagged as suspect.
References:   Belian, R. D., Gisler, G. R., Cayton, T. E., Christensen, R. A.,
High-Z Energetic Particles at Geosynchronous Orbit During The Great Solar 
Proton Event Series of October 1989, J. Geophys. Res., 97, 16897, 1992


Modification History
created 30-Nov-1992 
added text to describe instrument 04-Feb-1993


Variable Notes

Electron temperature in 2 energy bands (50-225 keV, 315-1500 keV)
Electron temperature determined from relativistic Maxwellian distributions and
averaged over 3 11deg telescopes (separated by  30deg) rotating with spacecraft
Protron temperature in 2 energy bands (50-400 keV, 1.2-5.0 MeV)
Protron temperature determined from relativistic Maxwellian distributions and
averaged over 3 11deg telescopes (separated by  30deg) rotating with spacecraft
Partial electron densities in 2 energy bands (50-225 keV, 315-1500 keV)
Partial electron densities determined from relativistic Maxwellian distributions
and averaged over 3 11deg telescopes (separated by  30deg) rotating with
spacecraft
Partial protron densities in 2 energy bands (50-400 keV, 1.2-5.0 MeV)
Partial protron densities determined from relativistic Maxwellian distributions
and averaged over 3 11deg telescopes (separated by  30deg) rotating with
spacecraft
alpha flux (Helium) from ~0.9 MeV to ~1.3 Mev
alpha flux (Helium) averaged over 3 11deg telescopes (separated by  30deg)
rotating with spacecraft
Heavy Ion flux at ~5 MeV to ~15 MeV (includes carbon, nitrogen, and oxygen
Heavy Ion flux averaged over 3 11deg telescopes (separated by  30deg) rotating
with spacecraft
Electron flux in 2 energy bands (50-225 keV, 315-1500 keV)
Electron flux is averaged over 3 11deg telescopes (separated by  30deg) rotating
with spacecraft
protron flux in 2 energy bands (50-400 keV, 1.2-5.0 MeV)
protron flux averaged over 3 11deg telescopes (separated by  30deg) rotating
with spacecraft


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L9_H0_MPA
No TEXT global attribute.


Modification History
Created OCT 1998




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L9_K0_MPA
Description
This file contains numerical moments computed from measurements of the 
Los Alamos Magnetospheric Plasma Analyzer (MPA) [Bame et al., 
Rev. Sci. Inst., in press 1993]. 
The moments are presented in s/c coordinates: the z-axis is aligned with 
the spin axis, which points radially toward the center of the Earth; 
the x-axis is in the plane containing the spacecraft spin axis and the spin 
axis of the Earth, with +X generally northward; and the y-axis points 
generally eastward. Polar angles are measured relative to the spin axis 
(+Z), and azimuthal angles are measured around the z-axis, with zero along 
the +X direction. The moments are computed for three 'species': 
lop (low-ener. ions, ~1eV/e-~130eV/e); hip (hi-ener. ions, ~130eV/e-~45keV/e);
 alle (electrons, ~30eV - ~45keV ). The electron measurements are obtained 
21.5 secs after the ion measurements. Epoch is the measurement time 
appropriate for the ions. The moments are computed after the fluxes are 
corrected for background and s/c potential. Algorithms for these corrections
 are relatively unsophisticated, so the moments are suspect during times of 
high background and/or high spacecraft potential. Because the determined  
spacecraft potential is not very precise, the magnitude of the low-energy 
ion flow velocity is probably not accurate, but the flow direction is well 
determined.  Tperp and Tpara are obtained from diagonalization of the  
3-dimensional temperature matrix, with the parallel direction assigned 
to the eigenvalue which is most different from the other two. 
The corresponding eigenvector is the symmetry axis of the distribution and 
should be equivalent to the magnetic field direction. The eigenvalue ratio 
Tperp/Tmid, which is provided for each species, is a measure of the symmetry 
of the distribution and should be ~1.0 for a good determination. Several of  
the parameters have a fairly high daily dynamic range and for survey purposes 
are best displayed logarithmically. These parameters are indicated by  
non-zero 'SCALEMIN' values in this file. A quality flag value of 1  
indicates that the values are  preliminary and have not been checked 
in detail.


Modification History
Created SEP 1992 Modified JAN 1993 
Electron time tags removed Mag Latitude added 
Local time added Post Gap flag added 
Ratio variables changed Modified SEP 1994 
Changes noted in mail message from M.Kessel


Variable Notes

[Computed 3-min vector] S/C position, GCI coordinates (X, Y, Z)
This is a virtual variable generated by read_myCDF w/ useof the data in the
sc_pos_geo variable and a conversion routinespecified in the function attribute,
namely conv_pos
[Computed 3-min vector] S/C position, GEO coordinates (Radius, Lat.,Lon.)
This is a virtual variable generated by read_myCDF w/ useof the data in the
sc_pos_geo variable and a conversion routinespecified in the function attribute,
namely conv_pos


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L9_K0_SPA
Description
     Electron, proton and helium measurements are taken every 160 ms from one 
of the three telescopes according to the following sequence:  T1, T2, T3, 
T2, T1, T2 etc.  Heavy ion data accumulated from each of the three telescopes 
again according to the timing and sequence above and summed for 10.24 seconds
which is approximately one spacecraft rotation.  SOPA Key Parameters are 
normally averaged over three telescopes for ~ 1 minute (6 - 10.24 second
data accumulation cycles) giving an average over much of the sky.  The time 
associated with each set of Key Parameters is determined by using the time 
(in minutes of the day) at the start of each data collection cycle as an index
into an array of 1440 time slots dividing the day into 1440 one minute 
intervals.  The time reported is the midpoint of each interval.  
     We provide six fluxes:
        Low energy Protons:  50 keV to 400 keV
        High energy Protons: 1.2 MeV to 5 MeV
        Low energy Electrons:  50 keV to 225 keV
        High energy Electrons: 315 keV to 1.5 MeV
        Helium      : ~0.9 MeV to ~1.3 Mev
        Heavy Ions  : ~5 MeV to ~15 MeV (includes carbon, nitrogen,
                       and oxygen
     We also compute two electron temperatures and densities and two proton
temperatures and densities.  These are based on approximately the same energy
ranges as the fluxes given in above and are determined for relativistic
Maxwellian distributions.  
 
Status of SOPA Instrument 1989-046:  Operating normally as of 01-Feb-1993
   
Data is flagged with a data quality flag as follows:
   +1 Data is Good
    0 Data is Suspect
   -1 Data is Unusable
LANL personnel should be contacted before using any data tagged as suspect.
References:   Belian, R. D., Gisler, G. R., Cayton, T. E., Christensen, R. A.
High-Z Energetic Particles at Geosynchronous Orbit During The Great Solar 
Proton Event Series of October 1989, J. Geophys. Res., 97, 16897, 1992


Modification History
created 30-Nov-1992 
added text to describe instrument 04-Feb-1993
Data reduction software updated.  Temperature and 
Density algorithms implemented  15-dec-1993
Repaired some errors in the skeleton table 21-Feb-1995
Implemented updated algorithm for calculating Electron and Proton densities
 and temperatures  21-Feb-1995


Variable Notes

Electron temperature in 2 energy bands (50-225 keV, 315-1500 keV)
Electron temperature determined from relativistic Maxwellian distributions and
averaged over 3 11deg telescopes (separated by  30deg) rotating with spacecraft
Protron temperature in 2 energy bands (50-400 keV, 1.2-5.0 MeV)
Protron temperature determined from relativistic Maxwellian distributions and
averaged over 3 11deg telescopes (separated by  30deg) rotating with spacecraft
Partial electron densities in 2 energy bands (50-225 keV, 315-1500 keV)
Partial electron densities determined from relativistic Maxwellian distributions
and averaged over 3 11deg telescopes (separated by  30deg) rotating with
spacecraft
Partial protron densities in 2 energy bands (50-400 keV, 1.2-5.0 MeV)
Partial protron densities determined from relativistic Maxwellian distributions
and averaged over 3 11deg telescopes (separated by  30deg) rotating with
spacecraft
alpha flux (Helium) from ~0.9 MeV to ~1.3 Mev
alpha flux (Helium) averaged over 3 11deg telescopes (separated by  30deg)
rotating with spacecraft
Heavy Ion flux at ~5 MeV to ~15 MeV (includes carbon, nitrogen, and oxygen
Heavy Ion flux averaged over 3 11deg telescopes (separated by  30deg) rotating
with spacecraft
Electron flux in 2 energy bands (50-225 keV, 315-1500 keV)
Electron flux is averaged over 3 11deg telescopes (separated by  30deg) rotating
with spacecraft
protron flux in 2 energy bands (50-400 keV, 1.2-5.0 MeV)
protron flux averaged over 3 11deg telescopes (separated by  30deg) rotating
with spacecraft


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MAP_HK_ACS
Description
tbs


Modification History
tbs




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MAP_HK_CDH
Description
tbs


Modification History
tbs




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MAP_HK_PRO
Description
tbs


Modification History
tbs




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MAP_HK_PSE
Description
tbs


Modification History
tbs




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MAP_HK_RF
Description
tbs


Modification History
tbs




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MAP_HL_ACS
Description
tbs


Modification History
tbs




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MAP_HL_CDH
Description
tbs


Modification History
tbs




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MAP_HL_PRO
Description
tbs


Modification History
tbs




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MAP_HL_PSE
Description
tbs


Modification History
tbs




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MAP_HL_RF
Description
tbs


Modification History
tbs




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NOAA05_H0_SEM
Description
TIROS/NOAA SEM MEPED Data Archive         
                                          
This is the re-processed version of the   
MEPED data archive from the TIROS/NOAA    
spacecraft.  The raw data from the NOAA   
archive have been processed to correct    
the magnetic field parameters (BR, BT,    
BP, Bmin, and L) and to sum the detector  
counts over an 8 second interval.         
Details of the processing can be found    
in NASA/CR-1998-208593.  Processing was   
done by:                                  
                                          
S. L. Huston                              
The Boeing Company                        
5301 Bolsa Ave.                           
Huntington Beach, CA 92647                
USA                                       
Phone: 714-896-4787                       
e-mail: stuart.l.huston@boeing.com


Modification History
Created Nov. 1998




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NOAA06_H0_SEM
Description
TIROS/NOAA SEM MEPED Data Archive         
                                          
This is the re-processed version of the   
MEPED data archive from the TIROS/NOAA    
spacecraft.  The raw data from the NOAA   
archive have been processed to correct    
the magnetic field parameters (BR, BT,    
BP, Bmin, and L) and to sum the detector  
counts over an 8 second interval.         
Details of the processing can be found    
in NASA/CR-1998-208593.  Processing was   
done by:                                  
                                          
S. L. Huston                              
The Boeing Company                        
5301 Bolsa Ave.                           
Huntington Beach, CA 92647                
USA                                       
Phone: 714-896-4787                       
e-mail: stuart.l.huston@boeing.com


Modification History
Created February 2002




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OHZORA_H0_HEP
Description
OHZORA High Energy Particle Observations, K. Nagata, et al., J. Geomag. Geoelectr., 37, 329-345,
1985


Modification History
TBD




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OMNI_H0_MRG1HR
Description
Hourly averaged definitive multispacecraft interplanetary parameters data


Modification History
created October 1998;
conversion to ISTP/IACG CDFs via SKTEditor Feb 2000




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PO_AT_DEF
Description
TBS


Modification History
6/13/91 - Original Implementation
9/18/91 - Modified for new attitude file format changes.  ICCR 881
2/11/92 - Used the variable name TIME and type CDF_INT4 and size 3 instead of 
EPOCH, CDF_EPOCH and 1 for the time tags.  CCR 490
6/1/92 - Added global attributes TITLE, PROJECT, DISCIPLINE, SOURCE_NAME, 
DATA_VERSION, and MODS; added variable attributes VALIDMIN, VALIDMAX, 
LABL_PTR_1, and MONOTON; added variables EPOCH and LABEL_TIME; 
changed variable name TIME to TIME_PB5.  CCR 1066
11/07/92 - use cdf variable Epoch and Time_PB5
6/8/93 - Added global attributes ADID_ref and Logical_file_id.  CCR 1092
7/5/94 - CCR ISTP 1852, updated CDHF skeleton to CDF standards - JT
9/20/94 - Added global attributes GCI_RA_ERR and GCI_DECL_ERR.  CCR 1932
11/7/94 - Merged CCR 1852 changes and corrected errors 
made in CCR 1852.  ICCR 1884
12/7/94 - Modified MODS and LABLAXIS to follow ISTP standards.  ICCR 1885




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PO_AT_PRE
Description
TBS


Modification History
6/13/91 - Original Implementation
9/18/91 - Modified for new attitude file format changes.  ICCR 881
2/11/92 - Used the variable name TIME and type CDF_INT4 and size 3 instead of 
EPOCH, CDF_EPOCH and 1 for the time tags.  CCR 490
6/1/92 - Added global attributes TITLE, PROJECT, DISCIPLINE, SOURCE_NAME, 
DATA_VERSION, and MODS; added variable attributes VALIDMIN, VALIDMAX, 
LABL_PTR_1, and MONOTON; added variables EPOCH and LABEL_TIME; 
changed variable name TIME to TIME_PB5.  CCR 1066
11/07/92 - use cdf variable Epoch and Time_PB5
6/8/93 - Added global attributes ADID_ref and Logical_file_id.  CCR 1092
7/5/94 - CCR ISTP 1852, updated CDHF skeleton to CDF standards - JT
9/20/94 - Added global attributes GCI_RA_ERR and GCI_DECL_ERR.  CCR 1932
11/7/94 - Merged CCR 1852 changes and corrected errors 
made in CCR 1852.  ICCR 1884
12/7/94 - Modified MODS and LABLAXIS to follow ISTP standards.  ICCR 1885




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PO_EJ_VIS
Description
Instrument functional description:
   The VIS is a set of three low-light-level cameras.  Two of these
   cameras share primary and some secondary optics and are designed to
   provide images of the nighttime auroral oval at visible wavelengths.
   A third camera is used to monitor the directions of the fields-of-view
   of the auroral cameras with respect to the sunlit Earth and return
   global images of the auroral oval at ultraviolet wavelengths.  The
   VIS instrumentation produces an auroral image of 256 x 256 pixels
   approximately every 24 seconds dependent on the integration time and
   filter selected.  The fields-of-view of the two nighttime auroral
   cameras are 5.6 x 6.3 degrees and 2.8 x 3.3 degrees for the low and
   medium resolution cameras, respectively.  One or more Earth camera
   images of 256 x 256 pixels are produced every five minutes, depending
   on the commanded mode.  The field-of-view of the Earth camera is
   approximately 20 x 20 degrees.
 
Reference:
   Frank, L. A., J. B. Sigwarth, J. D. Craven, J. P. Cravens, J. S. Dolan,
       M. R. Dvorsky, J. D. Harvey, P. K. Hardebeck, and D. Muller,
       'The Visible Imaging System (VIS) for the Polar Spacecraft',
       Space Science Review, vol. 71, pp. 297-328, 1995.
 
[Note to first-time users:  The first four variables are of primary
interest.  The displayable 256 x 256 image array is in variable 3.  The
correct orien- tation of a displayed image is explained in the
description of variable 3 below.]
 
Data set description:
   The VIS Earth camera data set comprises all Earth camera images for
the selected time period.  EJ-ER type files have images that have been
processed to remove the effects of penetrating radiation.  In addition,
the images have been flat-fielded and fixed pattern noise has been
removed.  Image pixels are median filtered with the images immediately
before and after in time.  The displayable image counts are in variable
3.  Some coordinate information is included for viewer orientation.
Coordinates are calculated for a grid of 18 x 18 points corresponding to
one pixel out of every 15 x 15 pixel block.  In addition, a rotation
matrix and a table of distortion-correcting look direction unit vectors
are provided for the purpose of calculating coordinates for every pixel.
See the description of variables 14 and 15 below.  To facilitate viewing
of the images, a mapping of pixel value to a recommended color table
based on the characteristics of the selected filter will be included with
each image.  See the description of variables 19, 20, and 21 below.  A
relative intensity scale is provided by the uncompressed count table of
variable 24.  Approximate intensity levels in kiloRayleighs are given in
the intensity table of variable 25.  Information on the availability of
more precisely calibrated intensities can be found on the VIS website at
URL .http://eiger.physics.uiowa.edu/~vis/software/. 
 
Variable descriptions:
 
   1,2. Center time
       The time assigned to an image is the center time of the integration
       period within a resolution of 50 milliseconds.
 
   3. Image counts
       Image pixel counts range from 0 to 255.  They are stored in a two-
       dimensional 256 x 256 byte array.  Images from the Earth camera
       (sensor 0) are conventionally displayed with row 1 at the top, row 256
       at the bottom, column 1 on the left, and column 256 on the right.  The
       conventional image display for the low resolution camera (sensor 1) is
       rotated 180 degrees so that the row 1-column 1 pixel is at the lower
       right corner and the row 256-column 256 pixel is at the upper left
       corner.  When displayed in this manner, the spacecraft spin axis is
       oriented to the right in the display, the X component is defined as
       the center of the image look direction, and the Y component is the
   4. Sensor number
 
       0 = Earth camera,
       1 = low resolution camera,
       2 = medium resolution camera.
 
   5. Half integration time
       This is half the length of the integration period for the image,
       measured in milliseconds.
 
   6. Filter
       Twelve filters are available for visible imaging; the filter number,
       1-12, is given here.  Ultra-violet imaging is done with one filter
       only, designated here as filter number 0.  In addition, the peak
       wavelength in Angstroms is given for the selected filter.
 
   7. Presumed altitude of emissions
       The presumed altitude of the emissions seen in the image varies
       with the characteristics of the filter used.
 
   8. Platform pitch angle
       This is the platform pointing angle of rotation around the spin
       axis, measured from nadir.
 
 9,10. Geographic coordinates
       Geographic north latitude and east longitude are provided for the
       pixels at these image array locations: every 15th row starting
       with row 1 and ending with row 256, and every 15th column starting
       with column 1 and ending with column 256, for a total of
       18 x 18 coordinate pairs.
 
11,12. Spacecraft position and velocity vectors, GCI
       The spacecraft position vector and velocity vector in GCI
       coordinates are for the image center time as given in variables
       1 and 2.
 
  13. Spacecraft spin axis unit vector, GCI
 
14,15. Image-to-GCI rotation matrix and look direction vector table
       The rotation matrix may be used with the look direction vector table to
       obtain pointing vectors in GCI coordinates for each pixel.  The
       resulting vectors may be used to calculate coordinates for the observed
       positions of the pixels.  Software for this purpose is available at URL
       .http://eiger.physics.uiowa.edu/~vis/software/.  The general method 
       used is described below.
 
       In the image coordinate system, the X axis is the center line-of-sight
       or look direction; the Y axis is the cross product of the spin axis an
       the X axis; and the Z axis is the cross product of the X axis and the
       Y axis.  When the display orientation conventions in the variable 3
       description are applied, the low resolution camera image is rotated so
       that both Earth camera and low resolution camera images are displayed
       with Y axis pointing up and Z axis pointing toward the right.
 
       To obtain the coordinates of the observed position of a pixel,
       calculate the intersection of the line-of-sight with the surface
       of an oblately spheroidal Earth at the altitude given as
       variable 7.  The equation of the spheroid is
           X**2/(A+ALT)**2 + Y**2/(A+ALT)**2 + Z**2/(B+ALT)**2 = 1
           where A is the Earth radius at the equator,
                 B is the Earth radius at the pole, and
                 ALT is the given altitude.
       The line-of-sight equations are
           (X-SCX)/DX = (Y-SCY)/DY = (Z-SCZ)/DZ
           where (SCX,SCY,SCZ) is the spacecraft position vector GCI, and
                   (DX,DY,DZ)  is the look direction unit vector GCI.
       Solve the line-of-sight equations for two variables in terms
       of the third; substitute into the spheroid equation; and use the
       quadratic formula to solve for the third variable.  Select
       the solution point closer to the spacecraft.
 
  16. Zenith angle of center line-of-sight at presumed altitude
       This is the angle between the geocentric vector through the
       observed point, assuming the altitude given as variable 7,
       and the reverse of the image center line-of-sight vector.
 
  17. Sun position unit vector, GCI
 
  18. Solar zenith angle at observed point of center line-of-sight
       This is the angle of the sun from zenith at the observed point
       of the center line-of-sight, assuming the altitude given as
       variable 7.
 
  19. RGB color table
       This is the recommended color table to be used with the
       limits given in variables 20 and 21.
 
20,21. Low and high color mapping limits
       The low and high color limits are recommended for remapping
       the color table entries, as follows:
           For pixel values less than the low limit, use the color
               at table position 1.
       assignments:
               and less than or equal to the high limit, use the color
               at table position (pix-low)/(high-low) x 255 + 1.
           For pixel values greater than the high limit, use the color
               at table position 256.
 
  22. Data quality flag
       The data quality word has bits set to 1 when the listed
       conditions are true.  Bit #31 is the most significant bit in the
       word, and it will not be used as a flag.  These are the bit
           bit 0 - image data frame sync error
           bit 1 - image data frame counters error
           bit 2 - image data fill frame flag.
 
  23. Post gap flag
       The post gap flag has these possible values:
           0 - no gap occurred immediately prior to this record,
           1 - the gap occurred because the instrument was not in
                 a mode that allowed for the production of images for the
                 selected sensor,
           2 - the gap occurred because level zero data were missing,
           3 - the gap occurred because level zero data were too
                 noisy to extract images.
 
  24. Expanded count table
       The image pixel counts are quasi-logarithmically compressed to the
       range 0-255.  This table gives the average of the uncompressed range
       for each compressed count value.  Table entries 1-256 correspond to
       compressed counts 0-255 respectively.
 
  25. Intensity table
       Approximate intensity levels in kiloRayleighs are given for each
       compressed count value.  Table entries 1-256 correspond to compressed
       counts 0-255 respectively.  Information on the availability of more
       precisely calibrated intensities can be found on the VIS website at
       URL .http://eiger.physics.uiowa.edu/~vis/software/. 
 
Supporting software:
   Supporting software is available on the VIS website at the URL
   .http://eiger.physics.uiowa.edu/~vis/software/.  Included is an IDL 
   program that displays the images with the recommended color bar and
   provides approximate intensities and coordinate data for each pixel.


Modification History
Initial development
Updated TEXT section bug
Updated some variables
Added an ADID number, same as K1
changed linear validmin 0->10, validmax 255->60 to suppress dayglow - 4/12/01 - REM
changed log validmin 0->1, validmax 255->18 to suppress dayglow - 4/12/01 - REM


Variable Notes

Earth Camara UV Images (quasi-log cnts), small format display with click-expand (~1 min. res.)
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> Larger format display with click-expand, no geographic registration.
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) With geographic map overlay
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> [DO NOT USE: UNDER-DEVELOPMENT] Test Display
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Azimuthal projection to geographic (fixed sun orientation)
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Azimuthal projection to magnetic LT and invariant lat
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
(USE SHORT TIME SPANS) Movie display of images, no geographic registration.
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) With geographic grid overlay
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Azimuthal projection to geographic (fixed sun orientation)
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Azimuthal projection to magnetic LT and invariant lat
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
Earth Camara UV Images (kRay), small format display with click-expand (~1 min. res.)
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> Larger format display with click-expand, no geographic registration.
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) With geographic grid overlay
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Azimuthal projection to geographic (fixed sun orientation)
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Azimuthal projection to magnetic LT and invariant lat
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
(USE SHORT TIME SPANS) Movie display of images, no geographic registration.
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) With geographic grid overlay
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Azimuthal projection to geographic (fixed sun orientation)
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Azimuthal projection to magnetic LT and invariant lat
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
Geographic latitude grid - virtual var.
Geographic N. latitude for pixels vals - computed by CDAWeb
Geographic longitude grid - virtual var.
Geographic E. longitude for pixels vals - computed by CDAWeb
Filter number and peak wavelength in Angstroms)
Filters #1-12 are visible wavelengths; filter #0 is UV for Earth camera images
Platform pointing angle from nadir
Platform angle of rotation around spin axis, measured from nadir in tenths of
degrees
Geographic latitude grid
Geographic N. latitude for pixels at every 15th row and column from 1 to 256
Geographic longitude grid
Geographic E. longitude for pixels at every 15th row and column from 1 to 256
Image-to-GCI rotation matrix
X component is look direction,Y component is the spin axis  cross X
RGB color lookup table
RGBColorTable should be remapped for displaying an image using the low and high
limits given for each image in Limit_Lo and Limit_Hi.Image_Counts count values
less than Limit_Lo use the color at table position 1.  Count values greater than
Limit_Hi use the color at table position 256.  For count values greater than or
equal to Limit_Lo and less than or equal to Limit_Hi, the table position is
(Count-Limit_Lo)/(Limit_Hi-Limit_Lo) x 255 + 1.At the selected table position C,
the color components are Red at RGBColorTable(1,C), Green at RGBColorTable(2,C),
and Blue at RGBColorTable(3,C).
Data quality flags
MSB will not be used as a flag; see TEXT for other bit assignments
Expanded count table: quasi-logarithmically uncompressed pixel counts
Image_Counts contains pixel counts which have been quasi-logarithmically
compressed by the instrument.  Approximate uncompressed value
forImage_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).
Approximate intensity levels in kiloRayleighs
Approximate intensity in kR for Image_Counts(i,j)
isIntens_Table(Image_Counts(i,j)+1)


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PO_H0_CAM
No TEXT global attribute.


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PO_H0_CEP
No TEXT global attribute.


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PO_H0_HYD
Description
Reference: HYDRA is a 3-Dimensional Electron and Ion Hot  plasma Instrument for the Polar Spacecraft
of the GGS Mission, J. Scudder et al., Space Sci. Rev., 71, 459-495, Feb. 1995.
This data set contains the differential electron and proton fluxes vs energy, at 13.8-second
resolution. There are 29 energy channels from 12.5 ev to 18.3 keV.
J. Scudder, et.al, Space Sci. Rev., 71, 459-495, 1995, http://www-st.physics.uiowa.edu




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PO_H0_PWI
Description
Reference:..Gurnett, D.A. et al, The Polar plasma wave instrument, Space Science Reviews, Vol. 71,
pp. 597-622, 1995.GURNETT@IOWAVE.physics.uiowa.edu
Note:..The electron cyclotron frequencies are derived from the following:  Fce = 0.028 kHz*B, where
B is the magnitude of the ambient magnetic field measured in nT.  All frequencies are converted to
Hz.
There are 20 MCA E frequency bands, logarithmically spaced and 14 MCA B frequency bands,
logarithmically spaced.


Modification History
Created Dec 1997


Variable Notes

Time, begin time of spectrum
Contains Year, DOY, MSOD
Mag. Field at 14 freq., 5.62-10000 Hz (MCA B)
Uses the first 14 Frequency Values


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PO_H0_TID
Description
TIDE data for dates 28-Mar-1996 to 15-Sep-1996 are mass resolved. 
TIDE data between 15-Sep-1996 and 07-Dec-1996 are not valid.


Modification History
Skeleton table version 1 created 08/10/98.
Skeleton table version 2 created 10/16/00.


Variable Notes

H+ Ion density
Only available before 15-Sep-1996
H+ Ion Plasma Velocity, Field Aligned, available before 15-Sep-1996
Available before 15-Sep-1996 only,for energy, spin angle, and polar angle
calculation see moments_lim.
H+ Ion Temperature, Parallel and Perendicular to the Magnetic Field, available before 15-Sep-1996.
Only available before 15-Sep-1996.  Direction of magnetic field obtained from
onboard values. See moments_lim for energy, spin angle, and polar angle
calculation limits.
H+ Energy Spectrogram
Flux values summed over spin and polarangles.  See spect_lim for summation
limits.
H+ Spin Angle Spectrogram
Flux values summed over energy and polar angle.  See spect_lim for summation
limits.
H+ Polar Angle Spectrogram
Flux values summed over energy and spin angle.  See spect_lim for summation
limits.
O+ Ion Density
Only available before 15-Sep-1996
O+ Ion Plasma Velocity, Field Aligned, available before 15-Sep-1996
Available before 15-Sep-1996 only,for energy, spin angle, and polar angle
calculation limits see moments_lim.
O+ Ion Temperature, Parallel and Perendicular to the Magnetic Field, available before 15-Sep-1996.
Only available before 15-Sep-1996.  Direction of magnetic field obtained from
onboard values. See moments_lim for energy, spin angle, and polar angle
calculation limits.
O+ Energy Spectrogram
Flux values summed over spin and polarangles.  See spect_lim for summation
limits.
O+ Spin Angle Spectrogram
Flux values summed over energy and polar angle.  See spect_lim for summation
limits.
O+ Polar Angle Spectrogram
Flux values summed over energy and spin angle.  See spect_lim for summation
limits.
He+ Ion Density
Only available before 15-Sep-1996
He+ Ion Plasma Velocity, Field Aligned, available before 15-Sep-1996
Available before 15-Sep-1996 only,for energy, spin angle, and polar angle
calculation see moments_lim.
He+ Ion Temperature, Parallel and Perendicular to Magnetic Field, available before 15-Sep-1996.
Only available before 15-Sep-1996.  Direction of magnetic field obtained from
onboard values. See moments_lim for energy, spin angle, and polar angle
calculation limits.
He+ Energy Spectrogram
Flux values summed over spin and polarangles.  See spect_lim for summation
limits.
He+ Spin Angle Spectrogram
Flux values summed over energy and polar angle.  See spect_lim for summation
limits.
He+ Polar Angle Spectrogram
Flux values summed over energy and spin angle.  See spect_lim for summation
limits.
TIDE Instrument Status (0-off,1-on,2-standby,3-mirrors stepped)
TIDE instrument status flag:  0 - TIDE not operational or data missing, 1 - TIDE
fully operational, 2 - TIDE MCP high voltages lowered for passage through
radiation belt, 3 - TIDE mirrors stepped down due to high counts, calibration
applied to correct counts.
PSI Instrument Status (0-off,1-on,2-standby)
PSI instrument status flag:  0 - PSI not operation or data missing, 1 - PSI
fully operational, 2 - PSI on but keeper not ignited.
Spacecraft Potential (from EFI K0 or a constant value)
value either constant or from EFI K0
Spacecraft Ram Spin Angle
spin angle direction of the spacecraft
Spacecraft Ram Polar Angle
polar angle direction of the spacecraft
Magnetic Field Azimuth
magnetic field elevation
Magnetic Field Elevation
magnetic field elevation
Spins Averaged
the number of spacecraft spins averaged for each time period
Minimum count subtracted
If sub_min = 1, the minimum count in each spin of data has been subtracted as a
means of reducing the noice level. If sub_min = 0, no minimum count subtraction
was done.
spectrogram count option
The counts in the spectrograms can be summed (1), averaged (2), or the maximum
(3) of the data whose ranges are specified in spect_lim.
source of b-field data
The b-field data (mag_az and mag_el) can either be from TIDE telemetry (0) or
from MFE high time resolution data (1).
software version number
The version of the TIDE level-zero processing software used to create the CDF
file.
moments calculation limits
The energy and spin and polar angle ranges used in the moments calculations
spectrogram summing limits
The energy and spin and polar angle ranges used to create the spectrogram sums


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PO_H0_TIM
Description
H+, O+, He+ and He++ number fluxes and statistical 
uncertainties processed by 
 the TIMAS science team.  Data acquired   
with various anglular and energy 
resolutions are combined here.  
Data Quality and other indicators are provided 
 to allow selection of high 
 resolution data (PA_status(ion)=0 and  
 Energy_status(ion)=0 )  and  
 High Quality data (Quality=0). 
 See the VAR_NOTES for the following  
 variables for more detailed information.  
Quality, PA_status, Energy_status 
Bcr, Fec, Even_odd,  
Energy_Range_ID and Spins. 
A PAPCO module exists that reads 
and displays these data and data 
From other POLAR instruments.  See
http://www.mpae.gwdg.de/mpae_projects/CCR/software/papco/papco.html and the pointer to a description
of the TIMAS PAPCO module on the TIMAS home page.
Reference:
E.G. Shelley et al., The Toroidal Imaging Mass-Angle Spectrograph (TIMAS) for the Polar Mission, Sp.
Sci. Rev, Vol 71, pp 497-530, 1995.
ftp://sierra.spasci.com/DATA/timas/TIMAS_description.html



Metadata provided by W.K. Peterson


Modification History
Version 0 December, 1997 
Version 1 July, 1998 
Version 2 December, 2000 Algorithm improved to more accurately subtract backgrounds arising from
spill over from H+ into He++ channel and other sources.  Fill data are now inserted for limited
energy and pitch angle ranges for Flux_H Flux_O Flux_He_1 and Flux_He_2 variables. The meanging of
values of the of Quality variable have been slightly modified


Variable Notes

NSSDC standard-reference time value at the center of the accumulation interval.
Center epoch (milliseconds since 0 AD of VARIABLE accumulation intervals for H+.
 See also variables Epoch_start, Epoch_stop, and Spins
NSSDC standard-reference time value at the center of the accumulation interval.
Center epoch (milliseconds since 0 AD of VARIABLE accumulation intervals for O+.
 See also variables Epoch_start, Epoch_stop, and Spins
NSSDC standard-reference time value at the center of the accumulation interval.
Center epoch (milliseconds since 0 ADof VARIABLE accumulation intervals for He+.
 See also variables Epoch_start, Epoch_stop, and Spins
NSSDC standard-reference time value at the center of the accumulation interval.
Center epoch (milliseconds since 0 ADof VARIABLE accumulation intervals for
He++.  See also variables Epoch_start, Epoch_stop, and Spins
NSSDC standard-reference time value. 
Start epoch of VARIABLE accumulation intervals for H+, O+, He+ and He++ ions. 
This variable is used to pass   interval times to the TIMAS PAPCO module.
NSSDC standard-reference time value. 
Stop epoch of VARIABLE accumulation intervals for H+, O+, He+ and He++ ions. 
This variable is used to pass   interval times to the TIMAS PAPCO module.
H+ number flux for 28 energy and 3 selected angle bins - quality flag applied.
CDAWeb VV - Negative values reflect low counting rates and background
subtraction.
H+ number flux for 6 selected energies and 12 angle bins - quality flag applied.
CDAWeb VV - Negative values reflect low counting rates and background
subtraction.
[DO NOT USE-NO QFLAG FILTER] % Sigma for H+ number flux for 28 energies and 3 selected angle bins.
Value clipped at 255% of flux.
% Sigma for H+ number flux for 28 energies and 3 selected angle bins - quality flag applied
Value clipped at 255% of flux.
% Sigma for H+ number flux for 6 selected energies and 12 angle bins.
VV - Value clipped at 255% of flux.
% Sigma for H+ number flux for 6 selected energies and 12 angle bins - quality flag applied.
VV - Value clipped at 255% of flux.
[DO NOT USE-NO QFLAG FILTER] O+ number flux for 28 energies and 3 selected angle bins.
Negative values reflect low counting rates and background subtraction.
O+ number flux for 28 energy and 3 selected angle bins - quality flag applied.
VV - Negative values reflect low counting rates and background subtraction.
O+ number flux for 6 selected energies and 12 angle bins.
VV - Negative values reflect low counting rates and background subtraction.
O+ number flux for 6 selected energies and 12 angle bins - quality flag applied.
VV - Negative values reflect low counting rates and background subtraction.
[DO NOT USE-NO QFLAG FILTER] % Sigma for O+ number flux for 28 energies and 3 selected angle bins.
Value clipped at 255% of flux.
% Sigma for O+ number flux for 28 energies and 3 selected angle bins - quality flag applied.
Value clipped at 255% of flux.
% Sigma for O+ number flux for 6 selected energies and 12 angle bins.
VV - Value clipped at 255% of flux.
% Sigma for O+ number flux for 6 selected energies and 12 angle bins - quality flag applied.
VV - Value clipped at 255% of flux.
[DO NOT USE-NO QFLAG FILTER] He+ number flux for 28 energies and 3 selected angle bins.
Negative values reflect low counting rates and background subtraction.
He+ number flux for 28 energies and 3 selected angle bins - quality flag applied.
Negative values reflect low counting rates and background subtraction.
He+ number flux for 6 selected energies and 12 angle bins.
VV - Negative values reflect low counting rates and background subtraction.
He+ number flux for 6 selected energies and 12 angle bins - quality flag applied.
VV - Negative values reflect low counting rates and background subtraction.
[DO NOT USE-NO QFLAG FILTER] % Sigma for He+ number flux for 28 energies and 3 selected angle bins.
Value clipped at 255% of flux.
% Sigma for He+ number flux for 28 energies and 3 selected angle bins - quality flag applied.
Value clipped at 255% of flux.
% Sigma for He+ number flux for 6 selected energies and 12 angle bins.
VV - Value clipped at 255% of flux.
% Sigma for He+ number flux for 6 selected energies and 12 angle bins - quality flag applied
VV - Value clipped at 255% of flux.
[DO NOT USE-NO QFLAG FILTER] He++ number flux for 28 energies and 3 selected angle bins.
Negative values reflect low counting rates and background subtraction.
He++ number flux for 28 energies and 3 selected angle bins - quality flag applied.
Negative values reflect low counting rates and background subtraction.
He++ number flux for for 28 energy and 12 angle bins.
VV-Negative values reflect low counting rates and background subtraction.
He++ number flux for for 28 energy and 12 angle bins - quality flag applied.
VV-Negative values reflect low counting rates and background subtraction.
[DO NOT USE-NO QFLAG FILTER] % Sigma for He++ number flux for 28 energy and 3 angle bins.
Value clipped at 255% of flux.
% Sigma for He++ number flux for 28 energy and 3 angle bins - quality flag applied.
Value clipped at 255% of flux.
% Sigma for He++ number flux for 6 selected energies and 12 angle bins.
VV - Value clipped at 255% of flux.
% Sigma for He++ number flux for 6 selected energies and 12 angle bins - quality flag applied. 
VV - Value clipped at 255% of flux.
Energy Range Identification: 0: Full energy range; 1: Reduced energy range; 2: Low energy range
TIMAS is operated in one of 3  energy ranges. Energy_Range_ID indicates which of
the 3 instrumental energy ranges is currently active. Each instrumental energy
range further divided into 3 Key Parameter (KP) energy channels (low - medium -
and high). The table below gives the full energy range and limits of the three
KP energy ranges. Energy_Range_ID=0: (Full instrumental energy range)Full range
(0.015 - 33.3 keV/e)low E channel (0.015 - 0.37 keV/e)mid E channel (0.37 - 3.3
keV/e)high E channel (3.3 - 33.3 keV/e)Energy_Range_ID=1: (Reduced instrumental
energy range)Full range (0.015 - 22.45 keV/e)low E channel (0.015 - 0.37
keV/e)mid E channel (0.37 - 3.3 keV/e)high E channel (3.3 - 22.45
keV/e)Energy_Range_ID=2: (Low instrumental energy range)Full range (0.015 - 2.18
keV/e)low E channel (0.015 - 0.11 keV/e)mid E channel (0.11 - 0.37 keV/e)high E
channel (0.37 - 2.18 keV/e)
Even/Odd Spin Identification
 0 first (even) spin with even    numbered energy steps   1 second (odd) spin
with odd    numbered energy steps. TIMAS samples 28 energy steps  over the full
energy range every  two spins (12 seconds).  On even  numbered spins the lowest
energy  step (centered at 25 eV/e) and  alternate energy steps over the  full
energy range are sampled. On odd spins the second energy step  (centered at 45
eV/e) and alternate  energy steps to the maximum are  sampled.
Total counts per spin in the fast event counter 
The TIMAS detector has a non  linear response at high count  rates that is, to
some extent  corrected for in the software  that generated the data here.  The
correction, however introduces  some uncertainty.  The FEC count  rate is
carried as an indication of  the corrections applied to the  raw data.
Total Background counts per spin 
Total background counts per  spin
Number of spins accumulated for the four ion species
Number of spins of data accumulatedfor each of the 4 major ion species .
Energy Resolution Indicators (0=best, 99=invalid energies)
TIMAS data are available from operational  modes with full (28 bins) or moderate
 (7 bins) energy resolution.  These data  were assembled from various data
products  with different energy resolution. Data are  given in this file with
full 28 energy  step resolution EVEN IF ONLY 7 energy  step resolution data are
available.    This flag documents the resolution of   the data included in the
average.   Values are:  0    All single spin 14 energy step data.  1    Mostly
14 energy step data. Some 7 energy step. All one or two spin.2    Mostly 7
energy step data. Some 14 energy step. All one or two spin. 3    All one or two
spin 7 energy step data.4    Mostly 14 energy step data. Some 7 energy step
multispins. 5    Mostly one or two spin 7 energy step data. Some multispins. 6  
 Mostly multispin 7 energy step data. 7    All multispin 7 energy step data. 99 
 Invalid energies.Some of these conditions (1,2,4,5,6) are very rare.
Pitch Angle Resolution Flags (0=best; >3=smeared PAs; 99=invalid PAs with omnidirec flux in 0-15 deg)
TIMAS data are available from operational  modes with various anglular
resolutions.  These data  were assembled from various data products  with
different angular  resolutions. Data  are  given in this file with full 12
angular   bin resolution EVEN IF 12 angular bin  resolution is not available in
the input  data. This flag documents the resolution of the data included in the
average.   Values are: 0    All 22 degree data. 1    Mostly 22 degree data. 2   
Mostly 45 degree data. 3    All 45 degree data. 4    Smeared 22 degree data. Not
spin locked.5    Smeared 45 degree data. Not spin locked.99   Invalid pitch
angles.
Quality flags for H+, O+, He+, He++ (values 0,1,2=good; 3=adequate; >3 bad/do not use)
A quality flag in the range 0-99 with  the following values/meanings  0    OK. 
1    Some data missing.  2    Slight MCP saturation.  3    Moderate MCP
saturation.  4    Severe MCP saturation.  5    No magnetometer data available. 
6    Warning flags set. 99   No valid data.
[DO NOT USE-NO QUALITY FILTERING] H+ number flux for 28 energy and 3 selected angle bins
Negative values reflect low counting rates and background subtraction.
H+ number flux for 6 selected energies and 12 angle bins.
CDAWeb VV - Negative values reflect low counting rates and background
subtraction.


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PO_H0_UVI
Description
References --------------------
1. M. R. Torr, et al., A far ultraviolet imager for the International Solar-Terrestrial Physics
mission, Space Sci. Rev., v71, pp329 - 383, 1995
Notes ------------------------ 
1. The UVI field of view is circular with an 8 degree full width.  The circular image is stored in
IMAGE_DATA as a rectangular array of 228 rows and 200 columns.
2.  Time information is contained in EPOCH, Time_PB5, IMG_MINUS_MSEC, and IMG_PLUS_MSEC.  
3. Pointing information is given in GCI_LOOK_DIR, GEODETIC_LAT, and GEODETIC_LONG.


Modification History
v1.0 Initial Prelaunch Release 10/16/95 
v1.0 Interim Prelaunch Release 
5/8/96 Added KPGS_VERSION
3/9/97 Changed min/max valuesfor IMAGE_DATA


Variable Notes

Epoch
The time in EPOCH and Time_PB5 refer to the center of the image in IMAGE_DATA.
There is an offset of up to 8 major frames between the beginning of the image
exposure and the ATC telemetry time stamp.  The times shown here are corrected
for this and describe the actual time of exposure.
MPEG canned images
The UVI field of view is circular with an 8 degree full width.  The circular
image is stored in IMAGE_DATA as a rectangular array of 228 rows and 200
columns.  Consequently, the corners of each image contain non-image data.  The
non-active corner pixel locations are identified by a corner fill value = -128. 
The image is oriented such that the direction of decreasing row number points
along the spacecraft spin axis.  The direction of decreasing column number
points to the outboard direction (relative to the spin axis).  The orientation
is the same for both detectors.


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PO_H1_PWI
Description
Reference:..Gurnett, D.A. et al, The Polar plasma wave instrument, Space Science Reviews, Vol. 71,
pp. 597-622, 1995.GURNETT@IOWAVE.physics.uiowa.edu
There are 224 SFR frequency bands, logarithmically spaced.  When SFR_MODE is Linear, the 448 linear
frequency bands are mapped to 224 logarithmic bands.


Modification History
Created July 2000


Variable Notes

SFR Mode (0 = Log, 1 = Linear)
Linear mode data is mapped to Log Mode


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PO_H1_TID
Description
TIDE data after 07-Dec-1996 are non-mass total ion contribution below 411 ev


Modification History
Original skeleton table created 10/16/00.


Variable Notes

Total Ion Density
Only avaliable after 07-Dec-1996
Total Ion Plasma Velocity, Field 
Available after 07-Dec-1996 only,for energy and spin angle calculation see
moments_lim.  Vx and Vy only.
Total Ion Temperature, Parallel and Perpendicular to the Magnetic Field. 
Avaliable after 07-Dec-1996.  Direction of magnetic field obtained from onboard
values.
Total Ion Energy Spectrogram. 
Flux values summed over spin and polar angles, see spect_lim for summation
ranges.
Total Ion Spin Angle Spectrogram
Flux values summed over energy and polar angle, see spect_lim for summation
ranges.
TIDE Instrument Status (0-off,1-on,2-standby,3-mirrors stepped)
TIDE instrument status flag:  0 - TIDE not operational or data missing, 1 - TIDE
fully operational, 2 - TIDE MCP high voltages lowered for passage through
radiation belt, 3 - TIDE mirrors stepped down due to high counts, calibration
applied to correct counts.
PSI Instrument Status (0-off,1-on,2-standby)
PSI instrument status flag:  0 - PSI not operation or data missing, 1 - PSI
fully operational, 2 - PSI on but keeper not ignited.
Spacecraft Potential (from EFI K0 or a constant value)
value either constant or from EFI K0
Spacecraft Ram Spin Angle
spin angle direction of the spacecraft
Spacecraft Ram Polar Angle
polar angle direction of the spacecraft
Magnetic Field Azimuth
magnetic field elevation
Magnetic Field Elevation
magnetic field elevation
Mass to Charge Ratio
The mass to charge ratio used in the moments calculations.
Spins Averaged
the number of spacecraft spins averaged for each time period
Minimum count subtracted
If sub_min = 1, the minimum count in each spin of data has been subtracted as a
means of reducing the noice level. If sub_min = 0, no minimum count subtraction
was done.
spectrogram count option
The counts in the spectrograms can be summed (1), averaged (2), or the maximum
(3) of the data whose ranges are specified in spect_lim.
source of b-field data
The b-field data (mag_az and mag_el) can either be from TIDE telemetry (0) or
from MFE high time resolution data (1).
software version number
The version of the TIDE level-zero processing software used to create the CDF
file.
moments calculation limits
The energy and spin and polar angle ranges used in the moments calculations
spectrogram summing limits
The energy and spin and polar angle ranges used to create the spectrogram sums


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PO_H1_UVI
Description
References --------------------
1. M. R. Torr, et al., A far ultraviolet imager for the International Solar-Terrestrial Physics
mission, Space Sci. Rev., v71, pp329 - 383, 1995
Notes ------------------------ 
1. The UVI field of view is circular with an 8 degree full width.  The circular image is stored in
IMAGE_DATA as a rectangular array of 228 rows and 200 columns.
2.  Time information is contained in EPOCH, Time_PB5, IMG_MINUS_MSEC, and IMG_PLUS_MSEC.  
3. Pointing information is given in GCI_LOOK_DIR, GEODETIC_LAT, and GEODETIC_LONG.


Modification History
v1.0 Initial Prelaunch Release 10/16/95 
v1.0 Interim Prelaunch Release 
5/8/96 Added KPGS_VERSION
3/9/97 Changed min/max valuesfor IMAGE_DATA


Variable Notes

Epoch
The time in EPOCH and Time_PB5 refer to the center of the image in IMAGE_DATA.
There is an offset of up to 8 major frames between the beginning of the image
exposure and the ATC telemetry time stamp.  The times shown here are corrected
for this and describe the actual time of exposure.
MPEG canned images
The UVI field of view is circular with an 8 degree full width.  The circular
image is stored in IMAGE_DATA as a rectangular array of 228 rows and 200
columns.  Consequently, the corners of each image contain non-image data.  The
non-active corner pixel locations are identified by a corner fill value = -128. 
The image is oriented such that the direction of decreasing row number points
along the spacecraft spin axis.  The direction of decreasing column number
points to the outboard direction (relative to the spin axis).  The orientation
is the same for both detectors.


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PO_H2_PWI
Description
Reference:..Gurnett, D.A. et al, The Polar plasma wave instrument, Space Science Reviews, Vol. 71,
pp. 597-622, 1995.GURNETT@IOWAVE.physics.uiowa.edu
An FFT on 256 or 464 values, depending on the snapshot size, was used in calibrating the data; i.e.,
perform FFT, calibrate in frequency domain, perform inverse FFT to get calibrated time series.
Coordinate System Used:  local magnetic field-aligned, a spacecraft centered coordinate system where
Z is parallel to the local B-field determined from Polar MFE, X points outward and lies in the plane
defined by the Z-axis and the radial vector from the earth to the spacecraft, and Y completes a
right-handed system and points eastward.  The X- and Z-axes are contained in the north-south plane.
The three orthogonal magnetic field components are given in units of nT/Sec rather than nT because
the response of the searchcoils across the passband is not flat.  In order to obtain units of nT,
the data would need to be digitally filtered to the frequency of interest and then integrated over
time.  Integrating over the entire passband could possibly destroy the resolution of the higher
frequency components since the low frequency noise, if present, will dominate.
Data are bandpass filtered.  The valid range of data in the frequency domain is from 0.5 to 22.5 Hz.


Modification History
Created Oct 1999


Variable Notes

LFWR Elec. Field, Antenna Ex (perp & outward in Local-Field-Aligned/LFA coords)
When FFT is applied, Filter Rolls off at 25 kHz
LFWR Elec. Field, Antenna Ey (perp & eastward in Local-Field-Aligned/LFA coords)
When FFT is applied, Filter Rolls off at 25 kHz
LFWR Elec. Field, Antenna Ez (parallel in Local-Field-Aligned/LFA coords)
When FFT is applied, Filter Rolls off at 25 kHz
LFWR Mag. Field, Antenna Bx (perp & outward in Local-Field-Aligned/LFA coords)
When FFT is applied, Filter Rolls off at 25 kHz
LFWR Mag. Field, Antenna By (perp & eastward in Local-Field-Aligned/LFA coords)
When FFT is applied, Filter Rolls off at 25 kHz
LFWR Mag. Field, Antenna Bz (parallel in Local-Field-Aligned/LFA coords)
When FFT is applied, Filter Rolls off at 25 kHz


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PO_H2_UVI
Description
Primary UVI team data products
CDAWeb displayed images have time-tags shifted 51 seconds back from nominal Epoch
This corrects that H2 Epochs are telemetry times, not centered collection time
51 seconds is an approximate, typical correction.  Exact values depend on modes and transition
status.


Modification History
Initial work at SPDF 3/20-x/xx/2001 by REM


Variable Notes

Data quality suspect flag (0=OK,1=Suspect)
0=OK  1=Suspect
System ID
0=PRIMARY, 1=SECONDARY
Actual integration period (# major frames)
1, 2, 4
Nominal integration period (# major frames)
1, 2, 4, 5, 6
Image number
1,2
# images every 4 major frames
1,2
# detector rows per line readout
1,2,3


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PO_H3_PWI
Description
Effective Bandwidth is 1.5*delta_f, where delta_f depends on the size of the FFT used to convert to
the frequency domain, and delta_t.


Modification History
Created Oct 1999


Variable Notes

Time, time between points
Determined by Filter Mode
Numper of Spectra of FFT_size in this file 
This is the number of Gain/Epoch0 Records
HFWR B Gain (all components, ~2 sec res) 
Applies to all 3 Magnetic Channels


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PO_H3_UVI
Description
Primary UVI team data products


Modification History
Initial work at SPDF 3/20-x/xx/2001 by REM


Variable Notes

Data quality suspect flag (0=OK,1=Suspect)
0=OK  1=Suspect
System ID
0=PRIMARY, 1=SECONDARY
Actual integration period (# major frames)
1, 2, 4
Nominal integration period (# major frames)
1, 2, 4, 5, 6
Image number
1,2
# images every 4 major frames
1,2
# detector rows per line readout
1,2,3


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PO_H4_PWI
Description
Reference:..Gurnett, D.A. et al, The Polar plasma wave instrument, Space Science Reviews, Vol. 71,
pp. 597-622, 1995.  donald-gurnett@.uiowa.edu
An FFT on 2048 values was used in calibrating the data; i.e., perform FFT, calibrate in frequency
domain, perform inverse FFT to get calibrated time series.
Data are lowpass filtered so that the data are valid only up to 2 kHz.
The three orthogonal magnetic field components are given in units of nT/Sec rather than nT because
the response of the searchcoils across the passband is not flat.  In order to obtain units of nT,
the data would need to be digitally filtered to the frequency of interest and then integrated over
time.  Integrating over the entire passband could possibly destroy the resolution of the higher
frequency components since the low frequency noise, if present, will dominate.
Effective Bandwidth is 1.5*delta_f, where delta_f depends on the size of the FFT used to convert to
the frequency domain, and delta_t.


Modification History
Created Oct 1999


Variable Notes

Time, time between points
Data are not continuous.  57-msec snapshotsare taken every 128.8 seconds
Number of Spectra of FFT_size in this file 
This is the number of Gain/Epoch0 Records
M Gain (HFWR 2 kHz, ~2 sec res) 
Applies to all 3 Magnetic Channels


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PO_K0_CAM
Description
This data set contains 96-second averaged counting rates for H+, He++, (O+, O++ together), (O>2+),
all from the MICS part of the instrument, with a +/- 1 degree field of view perpendicular to the
spin axis, segmented into bins of size 1/32 of a spin.
T.A. Fritz et.al, CAMMICE:The POLAR CAMMICE instruments
It also contains 96-second averaged counting rates from two proton channels (0.5-1.7 MeV and 1.7-5.8
MeV), two He channels (1.4-4.3 MeV and 4.3-9.6 MeV), and six CNO channels (5-10, 6-11, 7-13, 17-92,
18-92, 21-92 MeV), from the HIT part of the instrument, with a +/- 6 degree field of view
perpendicular to the spin axis, segmented into bins  
of 1/32 of a spin.
A. Fritz et.al, CAMMICE:The POLAR CAMMICE instruments


Modification History
This is the 1st version, generated on 17 November 1995.




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PO_K0_CEP
Description
Data: 96 second averages
J. B. Blake et.al, Comprehensive Energetic Particle & Pitch Angle Distribution




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PO_K0_EFI
Description
Reference: DATA FORMAT CONTROL DOCUMENT (DFCD) BETWEEN THE 
INTERNATIONAL SOLAR-TERRESTRIAL PHYSICS (ISTP) PROGRAM 
INFORMATION PROCESSING DIVISION (IPD) GROUND DATA PROCESSING 
SYSTEM AND THE ISTP MISSION INVESTIGATORS SEPTEMBER 1993 Pages 3-57 through 3-60.
GGS Instrument papers (DRAFT)December 1992 pages B.2.1 thru B.2.14 inclusive.
The Polar Electric Field Instrument KPS will record data from two sets of Langmuir probes.
The first set V12, are 130m apart, the second set V34, are 100m apart.


Modification History
Avoid B algorithm was added to the ground spinfits calculations in version 4.0.
Version 4.1: Update of Berkeley Modules.


Variable Notes

E-Field in xy plane, Scalar
ground spinfits calculations with avoid B
E-Field in z plane, Scalar
ground spinfits calculations with avoid B
E-Field Sigma, Scalar
ground spinfits calculations with avoid B


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PO_K0_HYD
Description
Reference: HYDRA is a 3-Dimensional Electron and Ion Hot  plasma Instrument for the Polar Spacecraft
of the GGS Mission, J. Scudder et al., Space Sci. Rev., 71, 459-495, Feb. 1995.
This data set contains the electron density and average energy, and the maximum and minimum Debye
energies, at 1-minute resolution.
J. Scudder, et.al, Space Sci. Rev., 71, 459-495, 1995, http://www-st.physics.uiowa.edu 
J. Scudder, et.al, Space Sci. Rev., 71, 459-495, 1995, http://www-st.physics.uiowa.edu


Modification History
Created Feb. 10, 1997
3/23/97: Corrected attribute errors


Variable Notes

Post Gap Flag: 0=no gap, other=gap
Gap Flag: 0=no gap; 1=instrument mode; 2=lz data not available; 4=generic lz
read error; 8=manuever mode; 16=No EFI data avail/PSI off or unknown; 32=burst
mode
Data Quality Flag: -1=good, 1=better, 0=best
Data Quality Flag: -1 = EFI SC Pot. used/PSI unknown; 0 = EFI SC Pot. used/PSI
off; 1 = 1 Volt SC Pot. used/PSI on


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PO_K0_MFE
Description
Data: 0.92 minute and6 second averages


Modification History
version 1.0 Jan 93 Test. Modified by JT on Nov. 30, 1995Modified by XL on Feb. 18, 1997




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PO_K0_PIX
Description
INSTRUMENT DESCRIPTION:              
The PIXIE instrument remotely images 
bremsstrahlung X-rays which are 
emitted from the earth's atmosphere. 
PIXIE measures the bremsstrahlung 
X-ray flux in two spatial dimensions 
and as a function of energy from 
2 keV to 60 keV in 64 energy 
channels.  The spatial 
resolution and sensitivity of the 
instrument are a function of orbital 
altitude.  Sensitivity is optimized 
by the use of a variable 
configuration of the instrument's 
adjustable aperture plate.    
Continuous imagery will be provided, 
since PIXIE is mounted on the 
despun platform.  Each X-ray photon 
is identified individually by the 
time and location at which it is 
detected within the focal plane.
 
INSTRUMENT REFERENCES:               
1.  Instrument Description Document 
for the Polar Ionospheric X-ray 
Imaging Experiment (PIXIE) on the 
ISTP/GGS POLAR Satellite (submitted 
to Project as a PIXIE deliverable). 
Document number LMSC F254274 
(Lockheed Space and Missiles Co.) 
                                  
2.  McKenzie, D. L., D. J. Gorney, 
and W. L. Imhof, Auroral X-ray 
Imaging from High- and Low-Earth 
Orbit, Proc. SPIE, 1745, 39, 1992. 
                                  
3.  McKenzie, D. L., D. J. Gorney, 
and W. L. Imhof, Auroral X-ray 
Imaging from High- and Low-Earth 
Orbit, Opt. Eng. (to be published in 
the February 1994 issue). 
                                  
4.  Imhof, W. L., et al., The Polar 
Ionospheric X-ray Imaging Experiment 
(PIXIE), Space Science Reviews (to 
be published as part of a special 
issue on the GGS instruments). 
KEY PARAMETERS DESCRIPTION:          
The Primary Key Parameter data 
consists of two 64x64 pixel X-ray 
image arrays and two Mean Intensity 
measures. The images and intensities 
are associated with two variable 
integrated energy channel ranges.  
The Secondary Key Parameter data 
contains information necessary to 
the appropriate interpretation of 
the images.  This information 
includes geographic and geomagnetic 
spatial registration references, 
integrated energy range definitions, 
data quality flags, and various 
mode/state indicators.  The spatial 
references include full pixel maps 
(providing the value of a particular 
coordinate, e.g., magnetic latitude, 
at each of the 4096 pixels) as well 
as simple pixel markers locating 
specific features (such as the 
geographic and geomagnetic poles).


Modification History
Unified image array has been split
into high & low energy image arrays.
VAR_NOTES attribute entries have
been included to supplement CATDESC
entries where appropriate.


Variable Notes

Indicates cause of large data gap
0=no gap, 1=instrument mode, 2=LZ missing, 3=LZ noisy, 4=telemetry mode
Indicates condition of KP data (0=good)
0=Good, 1=Questionable, 2=Poor, 99=No data
Low Energy X-ray Source Array, 64x64 image
Intensity of photons detected in the energyrange specified by the first array
elementof variable ENERGY_RANGE and its associated delta values
--> Low Energy X-ray Source Array with geographic map overlay
Intensity of photons detected in the energyrange specified by the first array
elementof variable ENERGY_RANGE and its associated delta values
[DO NOT USE: UNDER-DEVELOPMENT] --> Test Display 
Intensity of photons detected in the energyrange specified by the first array
elementof variable ENERGY_RANGE and its associated delta values
--> Low Energy X-ray Source Array, azimuthal projection to geographic coordinates
Intensity of photons detected in the energyrange specified by the first array
elementof variable ENERGY_RANGE and its associated delta values
--> Low Energy X-ray Source Array, azimuthal projection to magnetic local time and invariant latitude
Intensity of photons detected in the energyrange specified by the first array
elementof variable ENERGY_RANGE and its associated delta values
Low Energy X-ray Source Array, 64x64 mpeg movie image
Intensity of photons detected in the energyrange specified by the first array
elementof variable ENERGY_RANGE and its associated delta values
--> Low Energy X-ray Source Array with geographic map overlay
Intensity of photons detected in the energyrange specified by the first array
elementof variable ENERGY_RANGE and its associated delta values
--> Low Energy X-ray Source Array, azimuthal projection to geographic coordinates
Intensity of photons detected in the energyrange specified by the first array
elementof variable ENERGY_RANGE and its associated delta values
--> Low Energy X-ray Source Array, azimuthal projection to magnetic local time and invariant latitude
Intensity of photons detected in the energyrange specified by the first array
elementof variable ENERGY_RANGE and its associated delta values
64x64 X-ray Source Array for high energy range
Represents photons detected in the energyrange specified by the second array
elementof variable ENERGY_RANGE and its associated delta values
--> High Energy X-ray Source Array with geographic map overlay
Represents photons detected in the energyrange specified by the second array
elementof variable ENERGY_RANGE and its associated delta values
[DO NOT USE: UNDER-DEVELOPMENT] --> Test Display 
Represents photons detected in the energyrange specified by the second array
elementof variable ENERGY_RANGE and its associated delta values
--> High Energy X-ray Source Array, azimuthal projection to geographic coordinates (fixed-sun orientation)
Represents photons detected in the energyrange specified by the second array
elementof variable ENERGY_RANGE and its associated delta values
--> High Energy X-ray Source Array, azimuthal projection to magnetic local time and invariant latitude
Represents photons detected in the energyrange specified by the second array
elementof variable ENERGY_RANGE and its associated delta values
64x64 X-ray Source Array for high energy range, mpeg movie image.
Represents photons detected in the energyrange specified by the second array
elementof variable ENERGY_RANGE and its associated delta values
--> High Energy X-ray Source Array with geographic map overlay
Represents photons detected in the energyrange specified by the second array
elementof variable ENERGY_RANGE and its associated delta values
--> High Energy X-ray Source Array, azimuthal projection to geographic coordinates (fixed-sun orientation)
Represents photons detected in the energyrange specified by the second array
elementof variable ENERGY_RANGE and its associated delta values
--> High Energy X-ray Source Array, azimuthal projection to magnetic local time and invariant latitude
Represents photons detected in the energyrange specified by the second array
elementof variable ENERGY_RANGE and its associated delta values
Character string identifying special campaign
If no campaign in effect, value will be NONE
Number of A/B sub-images employed to produce the KP composite image
Values are encoded with first digitbeing the number of Plate A sub-images,
second digit being the number ofPlate B images
A/B Camera aperture sizes employed to accumulate photon events
Values are encoded with first four digitsbeing the Plate A aperture size,
secondfour digits being the Plate B aperture size(in units of microns)
Indicates processing status for current record
0=Nominal, 1=Event count below threshold, 2=Instrument condition not nominal,
10=Secondary KPs incomplete, 99=No data


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PO_K0_PWI
Description
Reference:..Gurnett, D.A. et al, The Polar plasma wave instrument, Space Science Reviews, Vol. 71,
pp. 597-622, 1995.GURNETT@IOWAVE.physics.uiowa.edu
Note:..The electron ion and cyclotron frequencies are derived from the following:  Fce = 0.028
kHz*B, where B is the magnitude of the ambient magnetic field measured in nT.  Fcp = Fce/1837 in
kHz.  FcO+ = Fcp/16 in kHz.  All frequencies in the key parameters are converted to Hz.
Since the SFR frequency steps vary with the mode, the measured SFR frequencies will be mapped to a
fixed array of 160 approximately logarithmically spaced frequency values, 32 frequency values for
each of the five SFR channels.  In the log mode, the 64 frequency steps of the fourth and fifth
frequency channels will be mapped to 32 frequency steps each, using geometric averaging.  In the
linear mode, the 448 linearly spaced frequency steps of the five frequency channels will be mapped
to the fixed array of 160 logarithmically spaced frequency values using a windowing technique.  The
magnetic and electric field values corresponding to each SFR frequency step will be similarly mapped
to 160-point fixed arrays corresponding to the mapped frequency array.


Modification History
Created Sept 1992, modified by JT 2/15/96




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PO_K0_SPHA
Description
To be supplied


Modification History
6/4/93 - Original Implementation
6/8/94 - CCR ISTP 1852, updated CDHF skeleton to CDF standards - JT
11/10/94 - Correct errors made in ccr 1852.  ICCR 1884




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PO_K0_TID
Description
Moore et al., The Thermal Ion Dynamics Experiment and Plasma Source Instrument, Space Sci Rev., 71,
409-458, 1995.
Key parameters for dates 28-Mar-1996 to 15-Sep-1996 are mass resolved. Key parameters between
15-Sep-1996 and 09-Dec-1996 are not valid. Key parameters after 09-Dec-1996 are non-mass total ion
contribution below 300 eV.
Key parameters for dates 28-Mar-1996 to 15-Sep-1996 are mass resolved. Key parameters between
15-Sep-1996 and 09-Dec-1996 are not valid. Key parameters after 09-Dec-1996 are non-mass total ion
contribution below 300 eV.
The following parameters are available before 15-Sep-1996: ion density, plasma velocity (GSE),
parallel and perpendicular temperatures, and density of ion noice mask, all for each of the ions H+,
He+, and O+.
The following parameters are available before 15-Sep-1996: ion density, plasma velocity (GSE),
parallel and perpendicular temperatures, and density of ion noice mask, all for each of the ions H+,
He+, and O+.
The following parameters are available only after 09-Dec-1996:  total ion density, total plasma
velocity (GSE), total ion parallel and perpendicular temperatures, and density of total ion noise
mask.
The following parameters are available only after 09-Dec-1996:  total ion density, total plasma
velocity (GSE), total ion parallel and perpendicular temperatures, and density of total ion noise
mask.


Modification History
Created Jul 9, 1997.


Variable Notes

Instrument mode code.
Instrument mode code value is the sum of: 0: TIDE off +200: TIDE on +0: PSI off
+400: PSI on +n: most closed mirror setting times 10: n = 0 = mirror fully
opened, n = 150 = mirror completely closed.


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PO_K0_TIM
Description
 Data: 1 minute average densities, velocities, and temperatures for H+, O+, He++ and He+ ions. 
Averages taken over various energy ranges in a coordinate system approximately aligned with the 1 
minute average magnetic field direction.
These data are Key Parameters for event identification and initial data analysis purposes. 
The codes used to generate these parameters were developed prior to launch and do not reflect
operational experience. 
Reference:
E.G. Shelley et al., The Toroidal Imaging Mass-Angle Spectrograph (TIMAS) for the Polar Mission, Sp.
Sci. Rev, Vol 71, pp 497-530, 1995.
The instrumental energy range is subject to change a few times per orbit. 
Energy_Range_ID indicates which of the 3 instrumental energy ranges is currently active. 
Each instrumental energy range further divided into 3 Key Parameter (KP) energy channels (low -
medium - and high). 
The table below gives the full energy range and limits of the thee KP energy ranges.
Energy_Range_ID=0: (Full instrumental energy range)Full range (0.015 - 33.3 keV/e)low E channel
(0.015 - 0.37 keV/e)mid E channel (0.37 - 3.3 keV/e)high E channel (3.3 - 33.3 keV/e)
Energy_Range_ID=1: (Reduced instrumental energy range)Full range (0.015 - 22.45 keV/e)low E channel
(0.015 - 0.37 keV/e)mid E channel (0.37 - 3.3 keV/e)high E channel (3.3 - 22.45 keV/e)
Energy_Range_ID=2: (Low instrumental energy range)Full range (0.015 - 2.18 keV/e)low E channel
(0.015 - 0.11 keV/e)mid E channel (0.11 - 0.37 keV/e)high E channel (0.37 - 2.18 keV/e)



Metadata provided by W.K. Peterson


Modification History
Version 0 September 1995
Text_supplement_2 added  10/9/95.
TEXT and VAR_NOTES now include discussions of the energy ranges 12/15/95


Variable Notes

NSSDC standard-reference time value. 
Center time of 60 second accumulation intervals, starting at 0 seconds of each
UT day.
Time PB5, centered
Center time of 60 second accumulation intervals, starting at 0 seconds of each
UT day
Partial H+ number density for 3 VARIABLE energy ranges.
Negative values reflect low counting rates and background subtraction. The width
of the energy channels is mode dependent. There are 3 instrumental energy ranges
identified by Energy_Range_ID, one of which is active.  Each instrumental energy
range is further divided into 3 Key Parameter (KP) energy channels (low - medium
- and high). The table below gives the full energy range and limits of the thee
KP energy ranges. Energy_Range_ID=0: (Full instrumental energy range)Full range
(0.015 - 33.3 keV/e)low E channel (0.015 - 0.37 keV/e)mid E channel (0.37 - 3.3
keV/e)high E channel (3.3 - 33.3 keV/e)Energy_Range_ID=1: (Reduced instrumental
energy range)Full range (0.015 - 22.45 keV/e)low E channel (0.015 - 0.37
keV/e)mid E channel (0.37 - 3.3 keV/e)high E channel (3.3 - 22.45
keV/e)Energy_Range_ID=2: (Low instrumental energy range)Full range (0.015 - 2.18
keV/e)low E channel (0.015 - 0.11 keV/e)mid E channel (0.11 - 0.37 keV/e)high E
channel (0.37 - 2.18 keV/e)
Partial O+ number density for 3 variable energy ranges.
Negative values reflect low counting rates and background subtraction. The width
of the energy channels is mode dependent. There are 3 instrumental energy ranges
identified by Energy_Range_ID, one of which is active.  Each instrumental energy
range is further divided into 3 Key Parameter (KP) energy channels (low - medium
- and high). The table below gives the full energy range and limits of the thee
KP energy ranges.Energy_Range_ID=0: (Full instrumental energy range)Full range
(0.015 - 33.3 keV/e)low E channel (0.015 - 0.37 keV/e)mid E channel (0.37 - 3.3
keV/e)high E channel (3.3 - 33.3 keV/e)Energy_Range_ID=1: (Reduced instrumental
energy range)Full range (0.015 - 22.45 keV/e)low E channel (0.015 - 0.37
keV/e)mid E channel (0.37 - 3.3 keV/e)high E channel (3.3 - 22.45
keV/e)Energy_Range_ID=2: (Low instrumental energy range)Full range (0.015 - 2.18
keV/e)low E channel (0.015 - 0.11 keV/e)mid E channel (0.11 - 0.37 keV/e)high E
channel (0.37 - 2.18 keV/e)
Partial He+ number density for the full active energy range.
Negative values reflect low counting rates and background subtraction. There are
3 instrumental energy ranges identified by Energy_Range_ID, one of which is
active.  The table below gives the full energy range for each possible value of
the Energy_Range_ID variable.  Energy_Range_ID=0: (Full instrumental energy
range) (0.015 - 33.3 keV/e)Energy_Range_ID=1: (Reduced instrumental energy
range)(0.015 - 22.45 keV/e)Energy_Range_ID=2: (Low instrumental energy
range)(0.015 - 2.18 keV/e).
Partial He++ number density for the full active energy range.
Negative values reflect low counting rates and background subtraction. There are
3 instrumental energy ranges identified by Energy_Range_ID, one of which is
active.  The table below gives the full energy range for each possible value of
the Energy_Range_ID variable.  Energy_Range_ID=0: (Full instrumental energy
range) (0.015 - 33.3 keV/e)Energy_Range_ID=1: (Reduced instrumental energy
range)(0.015 - 22.45 keV/e)Energy_Range_ID=2: (Low instrumental energy
range)(0.015 - 2.18 keV/e).
H+ velocity from the active low energy range in field aligned Coordinates.
Vel_H_low variables are derived by integrating over an energy range that depends
on the the value of the Energy_Range_ID variable.  For Energy_Range_ID =0 and 1,
the energy range is from 0.15 to 0.37 ,keV/e.  For Energy_Range_ID=2, the energy
range is 0.15 to 0.11 keV/e. Velocities are reported in a coordinate system with
the X axis aligned with the one minute average magnetic field direction
(TIMAS_B).  In this coordinate system the Y axis is in the spacecraft spin
plane, and the Z axis completes a right hand system.
O+ velocity from the variable low energy range in field aligned Coordinates. 
Vel_O_low variables are derived by integrating over an energy range that depends
on the the value of the Energy_Range_ID variable.  For Energy_Range_ID =0 and 1
,the energy range is from 0.15 to 0.37  ,keV/e.  For Energy_Range_ID=2, the
energy range is 0.15 to 0.11 keV/e. Velocities are reported in a coordinate
system with the X axis aligned with the one minute average magnetic field
direction (TIMAS_B).  In this coordinate system the Y axis is in the spacecraft
spin plane, and the Z axis completes a right hand system.
H+ velocity from the variable full energy range in field aligned Coordinates.
Velocity_H variables are derived by integrating over an energy range that
depends on the the value of the Energy_Range_ID variable.  For Energy_Range_ID
=0 the energy ranges is from 0.015 to 33.3 keV/e.  For Energy_Range_ID =1 0.015
to 22.45 keV/e.  For Energy_Range_ID=2 0.015 to 2.18 keV/e. Velocities are
reported in a coordinate system with the X axis aligned with the one minute
average magnetic field direction (TIMAS_B).  In this coordinate system the Y
axis is in the spacecraft spin plane, and the Z axis completes a right hand
system.
O+ velocity from the variable full energy range in field aligned Coordinates.
Velocity_O variables are derived by integrating over an energy range that
depends on the the value of the Energy_Range_ID variable.  For Energy_Range_ID
=0 the energy ranges is from 0.015 to 33.3 keV/e.  For Energy_Range_ID =1 0.015
to 22.45 keV/e.  For Energy_Range_ID=2 0.015 to 2.18 keV/e. Velocities are
reported in a coordinate system with the X axis aligned with the one minute
average magnetic field direction (TIMAS_B).  In this coordinate system the Y
axis is in the spacecraft spin plane, and the Z axis completes a right hand
system.
H+ Temperature from the variable low energy range in field aligned coordinates.
H+ Temperature perpendicular and parallel to the one minute average magnetic
field direction  for the low KP energy range.  Temp_H_low variables are derived
by integrating over an energy range that depends on the the value of the
Energy_Range_ID variable.  For Energy_Range_ID =0 and 1 ,the energy range is
from 0.15 to 0.37  ,keV/e.  For Energy_Range_ID=2, the energy range is 0.15 to
0.11 keV/e. Temperatures are reported in a coordinate system with the X axis
aligned with the one minute average magnetic field direction (TIMAS_B).  In this
coordinate system.
O+ Temperature from the variable low energy range in field aligned coordinates.
O+ Temperature perpendicular and parallel to the one minute average magnetic
field direction  for the low KP energy range.  Temp_H_low variables are derived
by integrating over an energy range that depends on the the value of the
Energy_Range_ID variable.  For Energy_Range_ID =0 and 1, the energy range is
from 0.15 to 0.37, keV/e.  For Energy_Range_ID=2, the energy range is 0.15 to
0.11 keV/e. Temperatures are reported in a coordinate system with the X axis
aligned with the one minute average magnetic field direction (TIMAS_B).  In this
coordinate system.
H+ Temperature from the variable full energy range in field aligned coordinates.
H+ Temperature perpendicular and parallel to the one minute average magnetic
field direction (TIMAS_B). for the full instrumental energy range. 
Temperature_x variables are derived by integrating over an energy range that
depends on the the value of the Energy_Range_ID variable.  For Energy_Range_ID
=0, the energy range is from 0.15 to 33.3 keV/e. For Energy_Range_ID =1 the
range, is 0.15 to 22.45 keV/e.  For  Energy_Range_ID=2, the energy range is 0.15
to 2.18 keV/e. Temperatures are reported in a coordinate system with the X axis
aligned with the one minute average magnetic field direction (TIMAS_B).
O+ Temperature from the variable full energy range in field aligned coordinates.
O+ Temperature perpendicular and parallel to the one minute average magnetic
field direction (TIMAS_B). for the full instrumental energy range. 
Temperature_x variables are derived by integrating over an energy range that
depends on the the value of the Energy_Range_ID variable.  For Energy_Range_ID
=0, the energy range is from 0.15 to 33.3, keV/e. For Energy_Range_ID =1 the
range, is 0.15 to 22.45 keV/e.  For  Energy_Range_ID=2, the energy range is 0.15
to 2.18 keV/e. Temperatures are reported in a coordinate system with the X axis
aligned with the one minute average magnetic field direction (TIMAS_B).
Mode Identification Number
IDENTIFICATION NUMBER of the TIMAS ICP Table active at the start of the one
minute averaging period.
Energy Range Identification: 0: Full energy range; 1: Reduced energy range; 2: Low energy range
TIMAS is operated in one of 3  energy ranges. Energy_Range_ID indicates which of
the 3 instrumental energy ranges is currently active. Each instrumental energy
range further divided into 3 Key Parameter (KP) energy channels (low - medium -
and high). The table below gives the full energy range and limits of the thee KP
energy ranges.Energy_Range_ID=0: (Full instrumental energy range)Full range
(0.015 - 33.3 keV/e)low E channel (0.015 - 0.37 keV/e)mid E channel (0.37 - 3.3
keV/e)high E channel (3.3 - 33.3 keV/e)Energy_Range_ID=1: (Reduced instrumental
energy range)Full range (0.015 - 22.45 keV/e)low E channel (0.015 - 0.37
keV/e)mid E channel (0.37 - 3.3 keV/e)high E channel (3.3 - 22.45
keV/e)Energy_Range_ID=2: (Low instrumental energy range)Full range (0.015 - 2.18
keV/e)low E channel (0.015 - 0.11 keV/e)mid E channel (0.11 - 0.37 keV/e)high E
channel (0.37 - 2.18 keV/e)
Magnetic Field From 9.2 second average Level 0 data records.
Average Magnetic Field in Fixed-Payload (FP) coordinates.  (Z parallel to spin
axis, X perpendicular to Z and in the same meridian plane containing the radius
vector to the sun, Y completes a right hand system.  The velocity  variables
here are reported in field aligned coordinates--a coordinate system that has the
X component of velocity parallel to the TIMAS_B vector. The rotation from
Fixed-Payload to field aligned coordinates is done by first rotating about the Z
(spin axis) and then about the TIMAS_B Y axis until the TIMAS_X axis is aligned
with the magnetic field direction. The temperature variables are reported in
components perpendicular and  parallel to the TIMAS_B direction. NOTE: TIMAS_B
is a diagnostic parameter. It is not intended for general data analysis. Use the
Magnetometer (MFE) Key Parameters for data analysis.
Modified H+ signal to background ratio.
Set to the ratio of the density calculated using raw counts uncorrected for
background to the same sums using only count rates from a separate background
monitor. The ratio is set to Zero if no data for the relevant energy/mass range
or background are available. The ratio is set to 999 if the measured background
is zero.
Modified O+ signal to background ratio.
Set to the ratio of the density calculated using raw counts uncorrected for
background to the same sums using only count rates from a separate background
monitor. The ratio is set to Zero if no data for the relevant energy/mass range
or background are available. The ratio is set to 999 if the measured background
is zero.
Modified He+ signal to background ratio.
Set to the ratio of the density calculated using raw counts uncorrected for
background to the same sums using only count rates from a separate background
monitor. The ratio is set to Zero if no data for the relevant energy/mass range
or background are available. The ratio is set to 999 if the measured background
is zero.
Modified He++ signal to background ratio.
Set to the ratio of the density calculated using raw counts uncorrected for
background to the same sums using only count rates from a separate background
monitor. The ratio is set to Zero if no data for the relevant energy/mass range
or background are available. The ratio is set to 999 if the measured background
is zero.
Invariant Latitude, Magnetic local time, and Geomagnetic latitude in a 3 element vector. 
Invariant Latitude, Geomagnetic Local time and Geomagnetic Latitude.
Time axis label: Invariant Latitude, Magnetic local time, and Geomagnetic latitude in a 3 element vector. 
Invariant Latitude, Geomagnetic Local time and Geomagnetic Latitude.
Sub-satellite Latitude longitude and geocentric distance. 
r/Re is the geocentric distance expressed in units of Earth radii (6367 km)
Sub-satellite Latitude longitude and geocentric distance. 
r/Re is the geocentric distance expressed in units of Earth radii (6367 km)
Labels for 3 KP energy ranges. 
The KP high Energy Range limit is set by the Instrumental Energy Mode, which is
indicated by the Energy_Range_ID.


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PO_K0_UVI
Description
References --------------------
1. M. R. Torr, et al., A far ultraviolet imager for the International Solar-Terrestrial Physics
mission, Space Sci. Rev., v71, pp329 - 383, 1995
Notes ------------------------ 
1. The UVI field of view is circular with an 8 degree full width.  The circular image is stored in
IMAGE_DATA as a rectangular array of 228 rows and 200 columns.
2.  Time information is contained in EPOCH, Time_PB5, IMG_MINUS_MSEC, and IMG_PLUS_MSEC.  
3. Pointing information is given in GCI_LOOK_DIR, GEODETIC_LAT, and GEODETIC_LONG.


Modification History
v1.0 Initial Prelaunch Release 10/16/95 
v1.0 Interim Prelaunch Release 
5/8/96 Added KPGS_VERSION
3/9/97 Changed min/max valuesfor IMAGE_DATA


Variable Notes

Image time.
The time in EPOCH and Time_PB5 refer to the center of the image in IMAGE_DATA.
There is an offset of up to 8 major frames between the beginning of the image
exposure and the ATC telemetry time stamp.  The times shown here are corrected
for this and describe the actual time of exposure.
Image time.
The time in EPOCH and Time_PB5 refer to the center of the image in IMAGE_DATA. 
There is an offset of up to 8 major frames between the beginning of the image
exposure and the ATC telemetry time stamp.  The times shown here are corrected
for this and describe the actual time of exposure.
The start of the image, measured from EPOCH/Time_PB5.
The beginning and ending time of the image is specified in msec relative to the
time in EPOCH and Time_PB5 by IMG_MINUS_MSEC and IMG_PLUS_MSEC, respectively.
The end of the image, measured from EPOCH/Time_PB5.
The beginning and ending time of the image is specified in msec relative to the
time in EPOCH and Time_PB5 by IMG_MINUS_MSEC and IMG_PLUS_MSEC, respectively.
Explanation of preceding gap.
A gap is defined if the time between records is greater than twice the nominal
output time (NOMINAL_OUTPUT_PERIOD).  The following values are defined for
POST_GAP_FLAG: O = No Gap; 1 = Wrong Mode; 2 = Missing Data; 3 = Noisy Data; 4-9
= undefined; 10 = High voltage not enabled; 11 = gain set to zero; 12 =The first
minor frame containing UVI housekeeping was zero filled 13 = Unable to sync with
telemetry stream; 14 = No background images were present; 15 = Requested filter
setting was not present; 16 = Spacecraft was near perigee pass where no kp's are
generated; 17 = Despun platform was pointing away from the earth; 18 = Image
data lay outside requested process window (Not used for production); 19 =
Unknown. Note that long gaps may be caused by multiple events.  POST_GAP_FLAG
attempts to represent the most severe event contributing to the gap. Also, since
each image frame requires a minimum of 4 major frames (36.8 s) very short values
of NOMINAL_OUTPUT_PERIOD on the order of 1 minute may always encounter a gap
since the desired images may be several minutes apart.  This condition is not
trapped and will result in an unknown value for the post gap flag.
Quality indicator (also quickly shows times when images are available)
QUALITY_FLAG is a  bit-mapped flag in which each bit corresponds to a single
quality condition.  The most  significant bit (minus sign) is not used. 
Consequently up to 31 different quality conditions can be simultaneously
flagged.  The flags are ordered in severity with increasing bit position.  The
following _hexadecimal_ values have been defined  for QUALITY_FLAG: 0 = No
errors or quality conditions;  1 = an error occurred writing an SFDU comment; 2
=  image time was outside of selected processing window; 4 = some level zero
minor frames had fill values;  8 = some level zero minor frames had sync errors;
10 = the image single frame integration period could not be determined due to
bad telemetry (assumed to be 4 major frames);  20 = the despun platform was in
motion or had not settled down from a motion;   40 = the pointing calculations
have not been validated or may be unreliable;  80 = the time flags for this
image may be unreliable; 100 = there was an error decode star mode data; 200
=some major frames were missing but an image could be partially  reconstructed; 
400 = calibration data is missing or otherwise invalid;  800 = a background
image could not be found; 1000 = the  requested output image could not be found.
KPGS sw version.
Incremented with each update.
Nominal time between output records.
This is the nominal time between output records.  The actual output spacing will
vary depending on the nature of the observing sequences being run.
Operating system.
UVI has two independent systems. PRIMARY: +1, SECONDARY: -1
Instrument operating mode.
(1=Normal, 2=Star, 3=Idle) Normal mode produces one 200 x 228 image every 4
major frames.  Star mode produces multiple miniframe images every major frame. 
Idle mode produces no image output.
Detector gain setting
0=off, 16=highest sensitivity
Aperture door position
(OPEN: +1, CLOSED: -1) MgF2 window in door allows viewing when closed.
Far UV Images (kRay), small format display with click-expand (~10 min res)
The UVI field of view is circular with an 8 degree full width.  The circular
image is stored in IMAGE_DATA as a rectangular array of 228 rows and 200
columns.  Consequently, the corners of each image contain non-image data.  The
non-active corner pixel locations are identified by a corner fill value = -128. 
The image is oriented such that the direction of decreasing row number points
along the spacecraft spin axis.  The direction of decreasing column number
points to the outboard direction (relative to the spin axis).  The orientation
is the same for both detectors.
--> (USE SHORT TIME SPANS) Large format display with click-expand, no geographic registration
The UVI field of view is circular with an 8 degree full width.  The circular
image is stored in IMAGE_DATA as a rectangular array of 228 rows and 200
columns.  Consequently, the corners of each image contain non-image data.  The
non-active corner pixel locations are identified by a corner fill value = -128. 
The image is oriented such that the direction of decreasing row number points
along the spacecraft spin axis.  The direction of decreasing column number
points to the outboard direction (relative to the spin axis).  The orientation
is the same for both detectors.
Geodetic latitude for IMAGE_DATA (23 x 20 pixels)
Sparse matrices (every 10 pixels) of latitude and longitude are given in
GEODETIC_LAT and GEODETIC_LONG, respectively.  Latitude & longitude are given in
geodetic coordinates (determined from the normal to the assumed surface of the
earth [assumed to be an ellipsoid of revolution]) and not in geocentric
coordinates (determined relative to the center of the earth).
Geodetic longitude for IMAGE_DATA (23 x 20 pixels)
Sparse matrices (every 10 pixels) of latitude and longitude are given in
GEODETIC_LAT and GEODETIC_LONG, respectively.  Latitude & longitude are given in
geodetic coordinates (determined from the normal to the assumed surface of the
earth [assumed to be an ellipsoid of revolution]) and not in geocentric
coordinates (determined relative to the center of the earth).
Image registered geodetic latitude
This is a virtual variable computed in read_myCDF. Calling conv_map_image w/ the
component variables results in the image registered latitudes.
Image registered geodetic longitude
This is a virtual variable computed in read_myCDF. Calling conv_map_image w/ the
component variables results in the image registered longitudes.
--> (USE SHORT TIME SPANS) With geographic map overlay
This is a virtual variable computed in read_myCDF
--> [DO NOT USE: UNDER-DEVELOPMENT] Test Display
This is a virtual variable computed in read_myCDF
--> (USE SHORT TIME SPANS) Azimuthal projection to geographic (with fixed sun orientation)
This is a virtual variable computed in read_myCDF. Calling conv_map_image
--> (USE SHORT TIME SPANS) Azimuthal projection to magnetic LT and invariant lat
This is a virtual variable computed in read_myCDF. MLT map generated in
plot_map_images.pro
--> (USE SHORT TIME SPANS) Movie display of images, no geographic registration
This is a virtual variable computed in read_myCDF
--> (USE SHORT TIME SPANS) Movie, with geographic map overlay
This is a virtual variable computed in read_myCDF
--> (USE SHORT TIME SPANS) Movie, azimuthal projection to geographic (with fixed sun orientation)
This is a virtual variable computed in read_myCDF. Calling conv_map_image
--> (USE SHORT TIME SPAN) Movie, azimuthal projection to magnetic LT and invariant lat
This is a virtual variable computed in read_myCDF. MLT map generated in
plot_map_images.pro
Spacecraft Position in GCI, 3 comp.
Copied from S/C orbit file.
Spacecraft Attitude in GCI, 3 comp.
Calculated from S/C attitude file.
Sun Position in GCI, 3 comp.
Vector pointing to sun.
Unit vector along field of view.
GCI_LOOK_DIR is a unit vector in GCI coordinates pointing from the spacecraft
along the center of the UVI line of sight.  An external utility can be used to
calculate latitude and longitude for any pixel of the UVI image.The pointing
utility can be found on the UVI WWW home page (URL: TBD)
Offset angle of despun platform from nadir. 
Positive in direction opposite of spacecraft rotation.
Filter selection.
1304=2, 1356=3, LBHS=4, LBHL=5, SOLR=6


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PO_K0_VIS
Description
 Instrument functional description:
    The VIS is a set of three low-light-level cameras.  Two of these
    cameras share primary and some secondary optics and are designed to
    provide images of the nighttime auroral oval at visible wavelengths.
    A third camera is used to monitor the directions of the fields-of-view
    of the auroral cameras with respect to the sunlit Earth and return
    global images of the auroral oval at ultraviolet wavelengths.  The
    VIS instrumentation produces an auroral image of 256 x 256 pixels
    approximately every 24 seconds dependent on the integration time and
    filter selected.  The fields-of-view of the two nighttime auroral
    cameras are 5.6 x 6.3 degrees and 2.8 x 3.3 degrees for the low and
    medium resolution cameras, respectively.  One or more Earth camera
    images of 256 x 256 pixels are produced every five minutes, depending
    on the commanded mode.  The field-of-view of the Earth camera is
    approximately 20 x 20 degrees.
 
 Reference:
    Frank, L. A., J. B. Sigwarth, J. D. Craven, J. P. Cravens, J. S. Dolan,
        M. R. Dvorsky, J. D. Harvey, P. K. Hardebeck, and D. Muller,
        'The Visible Imaging System (VIS) for the Polar Spacecraft',
        Space Science Review, vol. 71, pp. 297-328, 1995.
 [Note to first-time users:  The first four variables are of primary interest.
    The displayable 256 x 256 image array is in variable 3.  The correct orien-
    tation of a displayed image is explained in the description of variable 3
    below.]
 
 Data set description:
         The VIS key parameter data set is a survey of auroral activity
    provided by a series of single images showing a significant area of the
    auroral zone.  The displayable image counts are in variable 3.
         Some coordinate information is included for viewer orientation.
    Coordinates are calculated for a grid of 18 x 18 points corresponding
    to one pixel out of every 15 x 15 pixel block.  In addition, a rotation
    matrix and a table of distortion-correcting look direction unit vectors
    are provided for the purpose of calculating coordinates for every pixel.
    See the description of variables 17 and 18 below.
         To facilitate viewing of the images, a mapping of pixel value to a
    recommended color table based on the characteristics of the selected
    filter will be included with each image.  See the description of variables
    22, 23, and 24 below.
         A relative intensity scale is provided by the uncompressed count table
    of variable 27.  Approximate intensity levels in kiloRayleighs are given in
    the intensity table of variable 28.  Information on the availability of
    more precisely calibrated intensities can be found on the VIS website at
    URL .http://eiger.physics.uiowa.edu/~vis/software/. 
 
 Variable descriptions:
 
    1,2. Center time
        The time assigned to an image is the center time of the integration
        period within a resolution of 50 milliseconds.
 
    3. Image counts
        Image pixel counts range from 0 to 255.  They are stored in a two-
        dimensional 256 x 256 byte array.  Images from the Earth camera
        (sensor 0) are conventionally displayed with row 1 at the top, row 256
        at the bottom, column 1 on the left, and column 256 on the right.  The
        conventional image display for the low resolution camera (sensor 1) is
        rotated 180 degrees so that the row 1-column 1 pixel is at the lower
        right corner and the row 256-column 256 pixel is at the upper left
        corner.  When displayed in this manner, the spacecraft spin axis is
        oriented to the right in the display, the X component is defined as
        the center of the image look direction, and the Y component is the
        cross product of the spin axis and the look direction.
 
    4. Sensor number
        0 = Earth camera,
        1 = low resolution camera,
        2 = medium resolution camera.
 
    5. Half integration time
        This is half the length of the integration period for the image,
        measured in milliseconds.
 
    6. Filter
        Twelve filters are available for visible imaging; the filter number,
        1-12, is given here.  Ultra-violet imaging is done with one filter only,
        designated here as filter number 0.  In addition, the peak wavelength
        in Angstroms is given for the selected filter.
 
    7. Presumed altitude of emissions
        The presumed altitude of the emissions seen in the image varies
        with the characteristics of the filter used.
 
    8. Field stop position
        The field stop may partially occlude the field of view of the low
        or medium resolution cameras.  The position is given in 1.5 degree
        steps.
 
    9. Platform pitch angle
        This is the platform pointing angle of rotation around the spin
        axis, measured from nadir.
 
 10,11. Mirror elevation and azimuth angles
        For the low or medium resolution camera, the two-axis mirror
        position is given in steps measured from the instrument calibration
        switches.  The boresight of the instrument is located at step 68 in
        azimuth and step 118 in elevation.
 
 12,13. Geographic coordinates
        Geographic north latitude and east longitude are provided for the
        pixels at these image array locations: every 15th row starting
        with row 1 and ending with row 256, and every 15th column starting
        with column 1 and ending with column 256, for a total of
        18 x 18 coordinate pairs.
 
 14,15. Spacecraft position and velocity vectors, GCI
        The spacecraft position vector and velocity vector in GCI
        coordinates are for the image center time as given in variables
        1 and 2.
 
   16. Spacecraft spin axis unit vector, GCI
 
 17,18. Image-to-GCI rotation matrix and look direction vector table
        The rotation matrix may be used with the look direction vector table to
        obtain pointing vectors in GCI coordinates for each pixel.  The
        resulting vectors may be used to calculate coordinates for the observed
        positions of the pixels.  Software for this purpose is available at URL
         .http://eiger.physics.uiowa.edu/~vis/software/.  The general method 
         used is described below.
 
        In the image coordinate system, the X axis is the center line-of-sight
        or look direction; the Y axis is the cross product of the spin axis an
        the X axis; and the Z axis is the cross product of the X axis and the
        Y axis.  When the display orientation conventions in the variable 3
        description are applied, the low resolution camera image is rotated so
        that both Earth camera and low resolution camera images are displayed
        with Y axis pointing up and Z axis pointing toward the right.
 
        To obtain the coordinates of the observed position of a pixel,
        calculate the intersection of the line-of-sight with the surface
        of an oblately spheroidal Earth at the altitude given as
        variable 7.  The equation of the spheroid is
            X**2/(A+ALT)**2 + Y**2/(A+ALT)**2 + Z**2/(B+ALT)**2 = 1
            where A is the Earth radius at the equator,
                  B is the Earth radius at the pole, and
                  ALT is the given altitude.
        The line-of-sight equations are
            (X-SCX)/DX = (Y-SCY)/DY = (Z-SCZ)/DZ
            where (SCX,SCY,SCZ) is the spacecraft position vector GCI, and
                    (DX,DY,DZ)  is the look direction unit vector GCI.
        Solve the line-of-sight equations for two variables in terms
        of the third; substitute into the spheroid equation; and use the
        quadratic formula to solve for the third variable.  Select
        the solution point closer to the spacecraft.
 
   19. Zenith angle of center line-of-sight at presumed altitude
        This is the angle between the geocentric vector through the
        observed point, assuming the altitude given as variable 7,
        and the reverse of the image center line-of-sight vector.
 
   20. Sun position unit vector, GCI
 
   21. Solar zenith angle at observed point of center line-of-sight
        This is the angle of the sun from zenith at the observed point
        of the center line-of-sight, assuming the altitude given as
        variable 7.
 
   22. RGB color table
        This is the recommended color table to be used with the
        limits given in variables 23 and 24.
 
 23,24. Low and high color mapping limits
        The low and high color limits are recommended for remapping
        the color table entries, as follows:
            For pixel values less than the low limit, use the color
                at table position 1.
            For pixel values greater than or equal to the low limit
                and less than or equal to the high limit, use the color
                at table position (pix-low)/(high-low) x 255 + 1.
            For pixel values greater than the high limit, use the color
                at table position 256.
 
   25. Data quality flag
        The data quality word has bits set to 1 when the listed
        conditions are true.  Bit #31 is the most significant bit in the
        word, and it will not be used as a flag.  These are the bit
        assignments:
            bit 0 - image data frame sync error
            bit 1 - image data frame counters error
            bit 2 - image data fill frame flag.
 
   26. Post gap flag
        The post gap flag has these possible values:
            0 - no gap occurred immediately prior to this record,
            1 - the gap occurred because the instrument was not in
                  a mode that allowed for the production of images for the
                  selected sensor,
            2 - the gap occurred because level zero data were missing,
            3 - the gap occurred because level zero data were too
                  noisy to extract images.
 
   27. Expanded count table
        The image pixel counts are quasi-logarithmically compressed to the
        range 0-255.  This table gives the average of the uncompressed range
        for each compressed count value.  Table entries 1-256 correspond to
        compressed counts 0-255 respectively.
 
   28. Intensity table
        Approximate intensity levels in kiloRayleighs are given for each
        compressed count value.  Table entries 1-256 correspond to compressed
        counts 0-255 respectively.  Information on the availability of more
        precisely calibrated intensities can be found on the VIS website at
        URL .http://eiger.physics.uiowa.edu/~vis/software/. 
 
 Supporting software:
    Supporting software is available on the VIS website at the URL
    .http://eiger.physics.uiowa.edu/~vis/software/.  Included is an IDL program 
    that displays the images with the recommended color bar and provides
    approximate intensities and coordinate data for each pixel.


Modification History
Initial development


Variable Notes

Visible Image (quasi-log cnts), small format display with click-expand (~4 min. res.)
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> Larger format display with click-expand, no geographics registration 
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> [DO NOT USE: BAD MAPPINGS] (USE SHORT TIME SPANS) With geographic map overlay
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> [DO NOT USE: UNDER-DEVELOPMENT] Test Display
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> [DO NOT USE: BAD MAPPINGS] (USE SHORT TIME SPANS) Azimuthal projection to geographic (fixed sun orientation)
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> [DO NOT USE: BAD MAPPINGS] (USE SHORT TIME SPANS) Azimuthal projection to magnetic LT and invariant lat
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Movie display of images, no geographic registration
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> [DO NOT USE: BAD MAPPINGS] (USE SHORT TIME SPANS) Movie, with geographic grid overlay
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> [DO NOT USE: BAD MAPPINGS] (USE SHORT TIME SPANS) Movie, azimuthal projection to geographic (fixed sun orientation)
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> [DO NOT USE: BAD MAPPINGS] (USE SHORT TIME SPANS) Movie, azimuthal projection to magnetic LT and invariant lat
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
Visible Image (kRay), small format display with click-expand (~4 min. res.)
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> Larger format display with click-expand, no geographic registration
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> [DO NOT USE: BAD MAPPINGS] (USE SHORT TIME SPANS) With geographic grid overlay
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> [DO NOT USE: BAD MAPPINGS] (USE SHORT TIME SPANS) Azimuthal projection to geographic (fixed sun orientation)
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> [DO NOT USE: BAD MAPPINGS] (USE SHORT TIME SPANS) Azimuthal projection to magnetic LT and invariant lat
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Movie display of images, no geographic registration
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> [DO NOT USE: BAD MAPPINGS] (USE SHORT TIME SPANS) Movie, with geographic grid overlay
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> [DO NOT USE: BAD MAPPINGS] (USE SHORT TIME SPANS) Movie, azimuthal projection to geographic (fixed sun orientation)
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> [DO NOT USE: BAD MAPPINGS] (USE SHORT TIME SPANS) Movie, azimuthal projection to magnetic LT and invariant lat
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
Geographic latitude grid - virtual var.
Geographic N. latitude for pixels vals - computed by CDAWeb
Geographic longitude grid - virtual var.
Geographic E. longitude for pixels vals - computed by CDAWeb
Filter number and peak wavelength in Angstroms)
Filters #1-12 are visible wavelengths; filter #0 is UV for Earth camera images
Field-stop wheel position (1 step = 1.5 degrees)
A field stop may occultsome part of a visible image
Platform pointing angle from nadir
Platform angle of rotation around spin axis, measured from nadir in tenths of
degrees
Mirror pointing angle, elevation
Mirror pointing angle out of s/c X-Y plane in steps of ~.08660 degrees
Mirror pointing angle, azimuth
Mirror pointing angle of rotation around spin axis, w/r/t platform position, in
steps of ~.09375 degrees.
Geographic latitude grid
Geographic N. latitude for pixels at every 15th row and column from 1 to 256
Geographic longitude grid
Geographic E. longitude for pixels at every 15th row and column from 1 to 256
Image-to-GCI rotation matrix
X component is look direction,Y component is the spin axis  cross X
RGB color lookup table
RGBColorTable should be remapped for displaying an image using the low and high
limits given for each image in Limit_Lo and Limit_Hi.Image_Counts count values
less than Limit_Lo use the color at table position 1.  Count values greater than
Limit_Hi use the color at table position 256.  For count values greater than or
equal to Limit_Lo and less than or equal to Limit_Hi, the table position is
(Count-Limit_Lo)/(Limit_Hi-Limit_Lo) x 255 + 1.At the selected table position C,
the color components are Red at RGBColorTable(1,C), Green at RGBColorTable(2,C),
and Blue at RGBColorTable(3,C).
Data quality flags
MSB will not be used as a flag; see TEXT for other bit assignments
Expanded count table: quasi-logarithmically uncompressed pixel counts
Image_Counts contains pixel counts which have been quasi-logarithmically
compressed by the instrument.  Approximate uncompressed value
forImage_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).
Approximate intensity levels in kiloRayleighs
Approximate intensity in kR for Image_Counts(i,j)
isIntens_Table(Image_Counts(i,j)+1)


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PO_K1_TIM
Description
H+, O+, He+ and He++ number fluxes for survey  purposes only 
E.G. Shelley et al., The Toroidal Imaging Mass-Angle Spectrograph (TIMAS) for the Polar Mission, Sp.
Sci. Rev, Vol 71, pp 497-530, 1995.
ftp://sierra.spasci.com/DATA/timas/TIMAS_description.html



Metadata provided by W.K. Peterson


Modification History
Version 0 June, 2001




Back to Top
PO_K1_VIS
Description
 Instrument functional description:
    The VIS is a set of three low-light-level cameras.  Two of these
    cameras share primary and some secondary optics and are designed to
    provide images of the nighttime auroral oval at visible wavelengths.
    A third camera is used to monitor the directions of the fields-of-view
    of the auroral cameras with respect to the sunlit Earth and return
    global images of the auroral oval at ultraviolet wavelengths.  The
    VIS instrumentation produces an auroral image of 256 x 256 pixels
    approximately every 24 seconds dependent on the integration time and
    filter selected.  The fields-of-view of the two nighttime auroral
    cameras are 5.6 x 6.3 degrees and 2.8 x 3.3 degrees for the low and
    medium resolution cameras, respectively.  One or more Earth camera
    images of 256 x 256 pixels are produced every five minutes, depending
    on the commanded mode.  The field-of-view of the Earth camera is
    approximately 20 x 20 degrees.
 
 Reference:
    Frank, L. A., J. B. Sigwarth, J. D. Craven, J. P. Cravens, J. S. Dolan,
        M. R. Dvorsky, J. D. Harvey, P. K. Hardebeck, and D. Muller,
        'The Visible Imaging System (VIS) for the Polar Spacecraft',
        Space Science Review, vol. 71, pp. 297-328, 1995.
 [Note to first-time users:  The first four variables are of primary interest.
    The displayable 256 x 256 image array is in variable 3.  The correct orien-
    tation of a displayed image is explained in the description of variable 3
    below.]
 
 Data set description:
         The VIS Earth camera key parameter data set is a survey of global
    auroral activity providedby a series of piled images produced by the median-
    filtering of up to five consecutive images.  The displayable image counts
    are in variable 3.
         Some coordinate information is included for viewer orientation.
    Coordinates are calculated for a grid of 18 x 18 points corresponding
    to one pixel out of every 15 x 15 pixel block.  In addition, a rotation
    matrix and a table of distortion-correcting look direction unit vectors
    are provided for the purpose of calculating coordinates for every pixel.
    See the description of variables 14 and 15 below.
         To facilitate viewing of the images, a mapping of pixel value to a
    recommended color table based on the characteristics of the selected
    filter will be included with each image.  See the description of variables
    19, 20, and 21 below.
         A relative intensity scale is provided by the uncompressed count table
    of variable 24.  Approximate intensity levels in kiloRayleighs are given in
    the intensity table of variable 25.  Information on the availability of
    more precisely calibrated intensities can be found on the VIS website at
    URL .http://eiger.physics.uiowa.edu/~vis/software/. 
 
 Variable descriptions:
 
    1,2. Center time
        The time assigned to an image is the center time of the integration
        period within a resolution of 50 milliseconds.
 
    3. Image counts
        Image pixel counts range from 0 to 255.  They are stored in a two-
        dimensional 256 x 256 byte array.  Images from the Earth camera
        (sensor 0) are conventionally displayed with row 1 at the top, row 256
        at the bottom, column 1 on the left, and column 256 on the right.  The
        conventional image display for the low resolution camera (sensor 1) is
        rotated 180 degrees so that the row 1-column 1 pixel is at the lower
        right corner and the row 256-column 256 pixel is at the upper left
        corner.  When displayed in this manner, the spacecraft spin axis is
        oriented to the right in the display, the X component is defined as
        the center of the image look direction, and the Y component is the
        cross product of the spin axis and the look direction.
 
    4. Sensor number
        0 = Earth camera,
        1 = low resolution camera,
        2 = medium resolution camera.
 
    5. Half integration time
        This is half the length of the integration period for the image,
        measured in milliseconds.
 
    6. Filter
        Twelve filters are available for visible imaging; the filter number,
        1-12, is given here.  Ultra-violet imaging is done with one filter only,
        designated here as filter number 0.  In addition, the peak wavelength
        in Angstroms is given for the selected filter.
 
    7. Presumed altitude of emissions
        The presumed altitude of the emissions seen in the image varies
        with the characteristics of the filter used.
 
    8. Platform pitch angle
        This is the platform pointing angle of rotation around the spin
        axis, measured from nadir.
 
  9,10. Geographic coordinates
        Geographic north latitude and east longitude are provided for the
        pixels at these image array locations: every 15th row starting
        with row 1 and ending with row 256, and every 15th column starting
        with column 1 and ending with column 256, for a total of
        18 x 18 coordinate pairs.
 
 11,12. Spacecraft position and velocity vectors, GCI
        The spacecraft position vector and velocity vector in GCI
        coordinates are for the image center time as given in variables
        1 and 2.
 
   13. Spacecraft spin axis unit vector, GCI
 
 14,15. Image-to-GCI rotation matrix and look direction vector table
        The rotation matrix may be used with the look direction vector table to
        obtain pointing vectors in GCI coordinates for each pixel.  The
        resulting vectors may be used to calculate coordinates for the observed
        positions of the pixels.  Software for this purpose is available at URL
         .http://eiger.physics.uiowa.edu/~vis/software/.  The general method 
         used is described below.
 
        In the image coordinate system, the X axis is the center line-of-sight
        or look direction; the Y axis is the cross product of the spin axis an
        the X axis; and the Z axis is the cross product of the X axis and the
        Y axis.  When the display orientation conventions in the variable 3
        description are applied, the low resolution camera image is rotated so
        that both Earth camera and low resolution camera images are displayed
        with Y axis pointing up and Z axis pointing toward the right.
 
        To obtain the coordinates of the observed position of a pixel,
        calculate the intersection of the line-of-sight with the surface
        of an oblately spheroidal Earth at the altitude given as
        variable 7.  The equation of the spheroid is
            X**2/(A+ALT)**2 + Y**2/(A+ALT)**2 + Z**2/(B+ALT)**2 = 1
            where A is the Earth radius at the equator,
                  B is the Earth radius at the pole, and
                  ALT is the given altitude.
        The line-of-sight equations are
            (X-SCX)/DX = (Y-SCY)/DY = (Z-SCZ)/DZ
            where (SCX,SCY,SCZ) is the spacecraft position vector GCI, and
                    (DX,DY,DZ)  is the look direction unit vector GCI.
        Solve the line-of-sight equations for two variables in terms
        of the third; substitute into the spheroid equation; and use the
        quadratic formula to solve for the third variable.  Select
        the solution point closer to the spacecraft.
 
   16. Zenith angle of center line-of-sight at presumed altitude
        This is the angle between the geocentric vector through the
        observed point, assuming the altitude given as variable 7,
        and the reverse of the image center line-of-sight vector.
 
   17. Sun position unit vector, GCI
 
   18. Solar zenith angle at observed point of center line-of-sight
        This is the angle of the sun from zenith at the observed point
        of the center line-of-sight, assuming the altitude given as
        variable 7.
 
   19. RGB color table
        This is the recommended color table to be used with the
        limits given in variables 20 and 21.
 
 20,21. Low and high color mapping limits
        The low and high color limits are recommended for remapping
        the color table entries, as follows:
            For pixel values less than the low limit, use the color
                at table position 1.
            For pixel values greater than or equal to the low limit
                and less than or equal to the high limit, use the color
                at table position (pix-low)/(high-low) x 255 + 1.
            For pixel values greater than the high limit, use the color
                at table position 256.
 
   22. Data quality flag
        The data quality word has bits set to 1 when the listed
        conditions are true.  Bit #31 is the most significant bit in the
        word, and it will not be used as a flag.  These are the bit
        assignments:
            bit 0 - image data frame sync error
            bit 1 - image data frame counters error
            bit 2 - image data fill frame flag.
 
   23. Post gap flag
        The post gap flag has these possible values:
            0 - no gap occurred immediately prior to this record,
            1 - the gap occurred because the instrument was not in
                  a mode that allowed for the production of images for the
                  selected sensor,
            2 - the gap occurred because level zero data were missing,
            3 - the gap occurred because level zero data were too
                  noisy to extract images.
 
   24. Expanded count table
        The image pixel counts are quasi-logarithmically compressed to the
        range 0-255.  This table gives the average of the uncompressed range
        for each compressed count value.  Table entries 1-256 correspond to
        compressed counts 0-255 respectively.
 
   25. Intensity table
        Approximate intensity levels in kiloRayleighs are given for each
        compressed count value.  Table entries 1-256 correspond to compressed
        counts 0-255 respectively.  Information on the availability of more
        precisely calibrated intensities can be found on the VIS website at
        URL .http://eiger.physics.uiowa.edu/~vis/software/. 
 
 Supporting software:
    Supporting software is available on the VIS website at the URL
    .http://eiger.physics.uiowa.edu/~vis/software/.  Included is an IDL program 
    that displays the images with the recommended color bar and provides
    approximate intensities and coordinate data for each pixel.


Modification History
Initial development
modified linear validmin 0=>15, linear validmax 255=>50 to suppress dayglow for UVI testing -
4/12/01 - REM
modified log validmax 255=>15 to suppress dayglow - 4/12/01 - REM


Variable Notes

Earth Camera UV Images (quasi-log cnts), small format display with click-expand (~4 min. res.)
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> Larger format display with click-expand, no geographics registration 
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) With geographic grid overlay
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> [DO NOT USE: UNDER-DEVELOPMENT] Test Display
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Azimuthal projection to geographic (fixed sun orientation)
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Azimuthal projection to magnetic LT and invariant lat
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Movie display of images, no geographic registration
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Movie, with geographic grid overlay
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Movie, azimuthal projection to geographic (fixed sun orientation)
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Movie, azimuthal projection to magnetic LT and invariant lat
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
Earth Camera UV Images (kRay), small format display with click-expand (~4 min. res.)
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> Larger format display with click-expand, no geographic registration
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) With geographic grid overlay
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Azimuthal projection to geographic (fixed sun orientation)
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Azimuthal projection to magnetic LT and invariant lat
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Movie display of images, no geographics registration
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Movie, with geographic grid overlay
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Movie, azimuthal projection to geographic (fixed sun orientation)
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
--> (USE SHORT TIME SPANS) Movie, azimuthal projection to magnetic LT and invariant lat
Image_Counts contains the displayable image.  The counts have been
quasi-logarithmically compressed by the instrument.  Approximate uncompressed
value for Image_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).  Approximate
intensity in kR is Intens_Table(Image_Counts(i,j)+1).The appearance of the
actual count value 255 is rare.  When displaying an image,it works best to use
the fill value as an overflow (i.e. brightest) value.
Geographic latitude grid - virtual var.
Geographic N. latitude for pixels vals - computed by CDAWeb
Geographic longitude grid - virtual var.
Geographic E. longitude for pixels vals - computed by CDAWeb
Filter number and peak wavelength in Angstroms)
Filters #1-12 are visible wavelengths; filter #0 is UV for Earth camera images
Platform pointing angle from nadir
Platform angle of rotation around spin axis, measured from nadir in tenths of
degrees
Geographic latitude grid
Geographic N. latitude for pixels at every 15th row and column from 1 to 256
Geographic longitude grid
Geographic E. longitude for pixels at every 15th row and column from 1 to 256
Image-to-GCI rotation matrix
X component is look direction,Y component is the spin axis  cross X
RGB color lookup table
RGBColorTable should be remapped for displaying an image using the low and high
limits given for each image in Limit_Lo and Limit_Hi.Image_Counts count values
less than Limit_Lo use the color at table position 1.  Count values greater than
Limit_Hi use the color at table position 256.  For count values greater than or
equal to Limit_Lo and less than or equal to Limit_Hi, the table position is
(Count-Limit_Lo)/(Limit_Hi-Limit_Lo) x 255 + 1.At the selected table position C,
the color components are Red at RGBColorTable(1,C), Green at RGBColorTable(2,C),
and Blue at RGBColorTable(3,C).
Data quality flags
MSB will not be used as a flag; see TEXT for other bit assignments
Expanded count table: quasi-logarithmically uncompressed pixel counts
Image_Counts contains pixel counts which have been quasi-logarithmically
compressed by the instrument.  Approximate uncompressed value
forImage_Counts(i,j) is ExpandedCount(Image_Counts(i,j)+1).
Approximate intensity levels in kiloRayleighs
Approximate intensity in kR for Image_Counts(i,j)
isIntens_Table(Image_Counts(i,j)+1)
Header image number
Sequence number of image in pile of up to five images


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PO_OR_DEF
Description
TBS


Modification History
Originated Monday, May 13, 1991
Modified June 13, 1991 for version 2.1
Modified October 2,1991 for new global attributes, incr sizes
Modified 11/11/91 Add sun vector, replace space id with support id
Modified 1992 Feb 11 to use the variable name TIME and type CDF_INT4 instead of 
EPOCH and CDF_EPOCH for the time tags CCR 490
Modified 6/2/92 add project, discipline, source_name, data_version, title, and 
mods to global section; add validmin, validmax, labl_ptr_1 and monoton 
attributes to some variables; put epoch time back in, rename time to 
time_pb5; add label_time to variables
Modified 11/07/92 to use Epoch and Time_PB5 variable name
Modified 6/2/93 add ADID_ref and Logical_file_id
7/5/94 - CCR ISTP 1852 updated CDHF skeleton to CDF standards - JT
9/21/94 - Added 24 new global attributes to log the ephemeris 
comparison summary report from the definitive FDF orbit file.  CCR 1932
11/7/94 - Merged CCR 1852 changes and corrected errors 
made in CCR 1852.  ICCR 1884
12/7/94 - Modified MODS to follow ISTP standards.  ICCR 1885
01/05/95 - add heliocentric coordinate system.  CCR 1889
2/28/95 - added COMMENT1 and COMMENT2 for CCR 
11/03/95 - deleted crn_space for CCR 2154 - RM




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PO_OR_PRE
Description
TBS


Modification History
Originated Monday, May 13, 1991
Modified June 13, 1991 for version 2.1
Modified October 2,1991 for new global attributes, incr sizes
Modified 11/11/91 Add sun vector, replace space id with support id
Modified 1992 Feb 11 to use the variable name TIME and type CDF_INT4 instead of 
EPOCH and CDF_EPOCH for the time tags CCR 490
Modified 6/2/92 add project, discipline, source_name, data_version, title, and 
mods to global section; add validmin, validmax, labl_ptr_1 and monoton 
attributes to some variables; put epoch time back in, rename time to 
time_pb5; add label_time to variables
Modified 11/07/92 to use Epoch and Time_PB5 variable name
Modified 6/2/93 add ADID_ref and Logical_file_id
7/5/94 - CCR ISTP 1852 updated CDHF skeleton to CDF standards - JT
9/21/94 - Added 24 new global attributes to log the ephemeris 
comparison summary report from the definitive FDF orbit file.  CCR 1932
11/7/94 - Merged CCR 1852 changes and corrected errors 
made in CCR 1852.  ICCR 1884
12/7/94 - Modified MODS to follow ISTP standards.  ICCR 1885
01/05/95 - add heliocentric coordinate system.  CCR 1889
2/28/95 - added COMMENT1 and COMMENT2 for CCR 
11/03/95 - deleted crn_space for CCR 2154 - RM




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PO_PA_DEF
Description
Based on the FDF DPA algorithm


Modification History
6/11/93 - Original Implementation
4/1/94 - Modified VALIDMIN and VALIDMAX for ORB_ROLL, 
ORB_YAW, GCI_ROLL, GCI_YAW, GSE_ROLL, GSE_YAW, GSM_ROLL, and GSM_YAW
6/7/94 - CCR ISTP 1852, updated CDHF skeleton to CDF standards - JT
11/9/94 - Correct errors made in ccr 1852.  ICCR 1884
04/04/96 - Added despun plat.offset and lock status




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S1_C9_S019
Description
Derived from s019 in CDAW9 DB.
Data for all CDAW9 events A-E
CDAW-9; 1982-019A Energetic Part.; 10 s; 6.6
For time history: plot one flux channel from S019DJE or S019DJP vs time, filter on S019EEN or
S019PEN to select the channel.  Energy spectrum: use XY plot S019DJE vs S019EEN, with filter on
desired time.  Use Animation for multiple spectra. 
Longitudes:  S019: 322 E;   S037: 70 E;   S129: 205 E
A simplified subset of these data is available in SA19.
CDFs from the 3 s/c 1982-019A, 1984-037A and 1984-129A are identical in form. There are 4 detectors:
low energy electrons (LOE), high energy  electrons (HIE), each with 6 energy ranges; and LOP and HIP
for protons, with 10 and 16 energy ranges (only the 1st 6 or 7 of HIP are useful).  For LOE, HIE,
and LOP, each range is from a lower energy level up to the detector maximum--an integrated energy. 
For example, the 1st two LOE ranges are 30-300 keV and 45-300 keV.  The 30-45 keV range is thus the
difference between the two measurements.  For low levels, background is significant, and
measurements for a detector may not be strictly monotonic for any individual 10-s average.  In such
cases, the differential flux is made 0 for energies above the non-monotonic flux. 
6 HIE fluxes are stacked after 6 LOE fluxes in S019DJE. Low edge of each energy bin is in S019EEN
and bands are contiguous, so 1st bin is 30-45 keV. Band 6 is top band of LOE (200-300 keV), same as
band 7 (lowest energy of HIE).  Topmost energy is 2000 keV.  The 5 channels marked 1996-2000 keV are
fill values only.  
10 LOP channels are in elements 1-9 and 11 of S019DJP and the 1st 7 HIP channels are in elements 10
and 12-17, so ranges increase monotonically. Low edge of energy bin is in S019PEN; upper edge is
value of the bin above it except bins 9-11 have ranges .377-.462, .37-.52, and .462-.600 MeV.
Topmost energy bin is  1.7-2.2 MeV. 
For time history of the data, plot flux from S019DJE or S019DJP vs time, and filter on S019EEN or
S019PEN to select the channel.  Energy spectrum: make an XY plot of S019DJE vs S019EEN (for
electrons), filtered on desired time. For successive spectra (spectra are available every 10-s), use
Animation. 
Direction cosines for H, V, D are with respect to dipole-meridian coordinates: H is parallel to the
dipole axis, V radially outward, and D east.  S019THET and S019PHI are colatitude relative to the H
axis and the azimuth measured from the negative V axis.


Modification History
Converted to CDAWeb Feb 2000




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S1_C9_SA19
Description
Derived from sa19 in CDAW9 DB.
Data from all CDAW9 events A-E.
Selected energies from S019
CDFs from the 3 s/c 1982-019A, 1984-037A and 1984-129A are identical in form. There are 4 detectors:
low energy electrons (LOE), high energy  electrons (HIE), each with 6 energy ranges; and LOP and HIP
for protons, with 10 and 16 energy ranges (only the 1st 6 or 7 of HIP are useful).  For LOE, HIE,
and LOP, each range is from a lower energy level up to the detector maximum--an integrated energy. 
For example, the 1st two LOE ranges are 30-300 keV and 45-300 keV.  The 30-45 keV range is thus the
difference between the two measurements.  For low levels, background is significant, and
measurements for a detector may not be strictly monotonic for any individual 10-s average.  In such
cases, the differential flux is made 0 for energies above the non-monotonic flux. 
This CDF is a subset of S019, containing only selected energy channels for the  particle flux, and
some of the other variables.  Each energy channel is now in a separate variable.  The selected
fluxes are:  all 6 for LOE, the lowest 8 for LOP, and the lowest 5 for HIP, corresponding to
elements 1-6 in S019DJE, and elements 1-8,10,12-15 in S019DJP. 
Direction cosines for H, V, D are with respect to dipole-meridian coordinates: H is parallel to the
dipole axis, V radially outward, and D east.  S019THET and S019PHI are colatitude relative to the H
axis and the azimuth measured from the negative V axis.


Modification History
Converted to CDAWeb Feb 2000




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S1_ED_EP
Description
CDFs from the 3 s/c 1982-019A, 1984-037A and 1984-129A are identical in form. Th
ere are 4 detectors: low energy electrons (LOE), high energy  electrons (HIE), e
ach with 6 energy ranges; and LOP and HIP for protons, with 10 and 16 energy ran
ges (only the 1st 6 or 7 of HIP are useful).  For LOE, HIE, and LOP, each range
is from a lower energy level up to the detector maximum--an integrated energy.
For example, the 1st two LOE ranges are 30-300 keV and 45-300 keV. The 30-45 keV
 range is thus the difference between the two measurements.  For low levels, bac
kground is significant, and measurements for a detector may not be strictly mono
tonic for any individual 10-s average.  In such cases, the differential flux is
made 0 for energies above the non-monotonic flux. 6 HIE fluxes are stacked after
 6 LOE fluxes in S019DJE. Low edge of each energy bin is in S019EEN and bands ar
e contiguous, so 1st bin is 30-45 keV. Band 6 is top band of LOE (200-300 keV),
same as band 7 (lowest energy of HIE).  Topmost energy is 2000 keV.  The 5 chann
els marked 1996-2000 keV are fill values only. 10 LOP channels are in elements 1
-9 and 11 of S019DJP and the 1st 7 HIP channels are in elements 10 and 12-17, so
 ranges increase monotonically. Low edge of energy bin is in S019PEN; upper edge
 is value of the bin above it except bins 9-11 have ranges .377-.462, .37-.52, a
nd .462-.600 MeV. Topmost energy bin is 1.7-2.2 MeV. For time history of the dat
a, plot flux from S019DJE or S019DJP vs time, and filter on S019EEN or S019PEN t
o select the channel.  Energy spectrum: make an XY plot of S019DJE vs S019EEN (f
or electrons), filtered on desired time. For successive spectra (spectra are ava
ilable every 10-s), use Animation. Direction cosines for H, V, D are with respec
t to dipole-meridian coordinates: H is parallel to the dipole axis, V radially o
utward, and D east.  S019THET and S019PHI are colatitude relative to the H axis
and the azimuth measured from the negative V axis. Longitudes:  S019: 322 E;   S
037: 70 E;   S129: 205 E A simplified subset of these data is available in SA19.


Modification History




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S2_ED_EP
Description
CDFs from the 3 s/c 1982-019A, 1984-037A and 1984-129A are identical in form. Th
ere are 4 detectors: low energy electrons (LOE), high energy  electrons (HIE), e
ach with 6 energy ranges; and LOP and HIP for protons, with 10 and 16 energy ran
ges (only the 1st 6 or 7 of HIP are useful).  For LOE, HIE, and LOP, each range 
is from a lower energy level up to the detector maximum--an integrated energy.  
For example, the 1st two LOE ranges are 30-300 keV and 45-300 keV. The 30-45 keV
 range is thus the difference between the two measurements.  For low levels, bac
kground is significant, and measurements for a detector may not be strictly mono
tonic for any individual 10-s average.  In such cases, the differential flux is 
made 0 for energies above the non-monotonic flux. 6 HIE fluxes are stacked after
 6 LOE fluxes in S037DJE. Low edge of each energy bin is in S037EEN and bands ar
e contiguous, so 1st bin is 30-45 keV. Band 6 is top band of LOE (200-300 keV), 
same as band 7 (lowest energy of HIE).  Topmost energy is 2000 keV.  The 5 chann
els marked 1996-2000 keV are fill values only. 10 LOP channels are in elements 1
-9 and 11 of S037DJP and the 1st 7 HIP channels are in elements 10 and 12-17, so
 ranges increase monotonically.  Low edge of energy bin is in S037PEN; upper edg
e is value of the bin above it except bins 9-11 have ranges .35-.45, .38-.49, an
d .45-.56 MeV. Topmost energy bin is 1.8-2.3 MeV. For time history of the data, 
plot flux from S037DJE or S037DJP vs time, and filter on S037EEN or S037PEN to s
elect the channel.  Energy spectrum: make an XY plot of S037DJE vs S037EEN (for 
electrons), filtered on desired time. For successive spectra (spectra are availa
ble every 10-s), use Animation. Direction cosines H, V, D, S037THET and S037PHI 
have spurious values for S037. Longitudes:  S019: 322 E;   S037: 70 E;   S129: 2
05 E A simplified subset of these data is available in SA37.


Modification History




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S3_C9_S037
Description
Derived from c037 in CDAW9 DB.
Data from all CDAW9 events A-E
CDAW-9; 1984-037A; Energetic Part.; 10 s; 6.6 Re  
Variables HCOS,VCOS,DCOS, THET,PHI are spurious.  
For time history: plot one flux channel from S037DJE or S037DJP vs time, filter on S037EEN or
S037PEN to select the channel.  Energy spectrum: use XY plot S037DJE vs S037EEN, with filter on
desired time.  Use Animation for multiple spectra.   
Longitudes:  S019: 322 E;   S037: 70 E;   S129: 205 E  
A simplified subset of these data is available in SA37.  
CDFs from the 3 s/c 1982-019A, 1984-037A and 1984-129A are identical in form. There are 4 detectors:
low energy electrons (LOE), high energy  electrons (HIE), each with 6 energy ranges; and LOP and HIP
for protons, with 10 and 16 energy ranges (only the 1st 6 or 7 of HIP are useful).  For LOE, HIE,
and LOP, each range is from a lower energy level up to the detector maximum--an integrated energy. 
For example, the 1st two LOE ranges are 30-300 keV and 45-300 keV.  The 30-45 keV range is thus the
difference between the two measurements.  For low levels, background is significant, and
measurements for a detector may not be strictly monotonic for any individual 10-s average.  In such
cases, the differential flux is made 0 for energies above the non-monotonic flux.   
6 HIE fluxes are stacked after 6 LOE fluxes in S037DJE. Low edge of each energy bin is in S037EEN
and bands are contiguous, so 1st bin is 30-45 keV. Band 6 is top band of LOE (200-300 keV), same as
band 7 (lowest energy of HIE).  Topmost energy is 2000 keV.  The 5 channels marked 1996-2000 keV are
fill values only.   
10 LOP channels are in elements 1-9 and 11 of S037DJP and the 1st 7 HIP channels are in elements 10
and 12-17, so ranges increase monotonically.  Low edge of energy bin is in S037PEN; upper edge is
value of the bin above it except bins 9-11 have ranges .35-.45, .38-.49, and .45-.56 MeV. Topmost
energy bin is  1.8-2.3 MeV.   
For time history of the data, plot flux from S037DJE or S037DJP vs time, and filter on S037EEN or
S037PEN to select the channel.  Energy spectrum: make an XY plot of S037DJE vs S037EEN (for
electrons), filtered on desired time. For successive spectra (spectra are available every 10-s), use
Animation.   
Direction cosines H, V, D, S037THET and S037PHI have spurious values for S037.


Modification History
Converted to CDAWeb Feb 2000




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S3_C9_SA37
Description
Derived from sa37 in CDAW9 DB.
Data from all CDAW9 events A-E.
Selected energies from S037
CDFs from the 3 s/c 1982-019A, 1984-037A and 1984-129A are identical in form. There are 4 detectors:
low energy electrons (LOE), high energy  electrons (HIE), each with 6 energy ranges; and LOP and HIP
for protons, with 10 and 16 energy ranges (only the 1st 6 or 7 of HIP are useful).  For LOE, HIE,
and LOP, each range is from a lower energy level up to the detector maximum--an integrated energy. 
For example, the 1st two LOE ranges are 30-300 keV and 45-300 keV.  The 30-45 keV range is thus the
difference between the two measurements.  For low levels, background is significant, and
measurements for a detector may not be strictly monotonic for any individual 10-s average.  In such
cases, the differential flux is made 0 for energies above the non-monotonic flux.  
This CDF is a subset of S037, containing only selected energy channels for the  particle flux, and
some of the other variables.  Each energy channel is now in a separate variable.  The selected
fluxes are:  all 6 for LOE, the lowest 8 for LOP, and the lowest 5 for HIP, corresponding to
elements 1-6 in S037DJE, and elements 1-8,10,12-15 in S037DJP.  
Direction cosines for H, V, D are with respect to dipole-meridian coordinates: H is parallel to the
dipole axis, V radially outward, and D east.  S037THET and S037PHI are colatitude relative to the H
axis and the azimuth measured from the negative V axis.


Modification History
Converted to CDAWeb Feb 2000




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S3_ED_EP
Description
CDFs from the 3 s/c 1982-019A, 1984-037A and 1984-129A are identical in form. Th
ere are 4 detectors: low energy electrons (LOE), high energy  electrons (HIE), e
ach with 6 energy ranges; and LOP and HIP for protons, with 10 and 16 energy ran
ges (only the 1st 6 or 7 of HIP are useful).  For LOE, HIE, and LOP, each range 
is from a lower energy level up to the detector maximum--an integrated energy.  
For example, the 1st two LOE ranges are 30-300 keV and 45-300 keV. The 30-45 keV
 range is thus the difference between the two measurements.  For low levels, bac
kground is significant, and measurements for a detector may not be strictly mono
tonic for any individual 10-s average.  In such cases, the differential flux is 
made 0 for energies above the non-monotonic flux. 6 HIE fluxes are stacked after
 6 LOE fluxes in S129DJE. Low edge of each energy bin is in S129EEN and bands ar
e contiguous, so 1st bin is 30-45 keV. Band 6 is top band of LOE (200-300 keV), 
same as band 7 (lowest energy of HIE).  Topmost energy is 2000 keV.  The 5 chann
els marked 1996-2000 keV are fill values only. 10 LOP channels are in elements 1
-9 and 11 of S129DJP and the 1st 7 HIP channels are in elements 10 and 12-17, so
 ranges increase monotonically.  Low edge of energy bin is in S129PEN; upper edg
e is value of the bin above it except bins 9-11 have ranges .365-.457, .36-.48, 
and .457-.573 MeV.  Topmost energy bin is 1.80-2.05 MeV. For time history of the
 data, plot flux from S129DJE or S129DJP vs time, and filter on S129EEN or S129P
EN to select the channel.  Energy spectrum: make an XY plot of S129DJE vs S129EE
N (for electrons), filtered on desired time. For successive spectra (spectra are
 available every 10-s), use Animation. Direction cosines H, V, D, S129THET and S
129PHI  have spurious values for S129. Longitudes:  S019: 322 E;   S037: 70 E;  
 S129: 205 E. A simplified subset of these data is available in SA29.


Modification History




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S9_C9_S129
Description
Derived from CC01 in CDAW9 DB.
Data for all CDAW9 events A-E.
Variables HCOS,VCOS,DCOS, THET,PHI are spurious.
For time history: plot one flux channel from S129DJE or S129DJP vs time, filter on S129EEN or
S129PEN to select the channel.  Energy spectrum: use XY plot S129DJE vs S129EEN, with filter on
desired time. Use Animation for multiple spectra.  
Longitudes:  S019: 322 E;   S037: 70 E;   S129: 205 E 
A simplified subset of these data is available in SA29. 
CDFs from the 3 s/c 1982-019A, 1984-037A and 1984-129A are identical in form. There are 4 detectors:
low energy electrons (LOE), high energy  electrons (HIE), each with 6 energy ranges; and LOP and HIP
for protons, with 10 and 16 energy ranges (only the 1st 6 or 7 of HIP are useful).  For LOE, HIE,
and LOP, each range is from a lower energy level up to the detector maximum--an integrated energy. 
For example, the 1st two LOE ranges are 30-300 keV and 45-300 keV.  The 30-45 keV range is thus the
difference between the two measurements.  For low levels, background is significant, and
measurements for a detector may not be strictly monotonic for any individual 10-s average.  In such
cases, the differential flux is made 0 for energies above the non-monotonic flux.  
6 HIE fluxes are stacked after 6 LOE fluxes in S129DJE. Low edge of each energy bin is in S129EEN
and bands are contiguous, so 1st bin is 30-45 keV. Band 6 is top band of LOE (200-300 keV), same as
band 7 (lowest energy of HIE).  Topmost energy is 2000 keV.  The 5 channels marked 1996-2000 keV are
fill values only.  
10 LOP channels are in elements 1-9 and 11 of S129DJP and the 1st 7 HIP channels are in elements 10
and 12-17, so ranges increase monotonically.  Low edge of energy bin is in S129PEN; upper edge is
value of the bin above it except bins 9-11 have ranges .365-.457, .36-.48, and .457-.573 MeV. 
Topmost energy bin is  1.80-2.05 MeV.  
For time history of the data, plot flux from S129DJE or S129DJP vs time, and filter on S129EEN or
S129PEN to select the channel.  Energy spectrum: make an XY plot of S129DJE vs S129EEN (for
electrons), filtered on desired time. For successive spectra (spectra are available every 10-s), use
Animation.  
Direction cosines H, V, D, S129THET and S129PHI  have spurious values for S129.


Modification History
Converted to CDAWeb Feb 2000




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S9_C9_SA29
Description
Derived from sa29 in CDAW9 DB.
Data from all CDAW9 events A-E.
Selected energies from S129
CDFs from the 3 s/c 1982-019A, 1984-037A and 1984-129A are identical in form. There are 4 detectors:
low energy electrons (LOE), high energy  electrons (HIE), each with 6 energy ranges; and LOP and HIP
for protons, with 10 and 16 energy ranges (only the 1st 6 or 7 of HIP are useful).  For LOE, HIE,
and LOP, each range is from a lower energy level up to the detector maximum--an integrated energy. 
For example, the 1st two LOE ranges are 30-300 keV and 45-300 keV. The 30-45 keV range is thus the
difference between the two measurements.  For low levels, background is significant, and
measurements for a detector may not be strictly monotonic for any individual 10-s average.  In such
cases, the differential flux is made 0 for energies above the non-monotonic flux.  
This CDF is a subset of S129, containing only selected energy channels for the  particle flux, and
some of the other variables.  Each energy channel is now in a separate variable.  The selected
fluxes are:  all 6 for LOE, the lowest 8 for LOP, and the lowest 5 for HIP, corresponding to
elements 1-6 in S129DJE, and elements 1-8,10,12-15 in S129DJP.  
Direction cosines for H, V, D are with respect to dipole-meridian coordinates: H is parallel to the
dipole axis, V radially outward, and D east.  S129THET and S129PHI are colatitude relative to the H
axis and the azimuth measured from the negative V axis.


Modification History
Converted to CDAWeb Feb 2000




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SC_C9_SC00
Description
Derived from SC00 dataset in CDAW9.
Data from all CDAW9 events A-E.


Modification History
Converted to CDAWeb Feb 2000




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SC_C9_SC06
Description
Data derived from SC06 dataset in CDAW9.
Data for all CDAW9 events A-E.


Modification History
None




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SC_C9_SC08
Description
Data derived from SC08 dataset in CDAW9
Data for all CDAW9 events A-E.


Modification History
Converted to CDAWeb Feb 2000




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SC_C9_SC14
Description
Derived from SC14 dataset in CDAW9.
Data from all CDAW9 events A-E.


Modification History
None




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SC_C9_SCE0
Description
Derived from sce0 in CDAW9 DB.
Data for all CDAW9 events A-E.
The magnetic field model used to generate the BMOD parameter values was the sum of the Olsen-Pfitzer
1974 and the GRF 1979 or 1980 models.


Modification History
Conveted to CDAWeb Feb 2000




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SC_C9_SCMD
Description
Derived from SCMD dataset in CDAW9.
Data for all CDAW9 events A-E.


Modification History
Converted to CDAWeb Feb 2000




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SE_K0_AIS
Description
Ionospheric parameters derived from quarter-hourly ionograms
Ref: Grubb,RN The NOAA SEL HF Radar system (ionospheric sounder) NOAA Tech Memo 
ERL SEL-55, Space Environ Lab, Boulder, CO, 1979
Ref: Jarvis,MJ & Dudeney ,JR Reduction of ambiguities in HF radar results
through a revised receiving array & sounding pattern. Radio Sci 21, 151-158, 1986
Ref: Satellite Experiments Simultaneous with Antarctic Measurements (SESAME), 
in GGS Instrument Papers, submitted to Space Science Reviews
Info:Keith Morrison,GGS Scientist,British Antarctic Survey,Cambridge,CB3 0ET,UK
E-mail: 19989::MORRISON
QUALITY_FLAG Comprised of several additive values each with a specific meaning:-
0 okay,+1 <6 echoes used for fmin,+2 <6 echoes for fEmax,+4 <6 echoes for fFmax,
+8 fmin approx= min tx frequency,+16 fEmax approx= max tx frequency,
+32 fFmax approx= max tx  frequency (tx=transmitter)
eg 37 indicates <6 echoes used for fmin & fFmax, & fFmax approx= max tx freq


Modification History
This is first  operational version


Variable Notes

Lowest plasma frequency (-88.88=Insuf. echoes,-99.99=no echoes)
(-88.88=Insuff. echoes,-99.99=no echoes present)
Max E-region plasma frequency (-88.88=Insuf. echoes,-99.99=no echoes)
Virtual height approx<200km. -88.88=Insufficient echoes,-99.99=no echoes present
Max F-region plasma frequency (-88.88=Insuf. echoes,-99.99=no echoes)
Virtual height approx>200km. -88.88=Insufficient echoes,-99.99=no echoes present


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SE_K0_FPI
Description
Measurements made looking in South and East directions (positive) 
Ref1: Satellite Experiments Simultaneous with Antarctic Measurements (SESAME),
in GGS Instrument Papers, submitted to Space Science Reviews.
Ref2: Nature,317,p45 1985. Ref3: R.D.Stewart, PhD Thesis, Univ of Ulster, 1986
Info:Keith Morrison,GGS Scientist,British Antarctic Survey,Cambridge,CB3 0ET,UK
E-mail: 19989::MORRISON


Modification History
29-Oct-92 Changes in accordance with new Standards & Conventions document




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SE_K0_MAG
Description
H, D and Z components of the earth's magnetic field
Measuring variation of field relative to arbitrary baseline. Accurate to 1nT
1 minute data representing 'spot' values of the 1Hz sampling
Ref: Satellite Experiments Simultaneous with Antarctic Measurements (SESAME), 
in GGS Instrument Papers, submitted to Space Science Reviews
Info:Keith Morrison,GGS Scientist,British Antarctic Survey,Cambridge,CB3 0ET,UK
E-mail: 19989::MORRISON


Variable Notes

Components in cartesian HDZ coordinates 
H=Horizontal (+)North (-)South, D=Horizontal (+)East (-)West, Z=Vertical (+)Down
Magnetic field, cartesian HDZ coordinates
H=Horizontal (+)North (-)South, D=Horizontal (+)East (-)West, Z=Vertical (+)Down


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SE_K0_RIO
Description
Equivalent overhead absorption measured 45 degrees to vertical in N,S,E,W 
directions, but in an L-shell-aligned coordinate system (ie rotated 17 degrees 
anti-clockwise from geographic). Preliminary Quiet-Day Curve used.
1 minute data represent 'spot' values of the 1Hz sampling
Accurate to 0.05dB, but possible baseline uncertainties of +/-0.5dB
Ref1: The multiple riometer system at Halley, Antarctica, in 
British Antarctic Survey Bulletin, no 72, p13-23, 1986
Ref2: Satellite Experiments Simultaneous with Antarctic Measurements (SESAME), 
in GGS Instrument Papers, submitted to Space Science Reviews
Info:Keith Morrison,GGS Scientist,British Antarctic Survey,Cambridge,CB3 0ET,UK
E-mail: 19989::MORRISON




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SE_K0_VLF
Description
Omni-directional intensities in 2 narrow passband filters centred on 1kHz & 3kHz
Ref1: Satellite Experiments Simultaneous with Antarctic Measurements (SESAME),
in GGS Instrument Papers submitted to Space Science Reviews.
Ref2: VERSIM Newsletter No.4, p7 1992.
Info:Keith Morrison,GGS Scientist,British Antarctic Survey,Cambridge,CB3 0ET,UK
E-mail: 19989::MORRISON


Modification History
05-Aug-92 Changed fill values to +10.0E+30 and -2147483648
08-Oct-92 Changed DATA ENCODING to NETWORK. Added Quality and Post Gap Flags
Plotting range changed to  10-80
27-Oct-92 Put in Logical_file_id, ADID_ref, DEPEND_i, VAR_TYPE


Variable Notes

Omni-directional intensity (narrow passband filter centred on 1kHz), scalar
0dB is 10-33(Teslas)^2 / (Hertz)
Omni-directional intensity (narrow passband filter centred on 3kHz), scalar
0dB is 10-33(Teslas)^2 / (Hertz)


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SL_K0_210
Description
Reference:               Yumoto, K., Y.Tanaka, T.Oguti, K.Shiokawa, Y.Yoshimura, A.Isono,
B.J.Fraser, F.W.Menk, J.W.Lynn, M.Seto, and the 210 MM Magnetic Observation Group. Globally
coordinated magnetic observations along the 210 (deg) magnetic meridian during the STEP Period: 1.
Preliminary results of low-latitude Pc 3's, J. Geomag. Geoelectr., 44, 261-276, 1992. 
The present dataset is limited to 1-minute averages. One-second data are available but are limited
to collaborative projects  with the 210 team. Requests for these data should be addressed to the
Principal  Investigator, K. Yumoto at yumoto@geo.kyushu-u.ac.jp.


Modification History
Created 1/96


Variable Notes

Time, centered
The time given is the center point of 60 data samples, e.g., in the interval
00h01m00s - 00h01m59s, the time stamp is 00h01m30s.
Magnetic Field, 3 comp. HDZ coords (TIK)
Date of onset: 1992 August
Magnetic Field, 3 comp. HDZ coords (ZGN)
Date of onset: 1995
Magnetic Field, 3 comp. HDZ coords (YAK)
Date of onset:
Magnetic Field, 3 comp. HDZ coords (IRT)
Date of onset:
Magnetic Field, 3 comp. HDZ coords (PPI)
Date of onset: 1995
Magnetic Field, 3 comp. HDZ coords (BJI)
Date of onset:
Magnetic Field, 3 comp. HDZ coords (LNP)
Date of onset: 1994 January
Magnetic Field, 3 comp. HDZ coords (MUT)
Date of onset: 1993 July
Magnetic Field, 3 comp. HDZ coords (PTN)
Date of onset:
Magnetic Field, 3 comp. HDZ coords (WTK)
Date of onset:
Magnetic Field, 3 comp. HDZ coords (LMT)
Date of onset: 1991 August
Magnetic Field, 3 comp. HDZ coords (KAT)
Date of onset: 1995 August
Magnetic Field, 3 comp. HDZ coords (KTN)
Date of onset: 1994 October
Magnetic Field, 3 comp. HDZ coords (CHD)
Date of onset: 1992 August
Magnetic Field, 3 comp. HDZ coords (ZYK)
Date of onset: 1994 April
Magnetic Field, 3 comp. HDZ coords (MGD)
Date of onset: 1992 August
Magnetic Field, 3 comp. HDZ coords (PTK)
Date of onset: 1992 August
Magnetic Field, 3 comp. HDZ coords (MSR)
Date of onset: 1990 July.  The D- and Z-components of MSR data have a DC-level,
artificial fluctuation on a few days/year.
Magnetic Field, 3 comp. HDZ coords (ONW)
Date of onset: 1991 June
Magnetic Field, 3 comp. HDZ coords (KAG)
Date of onset: 1990 July
Magnetic Field, 3 comp. HDZ coords (CBI)
Date of onset: 1990 July
Magnetic Field, 3 comp. HDZ coords (GUA)
Date of onset: 1991 June
Magnetic Field, 3 comp. HDZ coords (YAP)
Date of onset: 1993 January
Magnetic Field, 3 comp. HDZ coords (KOR)
Date of onset: 1994 August
Magnetic Field, 3 comp. HDZ coords (BIK)
Date of onset: 1992 May
Magnetic Field, 3 comp. HDZ coords (WEW)
Date of onset: 1991 June
Magnetic Field, 3 comp. HDZ coords (DAW)
Date of onset: 1991 August
Magnetic Field, 3 comp. HDZ coords (WEP)
Date of onset: 1990 July
Magnetic Field, 3 comp. HDZ coords (BSV)
Date of onset: 1990 July.  The time of the data from BSV for Nov. 24, 1992 -
Dec. 7, 1992 is 10 hour behind the correct time. The Z-component of BSV data
sometimes becomes zero due to a temporal disconnection of cable. The time of the
data from BSV for Nov. 2, 1991 - Nov. 16, 1991 is 1 hour faster than the correct
time.
Magnetic Field, 3 comp. HDZ coords (DAL)
Date of onset: 1991 August.  The Z-component of DAL data is meaningless after
Jan. 1, 1993. The D-component of DAL data satulate for April 13, 1992 - July 10,
1992
Magnetic Field, 3 comp. HDZ coords (CAN)
Date of onset: 1994 August
Magnetic Field, 3 comp. HDZ coords (ADL)
Date of onset: 1990 July.  The Z-component of ADL data sometimes shows noisy
fluctuations due to an equipment problem.
Magnetic Field, 3 comp. HDZ coords (KOT)
Date of onset: 1993 November
Magnetic Field, 3 comp. HDZ coords (CST)
Date of onset:
Magnetic Field, 3 comp. HDZ coords (EWA)
Date of onset: 1991 January.  The H-component of EWA data sometimes shows noisy
fluctuations due to an equipment problem
Magnetic Field, 3 comp. HDZ coords (ASA)
Date of onset:
Magnetic Field, 3 comp. HDZ coords (MCQ)
Date of onset: 1992 November


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SL_K1_210
Description
Reference:               Yumoto, K., Y.Tanaka, T.Oguti, K.Shiokawa, Y.Yoshimura, A.Isono,
B.J.Fraser, F.W.Menk, J.W.Lynn, M.Seto, and the 210 MM Magnetic Observation Group. Globally
coordinated magnetic observations along the 210 (deg) magnetic meridian during the STEP Period: 1.
Preliminary results of low-latitude Pc 3's, J. Geomag. Geoelectr., 44, 261-276, 1992. 
The present dataset is limited to 1-hour averages. One-minute data are available in the K0 file.
One-second data are available but are limited to collaborative projects  with the 210 team. Requests
for these data should be addressed to the Principal  Investigator, K. Yumoto at
yumoto@geo.kyushu-u.ac.jp.


Modification History
Created 1/96


Variable Notes

Time, centered
The time given is the center point of 60 data samples, e.g., in the interval
00h01m00s - 00h01m59s, the time stamp is 00h01m30s.
Magnetic Field, 3 comp. HDZ coords (TIK)
Date of onset: 1992 August
Magnetic Field, 3 comp. HDZ coords (ZGN)
Date of onset: 1995
Magnetic Field, 3 comp. HDZ coords (YAK)
Date of onset:
Magnetic Field, 3 comp. HDZ coords (IRT)
Date of onset:
Magnetic Field, 3 comp. HDZ coords (PPI)
Date of onset: 1995
Magnetic Field, 3 comp. HDZ coords (BJI)
Date of onset:
Magnetic Field, 3 comp. HDZ coords (LNP)
Date of onset: 1994 January
Magnetic Field, 3 comp. HDZ coords (MUT)
Date of onset: 1993 July
Magnetic Field, 3 comp. HDZ coords (PTN)
Date of onset:
Magnetic Field, 3 comp. HDZ coords (WTK)
Date of onset:
Magnetic Field, 3 comp. HDZ coords (LMT)
Date of onset: 1991 August
Magnetic Field, 3 comp. HDZ coords (KAT)
Date of onset: 1995 August
Magnetic Field, 3 comp. HDZ coords (KTN)
Date of onset: 1994 October
Magnetic Field, 3 comp. HDZ coords (CHD)
Date of onset: 1992 August
Magnetic Field, 3 comp. HDZ coords (ZYK)
Date of onset: 1994 April
Magnetic Field, 3 comp. HDZ coords (MGD)
Date of onset: 1992 August
Magnetic Field, 3 comp. HDZ coords (PTK)
Date of onset: 1992 August
Magnetic Field, 3 comp. HDZ coords (MSR)
Date of onset: 1990 July.  The D- and Z-components of MSR data have a DC-level,
artificial fluctuation on a few days/year.
Magnetic Field, 3 comp. HDZ coords (ONW)
Date of onset: 1991 June
Magnetic Field, 3 comp. HDZ coords (KAG)
Date of onset: 1990 July
Magnetic Field, 3 comp. HDZ coords (CBI)
Date of onset: 1990 July
Magnetic Field, 3 comp. HDZ coords (GUA)
Date of onset: 1991 June
Magnetic Field, 3 comp. HDZ coords (YAP)
Date of onset: 1993 January
Magnetic Field, 3 comp. HDZ coords (KOR)
Date of onset: 1994 August
Magnetic Field, 3 comp. HDZ coords (BIK)
Date of onset: 1992 May
Magnetic Field, 3 comp. HDZ coords (WEW)
Date of onset: 1991 June
Magnetic Field, 3 comp. HDZ coords (DAW)
Date of onset: 1991 August
Magnetic Field, 3 comp. HDZ coords (WEP)
Date of onset: 1990 July
Magnetic Field, 3 comp. HDZ coords (BSV)
Date of onset: 1990 July.  The time of the data from BSV for Nov. 24, 1992 -
Dec. 7, 1992 is 10 hour behind the correct time. The Z-component of BSV data
sometimes becomes zero due to a temporal disconnection of cable. The time of the
data from BSV for Nov. 2, 1991 - Nov. 16, 1991 is 1 hour faster than the correct
time.
Magnetic Field, 3 comp. HDZ coords (DAL)
Date of onset: 1991 August.  The Z-component of DAL data is meaningless after
Jan. 1, 1993. The D-component of DAL data satulate for April 13, 1992 - July 10,
1992
Magnetic Field, 3 comp. HDZ coords (CAN)
Date of onset: 1994 August
Magnetic Field, 3 comp. HDZ coords (ADL)
Date of onset: 1990 July.  The Z-component of ADL data sometimes shows noisy
fluctuations due to an equipment problem.
Magnetic Field, 3 comp. HDZ coords (KOT)
Date of onset: 1993 November
Magnetic Field, 3 comp. HDZ coords (CST)
Date of onset:
Magnetic Field, 3 comp. HDZ coords (EWA)
Date of onset: 1991 January.  The H-component of EWA data sometimes shows noisy
fluctuations due to an equipment problem
Magnetic Field, 3 comp. HDZ coords (ASA)
Date of onset:
Magnetic Field, 3 comp. HDZ coords (MCQ)
Date of onset: 1992 November


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SN_K0_GISR
Description
Article describing equipment is: GRL, Vol. 10, No. 11, pp. 1112-1115, 1983.
The gate number is an independent variable that does not depend on time.
The maximum number of gates is a constant within each file.
The dependent variables depend on the gate number and on time.
The units for normalized power are number/(cubic meter).
Thus the units for normalized power are the same as for electron density.
Typical range of electron number density: 10^4 to 10^6 /cm^3
Typical range of electron temperature: 1500 to 3000 deg K
Typical range of ion temperature: 1000 to 2500 deg K
Typical range of line-of-sight ion velocity: 0.5 to 2 km/s
Both boiTime and eoiTime are expressed as single long integers.
Their format is hhmmsss where sss is given in tenths of seconds.


Modification History
No mods thus far.




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SN_K1_GISR
Description
Article describing equipment is: GRL, Vol. 10, No. 11, pp. 1112-1115, 1983.
The gate number is an independent variable that does not depend on time.
The maximum number of gates is a constant within each file.
The dependent variables depend on the gate number and on time.
The units for normalized power are number/(cubic meter).
Thus the units for normalized power are the same as for electron density.
Typical range of electron number density: 10^4 to 10^6 /cm^3
Typical range of electron temperature: 1500 to 3000 deg K
Typical range of ion temperature: 1000 to 2500 deg K
Typical range of line-of-sight ion velocity: 0.5 to 2 km/s
Both boiTime and eoiTime are expressed as single long integers.
Their format is hhmmsss where sss is given in tenths of seconds.


Modification History
No mods thus far.




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SO_AT_DEF
Description
Data: 10 minute intervals


Modification History
5/6/94 - Original Implementation
1/25/96 - Added SARVariables for CCR 2189




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SO_H0_CST
Description
LION>Low energy ION and Electron instrument




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SO_HK_CST
Description
LION>Low energy ION and Electron instrument




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SO_K0_CELS
Description
Data entry every 5 minutes
A description of the CELIAS instrument and scientific scope can be found on WWW
athttp://ubeclu.unibe.ch/phim/ms/soho/or on the SOHO homepage http://sohowww.nascom.nasa.gov/


Modification History
created Dec 1993
Modified by JT on 9/21/94
Modified by PW on 2/Mar/95
Modified by PW on 21/Jul/95
Modified by PW on 18/Aug/95




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SO_K0_CST
Description
Data: 5 minute averages Time tag = center of interval 
References                    1.Kunow, H., et al., COSTEP -   Comprehensive Suprathermal and 
Energetic Particle Analyser for SOHO, in V. Domingo, editor, The SOHO Mission - Scientific and 
Technical Aspects of the        Instruments, ESA SP-1104, pages 75 - 80, 1988 
2.Kunow, H., et al., COSTEP -  Comprehensive Suprathermal and  Energetic Particle Analyser for SOHO
- Scientific Goals and Data Description, Proc. First SOHO  Workshop, ESA SP-348,           pages 43
- 46, 1992 
2.Mueller-Mellin, R., et al.,  COSTEP -                        Comprehensive Suprathermal and 
Energetic Particle Analyser,    to be published in              Solar Physics, 1995
 19 Dec 1996 Caveat: 1. The EPHIN E-detector developed gradually a noise problem during 1996 and was
switched off logically on 1996-305-14.40. Check EPHIN status word >Ephin_Stat< bit 2 (2^2): if set
to one: E detector  is on, if set to zero, E detector is off. When off, the channels E3000, P41 and
H41 show zero intensity, the energy of the next lower channel E1300 is the average of E1300 and
E3000, the width of channel E1300 is the sum of the  width E1300 and E3000; P25, and H25 are changed
accordingly.  Note: the KPGS calulates correctly the new fluxes in channels E1300, P25, H25. Only
their interpretation needs to be changed by the user. 2. The geometric factor for the counting rate
channels can be changed either by ground command or autonomously by detecting high fluxes in the
center segment of detector A. Check EPHIN status word >Ephin_Stat<bits 9,10,11,12,13,17,18,19,20,21:
if set to one: large geometric factor, if set to zero: small geometric factor. Note: the KPGS
software calculates correctly the fluxes. No action needed by the user.


Modification History
 15 Feb 1994    Version  1.0 
 22 Nov 1994    Version  1.0                     Revision 1.0      new variables COVER, DQF, STATUS
 28 Mar 1995    Version  1.0                     Revision 2.0      Energy ranges updated           
 15 May 1995    Version  1.0                     Revision 3.0      Addition: TEXT                  
Correction: E_Energy [4]                     P_Energy [2]                     P_Label             
 28 Nov 1995  Version  1.0.                    Revision 4.0        Correction: # Var. from 24 to 25
Change: Descript. COST -> CST       Var_type data -> support_data         at: Epoch, PB5            
      at:  E_energy,  E_delta          at:  P_energy,  P_delta          at: He_energy, He_delta     
    at: E_energy, E_delta  
 19 Dec 1996  Version  7.0. EPHIN E, P and He channel values adapted to new investigations to
geometry factors




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SO_K0_ERN
Description
Data: 1 minute avarages Time tag = center of interval
Torsti et al.: ERNE - Energetic and Relativistic Nuclei and Electron experiment, The SOHO Mission
ESA SP-1104, 1988
Torsti et al.: Energetic Particle Experiment ERNEto be published in SolarPhysics, 1995
M. Lumme and Eino Valtonen: CEPAC Experiment Operations Manual, November 1994 
ERNE WWW Home page  http://helium.srl.utu.fi/erne.html


Modification History
Version 01 19-Nov-1995. Modified by JT on Dec. 4, 1995




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SO_OR_DEF
Description
TBS


Modification History
Originated Monday, May 13, 1991
Modified June 13, 1991 for version 2.1
Modified October 2,1991 for new global attributes, incr sizes
Modified 11/11/91 Add sun vector, replace space id with support id
Modified 1992 Feb 11 to use the variable name TIME and type CDF_INT4 instead of 
EPOCH and CDF_EPOCH for the time tags CCR 490
Modified 6/2/92 add project, discipline, source_name, data_version, title, and 
mods to global section; add validmin, validmax, labl_ptr_1 and monoton 
attributes to some variables; put epoch time back in, rename time to 
time_pb5; add label_time to variables
Modified 11/07/92 to use Epoch and Time_PB5 variable name
Modified 6/2/93 add ADID_ref and Logical_file_id
7/5/94 - CCR ISTP 1852 updated CDHF skeleton to CDF standards - JT
9/21/94 - Added 24 new global attributes to log the ephemeris 
comparison summary report from the definitive FDF orbit file.  CCR 1932
11/7/94 - Merged CCR 1852 changes and corrected errors 
made in CCR 1852.  ICCR 1884
12/7/94 - Modified MODS to follow ISTP standards.  ICCR 1885
01/05/95 - add heliocentric coordinate system.  CCR 1889
2/28/95 - added COMMENT1 and COMMENT2 for CCR 
11/03/95 - deleted crn_space for CCR 2154 - RM




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SO_OR_PRE
Description
TBS


Modification History
Originated Monday, May 13, 1991
Modified June 13, 1991 for version 2.1
Modified October 2,1991 for new global attributes, incr sizes
Modified 11/11/91 Add sun vector, replace space id with support id
Modified 1992 Feb 11 to use the variable name TIME and type CDF_INT4 instead of 
EPOCH and CDF_EPOCH for the time tags CCR 490
Modified 6/2/92 add project, discipline, source_name, data_version, title, and 
mods to global section; add validmin, validmax, labl_ptr_1 and monoton 
attributes to some variables; put epoch time back in, rename time to 
time_pb5; add label_time to variables
Modified 11/07/92 to use Epoch and Time_PB5 variable name
Modified 6/2/93 add ADID_ref and Logical_file_id
7/5/94 - CCR ISTP 1852 updated CDHF skeleton to CDF standards - JT
9/21/94 - Added 24 new global attributes to log the ephemeris 
comparison summary report from the definitive FDF orbit file.  CCR 1932
11/7/94 - Merged CCR 1852 changes and corrected errors 
made in CCR 1852.  ICCR 1884
12/7/94 - Modified MODS to follow ISTP standards.  ICCR 1885
01/05/95 - add heliocentric coordinate system.  CCR 1889
2/28/95 - added COMMENT1 and COMMENT2 for CCR 
11/03/95 - deleted crn_space for CCR 2154 - RM




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SX_K0_30F
Description


Variable Notes

ACS control mode
0=sunpoint; 1=mag_cal; 2=orb_rotation 3=coast
6 LICA flags
For each of 6 flags, 0 means gooddata. But F1=1: LICA off; F2=1:
calibrationtime; F3=1: excessive HV;F4=1: some noisy-SSD data; F5=1:some
noisy-MCP data; F6=1: some abnormality.When F1 or F2 or F3 or F6 is 1, data is a
fill value.
7 HILT flags 
For each of 7 flags, 0=good data.But, F1=1: HILT off; F2=1: calibrationtime;
F3=1: some noisy 4-9 MeV/n data;F4=1: some noisy 9-38 MeV/n data;F5=1: some
noisy 8-42 MeV/n data;F6=1: some noisy 41-220 MeV/n data;F7=1: abnormal time.
When F1 or F2or F7 is 1, data is fill value.
4 MAST flags
For each of 4 flagss, 0=good data.But F1=1: Mast off; F2=1: calibrationtime;
F3=1: abnormal time; F4=1 somenoisy data. If F1 or F2 or F3 is 1,data is a fill
value.
4 PET flags
For each of the 4 flags, 0=good dataBut F1=1: PET off; F2=1: calibrationtime;
F3=1: abnormal time; F4=1: somenoisy data. When F1 or F2 or F3 is 1,data is a
fill value.
Z>2 dif fluxes, 9 channels (0.5-220 MeV/nu)from LICA,HILT,and MAST detectors
L_ = LICA; H_ = HILT; M_ = MAST. L_hipri(0.49-8.3 MeV/nu);_H_hz1(8.2-42
Mev/nu);M_hizr1(19.3-22.8 MeV/nu;_hizr2(22.8-31.0
MeV/nu);_hizr3(31.0-51.7);_hizr4(51.7-76.2 MeV/nu;_hizr5(76.2-113
MeV/nu);_hizr6(113-156 MeV/nu);H_hz2(42-220 MeV/nu)
He Dif Fluxes, 4 channels (0.5-38 MeV/nu): from LICA, HILT, and MAST detectors
L_ = LICA; H_ = HILT; M_ = MAST. L_lopri(0.5-6.6 MeV/nu);H_he1(4-9
MeV/nu);M_z2(8-15 MeV/nu);H_he2(9-38 MeV/nu)
H+ (mainly) Dif Fluxes, 2 channels: from MAST and PET detectors
M_ = MAST; P_ = PET: M_m12(5-12 MeV/nu);P_plo(19-27 MeV/nu).Fluxes are mainly
H+.
Electr Dif Fluxes, 2 channels (1.5-14 MeV)from PET instrument.
pet_elo(1.5-6 MeV);pet_ehi(2.5-14 MeV)
Integral Flux, E- or H from LICA.E>0.6 MeV electrons and/or E>0.8 MeV protons
Data from lica_ssd channel
Sigma:Z>2 dif fluxes, 9 channels (0.5-220 MeV/nu)from LICA,HILT,and MAST detectors
L_ = LICA; H_ = HILT; M_ = MAST. All in meV/nu.
L_hipri_sigma(0.49-8.3MeV/nu);_H_hz1_sigma(8.2-42);M_hizr1_sigma(19.3-22.8;_hizr
2_sigma(22.8-31.0);_hizr3_sigma(31.0-51.7);_hizr4_sigma(51.7-76.2);_hizr5_sigma(
76.2-113);_hizr6_sigma(113-156);H_hz2_sigma(42-220)
Sigma: He Dif Fluxes, 4 channels;(0.5-38 MeV/nu):from LICA, HILT, and MAST detectors
L_ = LICA; H_ = HILT; M_ = MAST. All in MeV/nu.
L_lopri_sigma(0.5-6.6MeV/nu);H_he1_sigma(4-9);M_z2_sigma(8-15);H_hz2_sigma
Sigma: H+ (mainly) Dif Fluxes, 2 channels:from MAST and PET detectors
M_ =MAST; P_ =PET: M_m12_sigma(5-12);P_plo_sigma(19-27). All in MeV.
Sigma: Electr Dif Fluxes, 2 channels;(2-16 MeV) from PET instrument.
pet_elo_sigma (1.5-6 MeV);pet_ehi_sigma (2.5-14 MeV)
Sigma: Integral Flux, E- or H from LICA.E>0.6 MeV electrons and/orE>0.8 MeV protons
Sigma from LICA_ssd_sigma


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SX_K0_POF
Description


Variable Notes

Polarcap entry: mm/dd/yyyy hh:mm:ss
This is the time the s/c enteredpolarcap at 70 deg inva-lat; the datais averaged
over the next few minutes i.e, until the exit time. Occasionally,the trajectory
may miss the polarcap.
4 LICA quality/saturation flags.
For all flags 0 means perfect data.But 1 is an advisory to look intothe 30-s
flux data: PARTIAL '1' means some 30-s data were eliminated;BAD '1' means bad or
no data and entryis a fill value; SSD_SAT '1' means that a small amount of
saturatedSSD data is admitted; MCP_SAT '1' signifies that a small amount of
saturated MCP  data is admitted.So called 'Saturation' simply meansthat the
count rates in the SolidState Detectors or the Micro ChannelPlates exceeded the
calibrating ratesof 10,000 counts/s during any 30-s.
6 HILT quality flags.
If entry is '0', data is perfect. But  '1' is advisory to look into 30-sflux
data: PARTIAL '1' signifies thatsome 30-s values were ignored; BAD '1' signifies
bad/no data and entry is afill value. All flags with SAT in namesignifies that
some saturated 30-s fluxes were admitted in the correspondingenergy channel. So
called 'saturation' merely connotes that the count rate inthat energy channel
had exceeded thecalibration rate of 10,000/s
3 MAST quality flags
MAST flags: If '0' data is perfect But '1' is advisory to look into 30-sfluxes.
PARTIAL '1' signifies thatsome 30-s fluxes were omitted;BAD '1' signifies bad or
no data withentries being fill values. ADC_SATsignifies that count data mayhave
had saturated values. 'Saturation' only means that the count rate inany or all
channels exceeded thecalibration count rate of 10,000/s
3 PET quality flag
If flag is '0' data is perfect; if '1' it is advisable to look into the30-s
fluxes: PARTIAL '1' signifiesthat some 30-s data were omitted;BAD '1' signifies
bad/absent data,with fill value as the entry;P1HI_SAT '1' signifies that
somesaturated values. 'Saturation' simplymeans that the count rates exceededthe
calibration counts of 10,000/s.
Z>2 dif fluxes, 9 channels (0.5-220 MeV/nu)from LICA, HILT,and MAST detectors
L_ = LICA; H_ = HILT; M_ = MAST. L_hipri(0.49-8.3 MeV/nu);_H_hz1(8.2-42
Mev/nu);M_hizr1(19.3-22.8 MeV/nu;_hizr2(22.8-31.0
MeV/nu);_hizr3(31.0-51.7);_hizr4(51.7-76.2 MeV/nu;_hizr5(76.2-113
MeV/nu);_hizr6(113-156 MeV/nu);H_hz2(42-220 MeV/nu)
He Dif Fluxes, 4 channels (0.5-38 MeV/nu); from LICA, HILT, and MAST detectors
L_ = LICA; H_ = HILT; M_ = MAST. L_lopri(0.5-6.6 MeV/nu);H_he1(4-9
MeV/nu);M_z2(8-15 MeV/nu);H_he2(9-38 MeV/nu)
H+ (mainly) Dif Fluxes, 2 channels:from MAST and PET detectors
M_ = MAST; P_ = PET: M_m12(5-12 MeV/nu);P_plo(19-27 MeV/nu)
Electr Dif Fluxes, 2 channels (1.5-14 MeV)from PET instrument.
pet_elo(1.5-6 MeV);pet_ehi(2.5-14 MeV)
Integral Flux, E- or H from LICA.E>0.6 MeV electrons and/or E>0.8 MeV protons
Data from lica_ssd channel
Sigma:Z>2 dif fluxes, 9 channels (0.5-MeV/nu)from LICA,HILT,and MAST detectors
L_ = LICA; H_ = HILT; M_ = MAST. All in meV/nu.
L_hipri_sigma(0.49-8.3MeV/nu);_H_hz1_sigma(8.2-42);M_hizr1_sigma(19.3-22.8;_hizr
2_sigma(22.8-31.0);_hizr3_sigma(31.0-51.7);_hizr4_sigma(51.7-76.2);_hizr5_sigma(
76.2-113);_hizr6_sigma(113-156);H_hz2_sigma(42-220)
Sigma: He Dif Fluxes, 4 channels;(0.5-38 MeV/nu):from LICA, HILT, and MAST detectors
L_ = LICA; H_ = HILT; M_ = MAST. All in MeV/nu.
L_lopri_sigma(0.5-6.6MeV/nu);H_he1_sigma(4-9);M_z2_sigma(8-5);H_hz2_sigma(41-110
Sigma: H+ (mainly) Dif Fluxes, 2 channels:from MAST and PET detectors
M_ =mast; P_ =pet: M_m12_sigma(5-12);P_plo_sigma(19-27). All in MeV.
Sigma: Electr Dif Fluxes, 2 channels;(1.5-14 MeV) from PET instrument.
pet_elo_sigma (1.5-6 MeV);pet_ehi_sigma (2.5-14 MeV)
Sigma: Integral Flux, E- or H from LICA.E>0.6 MeV electrons and/orE>0.8 MeV protons
Sigma from LICA_ssd_sigma


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T1_ED_EP
Description
CDFs from the 3 s/c 1982-019A, 1984-037A and 1984-129A are identical in form. Th
ere are 4 detectors: low energy electrons (LOE), high energy  electrons (HIE), e
ach with 6 energy ranges; and LOP and HIP for protons, with 10 and 16 energy ran
ges (only the 1st 6 or 7 of HIP are useful).  For LOE, HIE, and LOP, each range
is from a lower energy level up to the detector maximum--an integrated energy.
For example, the 1st two LOE ranges are 30-300 keV and 45-300 keV. The 30-45 keV
 range is thus the difference between the two measurements.  For low levels, bac
kground is significant, and measurements for a detector may not be strictly mono
tonic for any individual 10-s average.  In such cases, the differential flux is
made 0 for energies above the non-monotonic flux. 6 HIE fluxes are stacked after
 6 LOE fluxes in S019DJE. Low edge of each energy bin is in S019EEN and bands ar
e contiguous, so 1st bin is 30-45 keV. Band 6 is top band of LOE (200-300 keV),
same as band 7 (lowest energy of HIE).  Topmost energy is 2000 keV.  The 5 chann
els marked 1996-2000 keV are fill values only. 10 LOP channels are in elements 1
-9 and 11 of S019DJP and the 1st 7 HIP channels are in elements 10 and 12-17, so
 ranges increase monotonically. Low edge of energy bin is in S019PEN; upper edge
 is value of the bin above it except bins 9-11 have ranges .377-.462, .37-.52, a
nd .462-.600 MeV. Topmost energy bin is 1.7-2.2 MeV. For time history of the dat
a, plot flux from S019DJE or S019DJP vs time, and filter on S019EEN or S019PEN t
o select the channel.  Energy spectrum: make an XY plot of S019DJE vs S019EEN (f
or electrons), filtered on desired time. For successive spectra (spectra are ava
ilable every 10-s), use Animation. Direction cosines for H, V, D are with respec
t to dipole-meridian coordinates: H is parallel to the dipole axis, V radially o
utward, and D east.  S019THET and S019PHI are colatitude relative to the H axis
and the azimuth measured from the negative V axis. Longitudes:  S019: 322 E;   S
037: 70 E;   S129: 205 E A simplified subset of these data is available in SA19.


Modification History




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T2_ED_EP
Description
CDFs from the 3 s/c 1982-019A, 1984-037A and 1984-129A are identical in form. Th
ere are 4 detectors: low energy electrons (LOE), high energy  electrons (HIE), e
ach with 6 energy ranges; and LOP and HIP for protons, with 10 and 16 energy ran
ges (only the 1st 6 or 7 of HIP are useful).  For LOE, HIE, and LOP, each range 
is from a lower energy level up to the detector maximum--an integrated energy.  
For example, the 1st two LOE ranges are 30-300 keV and 45-300 keV. The 30-45 keV
 range is thus the difference between the two measurements.  For low levels, bac
kground is significant, and measurements for a detector may not be strictly mono
tonic for any individual 10-s average.  In such cases, the differential flux is 
made 0 for energies above the non-monotonic flux. 6 HIE fluxes are stacked after
 6 LOE fluxes in S037DJE. Low edge of each energy bin is in S037EEN and bands ar
e contiguous, so 1st bin is 30-45 keV. Band 6 is top band of LOE (200-300 keV), 
same as band 7 (lowest energy of HIE).  Topmost energy is 2000 keV.  The 5 chann
els marked 1996-2000 keV are fill values only. 10 LOP channels are in elements 1
-9 and 11 of S037DJP and the 1st 7 HIP channels are in elements 10 and 12-17, so
 ranges increase monotonically.  Low edge of energy bin is in S037PEN; upper edg
e is value of the bin above it except bins 9-11 have ranges .35-.45, .38-.49, an
d .45-.56 MeV. Topmost energy bin is 1.8-2.3 MeV. For time history of the data, 
plot flux from S037DJE or S037DJP vs time, and filter on S037EEN or S037PEN to s
elect the channel.  Energy spectrum: make an XY plot of S037DJE vs S037EEN (for 
electrons), filtered on desired time. For successive spectra (spectra are availa
ble every 10-s), use Animation. Direction cosines H, V, D, S037THET and S037PHI 
have spurious values for S037. Longitudes:  S019: 322 E;   S037: 70 E;   S129: 2
05 E A simplified subset of these data is available in SA37.


Modification History




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T3_ED_EP
Description
CDFs from the 3 s/c 1982-019A, 1984-037A and 1984-129A are identical in form. Th
ere are 4 detectors: low energy electrons (LOE), high energy  electrons (HIE), e
ach with 6 energy ranges; and LOP and HIP for protons, with 10 and 16 energy ran
ges (only the 1st 6 or 7 of HIP are useful).  For LOE, HIE, and LOP, each range 
is from a lower energy level up to the detector maximum--an integrated energy.  
For example, the 1st two LOE ranges are 30-300 keV and 45-300 keV. The 30-45 keV
 range is thus the difference between the two measurements.  For low levels, bac
kground is significant, and measurements for a detector may not be strictly mono
tonic for any individual 10-s average.  In such cases, the differential flux is 
made 0 for energies above the non-monotonic flux. 6 HIE fluxes are stacked after
 6 LOE fluxes in S129DJE. Low edge of each energy bin is in S129EEN and bands ar
e contiguous, so 1st bin is 30-45 keV. Band 6 is top band of LOE (200-300 keV), 
same as band 7 (lowest energy of HIE).  Topmost energy is 2000 keV.  The 5 chann
els marked 1996-2000 keV are fill values only. 10 LOP channels are in elements 1
-9 and 11 of S129DJP and the 1st 7 HIP channels are in elements 10 and 12-17, so
 ranges increase monotonically.  Low edge of energy bin is in S129PEN; upper edg
e is value of the bin above it except bins 9-11 have ranges .365-.457, .36-.48, 
and .457-.573 MeV.  Topmost energy bin is 1.80-2.05 MeV. For time history of the
 data, plot flux from S129DJE or S129DJP vs time, and filter on S129EEN or S129P
EN to select the channel.  Energy spectrum: make an XY plot of S129DJE vs S129EE
N (for electrons), filtered on desired time. For successive spectra (spectra are
 available every 10-s), use Animation. Direction cosines H, V, D, S129THET and S
129PHI  have spurious values for S129. Longitudes:  S019: 322 E;   S037: 70 E;  
 S129: 205 E. A simplified subset of these data is available in SA29.


Modification History




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UY_H0_GLG
Description
The Ulysses/SWICS instrument is a mass spectrometer combining an 
electrostatic analyzer with post acceleration, followed by a time-of-flight 
and energy measurement. The instrument covers an energy per charge range 
from 0.16 to 59.6 keV/e with a time resolution of about 13 minutes.
SWICS is designed to determine uniquely the elemental and ionic-charge 
composition, the temperatures and mean speeds of all major solar wind ions, 
from H through Fe. For more information see G. Gloeckler, J. Geiss et al., 
Astron. Astrophys. Suppl. Ser. 92, 267-289, 1992.
This archive consists of all 18 Matrix Rates (MR) as a function of energy 
per charge (E/q) and of time. Each MR represents a specific element in one 
or several ionization states, but it may also contain significant 
contributions from neighbouring elements due to spillover. The MRs are given 
in units of count rates only. The accompanying SAPRO (SWICS Archive 
Processor) software can be used both to convert the MR count rates to 
physical units (differential flux, phase space density), to correct for 
spillover between different MRs, and to obtain kinetic parameters (density, 
speed, thermal speed) of selected ions (to be used with caution).


Modification History
1999-01-12: Initial CDF data file creation


Variable Notes

Instrument cycle start time in SCET format
Spacecraft Event Time (SCET) measured in sec. since 1-Jan-1950.
Post gap flag: 0 = no gap immediately prior to this record (see notes)
Post gap flag:  0 = no gap immediately prior to this record, 1 = prior gap due
to inappropriate instrument mode, 2 = prior gap due to missing level zero data,
3 = prior gap due to noisy level zero data, 10-255 = reserved
Deflection voltage cycle non nominal flag, no bit set = nominal (see notes)
Deflection voltage cycle non nominal flag bitmask: no bit set = all nominal, bit
 0 set = DPU error - no sun puls, bit  1 set = DPU error - sun puls not within
sun pulse sector, bit  2 set = DPU error - MCD address wrong, bit  3 set = DPU
error - no spin rate, bit  4 set = DPU error - no bubble sync. word, bit  5 set
= DPU error - no bubble HK identifier, bit  6 set = DPU error - interrupt error
2, bit  7 set = DPU error - interrupt error 1, bit  8 set = DPU error -
formating error, bit  9 set = DPU error - PHA error, bit 10 set = DPU error -
mode status error, bit 11 set = non nominal matrix rate value (i.e. matrix rate
overflow), bit 12 set = non nominal DV mode (i.e. DV mode != 1), bit 13 set =
non nominal PAPS value (i.e. PAPS value != 22.6), bit 14 set = non nominal MCP
bias power supply level (i.e. MCP level != 3), bit 15 set = non nominal
emergency mode (i.e. emergency mode enabled), bit 16 set = non nominal DPU mode
(i.e. DPU mode != 0), bit 17 set = non nominal TAC gain adjustment (i.e. TAC
gain != 0%), bit 18 set = non nominal DV stepping (i.e. step reversal), bit 19
set = non nominal aspect angle (i.e. not within range: ]0.0 .. 50.0[), bit 20
set = non nominal ADC trigger type (i.e. trigger type != T), bit 21-31  =
reserved (not set)
Instrument status flag (see notes)
Instrument status flag bitmask: bit  0-13: reserved (not set), bit 14-15 (2
bit): telemetry mode, bit 16-19 (4 bit): TAC gain adjustment, bit    20 (1 bit):
data compression code, bit 21-22 (2 bit): emergency mode, bit 23-26 (4 bit): MCP
bias power supply level, bit 27-29 (3 bit): DV mode, bit 30-31 (2 bit): DPU mode
Instrument Step duration
Instrument Step duration is 12 seconds, with few exceptions.


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UY_M0_AT1
Description
This data set contains 10 minute 
averages of the proton and Z>=1 
flux data from the Ulysses 
Cosmic Ray and Solar Particle 
Investigation Anisotropy Telescope 1. 
Flux units are /cm2/s/sr/Mev. 
Data Set Contact: S Dalla, 
Space & Atmospheric Physics Group, 
Imperial College, London, UK.
Principal Investigator: R B McKibben, 
Laboratory for Astrophysics and Space 
Research, Enrico Fermi Institute, 
University of Chicago, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 365-399 (1992). 
Relevant web sites: 
ftp://odysseus.uchicago.edu/WWW/Simpson/Ulysses.html
http://www.sp.ph.ic.ac.uk/Ulysses/


Modification History
TBD




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UY_M0_AT2
Description
This data set contains 10 minute 
averages of the proton and Z>=1 
flux data from the Ulysses 
Cosmic Ray and Solar Particle 
Investigation Anisotropy Telescope 2. 
Flux units are /cm2/s/sr/Mev. 
Data Set Contact: S Dalla, 
Space & Atmospheric Physics Group, 
Imperial College, London, UK.
Principal Investigator: R B McKibben, 
Laboratory for Astrophysics and Space 
Research, Enrico Fermi Institute, 
University of Chicago, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 365-399 (1992). 
Relevant web sites: 
ftp://odysseus.uchicago.edu/WWW/Simpson/Ulysses.html
http://www.sp.ph.ic.ac.uk/Ulysses/


Modification History
TBD




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UY_M0_BAE
Description
This data set contains 3 to 22 minute 
averages of the electron density and 
temperature data from the 
Ulysses Solar Wind Observations Over 
the Poles of the Sun instrument. 
Density units are /cm3, temperature 
units are K. 
Data Set Contact: B E Goldstein, 
NASA Ames Research Center, USA. 
Principal Investigator: D J McComas, 
Southwest Research Institute, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 237-265 (1992).
Relevant Web Sites: 
http://sst.lanl.gov/nis-projects/swoops/


Modification History
TBD




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UY_M0_BAI
Description
This data set contains 4 to 8 minute 
averages of the ion density, 
temperature and velocity data from the 
Ulysses Solar Wind Observations Over 
the Poles of the Sun instrument. 
Density units are /cm3, temperature 
units are K, velocity units are km/s. 
Data Set Contact: B E Goldstein, 
NASA Ames Research Center, USA. 
Principal Investigator: D J McComas, 
Southwest Research Institute, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 237-265 (1992).
Relevant Web Sites: 
http://sst.lanl.gov/nis-projects/swoops/


Modification History
TBD




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UY_M0_HET
Description
This data set contains 10 minute 
averages of the proton, electron, and 
Z>=3 count rate data from the Ulysses 
Cosmic Ray and Solar Particle 
Investigation High Energy Telescope. 
Count rate units are /s. 
Data Set Contact: R B McKibben, 
Laboratory for Astrophysics and Space 
Research, Enrico Fermi Institute, 
University of Chicago, USA.
Principal Investigator: R B McKibben, 
Laboratory for Astrophysics and Space 
Research, Enrico Fermi Institute, 
University of Chicago, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 365-399 (1992).
Relevant Web Sites: 
ftp://odysseus.uchicago.edu/WWW/Simpson/Ulysses.html
ftp://odysseus.uchicago.edu/WWW/Simpson/UlyDocs/HET.html


Modification History
TBD




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UY_M0_HFT
Description
This data set contains 10 minute 
averages of the ion flux data from the 
Ulysses Cosmic Ray and Solar Particle 
Investigation High Flux Telescope. 
Flux units are /cm2/s/sr. 
Data Set Contact: J D Anglin, 
Herzberg Institute for Astrophysics, 
National Research Council of Canada, 
Ottawa, Canada.
Principal Investigator: R B McKibben, 
Laboratory for Astrophysics and Space 
Research, Enrico Fermi Institute, 
University of Chicago, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 365-399 (1992).
Relevant Web Sites: 
ftp://odysseus.uchicago.edu/WWW/Simpson/Ulysses.html
For a fuller description of the data 
channels and their energy levels see 
the format file at 
file://helio.estec.esa.nl/ulysses/cospin/hft/doc/
 and Anglin et al., J. Geophys. Res., 
 102, 1 (1997).


Modification History
TBD




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UY_M0_KET
Description
This data set contains 10 minute 
averages of the proton, helium, 
and electron count rate data from the
Ulysses Cosmic Ray and Solar Particle 
Kiel Electron Telescope. 
Count rate units are /s. 
Data Set Contact: B Heber, 
CEA, DSM, Service d'Astrophysique, 
Centre d'Etudes de Saclay,
91191 Gif sur Yvette, Cedex, France.
Principal Investigator: R B McKibben, 
Laboratory for Astrophysics and Space 
Research, Enrico Fermi Institute, 
University of Chicago, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 365-399 (1992).
Relevant Web Sites: 
ftp://odysseus.uchicago.edu/WWW/Simpson/Ulysses.html
http://www.ifctr.mi.cnr.it/Ulysses/


Modification History
TBD




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UY_M0_LET
Description
This data set contains 10 minute 
averages of the ion and electron 
flux data from the Ulysses 
Cosmic Ray and Solar Particle 
Investigation Low Energy Telescope. 
Flux units are /cm2/s/sr/Mev. 
Data Set Contact: T R Sanderson, 
Solar System Division, ESA/ESTEC.
Principal Investigator: R B McKibben, 
Laboratory for Astrophysics and Space 
Research, Enrico Fermi Institute, 
University of Chicago, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 365-399 (1992).
Relevant Web Sites: 
ftp://odysseus.uchicago.edu/WWW/Simpson/Ulysses.html
http://helio.estec.esa.nl/ssd/let.html


Modification History
TBD




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UY_M0_PFRA
Description
This data set contains 10 minute 
averages of the average 
electric field intensities from the 
Unified Radio and Plasma Wave 
Instrument Plasma Frequency Receiver.
Units are microVolt/Hz**0.5.
Data Set Contact: R Hess, 
NASA Goddard Spaceflight Center, 
Greenbelt, Maryland, USA.
Principal Investigator: R J Macdowall, 
NASA Goddard Spaceflight Center, 
Greenbelt, Maryland, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 291-316 (1992).
Relevant Web Sites: 
http://urap.gsfc.nasa.gov/www/home.html


Modification History
TBD




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UY_M0_PFRP
Description
This data set contains 10 minute 
averages of the peak 
electric field intensities from the 
Unified Radio and Plasma Wave 
Instrument Plasma Frequency Receiver.
Units are microVolt/Hz**0.5.
Data Set Contact: R Hess, 
NASA Goddard Spaceflight Center, 
Greenbelt, Maryland, USA.
Principal Investigator: R J Macdowall, 
NASA Goddard Spaceflight Center, 
Greenbelt, Maryland, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 291-316 (1992).
Relevant Web Sites: 
http://urap.gsfc.nasa.gov/www/home.html


Modification History
TBD




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UY_M0_R144
Description
This data set contains 144 second 
averages of the electric field 
intensities from the 
Unified Radio and Plasma Wave 
Instrument Radio Astronomy Receiver.
Units are microVolt/Hz**0.5.
Data Set Contact: R Hess, 
NASA Goddard Spaceflight Center, 
Greenbelt, Maryland, USA.
Principal Investigator: R J Macdowall, 
NASA Goddard Spaceflight Center, 
Greenbelt, Maryland, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 291-316 (1992).
Relevant Web Sites: 
http://urap.gsfc.nasa.gov/www/home.html


Modification History
TBD




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UY_M0_RARA
Description
This data set contains 10 minute 
averages of the average 
electric field intensities from the 
Unified Radio and Plasma Wave 
Instrument Radio Astronomy Receiver.
Units are microVolt/Hz**0.5.
Data Set Contact: R Hess, 
NASA Goddard Spaceflight Center, 
Greenbelt, Maryland, USA.
Principal Investigator: R J Macdowall, 
NASA Goddard Spaceflight Center, 
Greenbelt, Maryland, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 291-316 (1992).
Relevant Web Sites: 
http://urap.gsfc.nasa.gov/www/home.html


Modification History
TBD




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UY_M0_RARP
Description
This data set contains 10 minute 
averages of the peak 
electric field intensities from the 
Unified Radio and Plasma Wave 
Instrument Radio Astronomy Receiver.
Units are microVolt/Hz**0.5.
Data Set Contact: R Hess, 
NASA Goddard Spaceflight Center, 
Greenbelt, Maryland, USA.
Principal Investigator: R J Macdowall, 
NASA Goddard Spaceflight Center, 
Greenbelt, Maryland, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 291-316 (1992).
Relevant Web Sites: 
http://urap.gsfc.nasa.gov/www/home.html


Modification History
TBD




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UY_M0_WFBA
Description
This data set contains 10 minute 
averages of the averaged magnetic field 
intensities from the Unified Radio and
Plasma Wave Instrument Waveform Analyzer
Units are 1.0e-15Tesla/Hz**0.5.
Data Set Contact: R Hess, 
NASA Goddard Spaceflight Center, 
Greenbelt, Maryland, USA.
Principal Investigator: R J Macdowall, 
NASA Goddard Spaceflight Center, 
Greenbelt, Maryland, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 291-316 (1992).
Relevant Web Sites: 
http://urap.gsfc.nasa.gov/www/home.html


Modification History
TBD




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UY_M0_WFBP
Description
This data set contains 10 minute 
averages of the peak magnetic field 
intensities from the Unified Radio and
Plasma Wave Instrument Waveform Analyzer
Units are 1.0e-15Tesla/Hz**0.5.
Data Set Contact: R Hess, 
NASA Goddard Spaceflight Center, 
Greenbelt, Maryland, USA.
Principal Investigator: R J Macdowall, 
NASA Goddard Spaceflight Center, 
Greenbelt, Maryland, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 291-316 (1992).
Relevant Web Sites: 
http://urap.gsfc.nasa.gov/www/home.html


Modification History
TBD




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UY_M0_WFEA
Description
This data set contains 10 minute 
averages of the averaged electric field 
intensities from the Unified Radio and
Plasma Wave Instrument Waveform Analyzer
Units are microVolt/Hz**0.5.
Data Set Contact: R Hess, 
NASA Goddard Spaceflight Center, 
Greenbelt, Maryland, USA.
Principal Investigator: R J Macdowall, 
NASA Goddard Spaceflight Center, 
Greenbelt, Maryland, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 291-316 (1992).
Relevant Web Sites: 
http://urap.gsfc.nasa.gov/www/home.html


Modification History
TBD




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UY_M0_WFEP
Description
This data set contains 10 minute 
averages of the peak electric field 
intensities from the Unified Radio and
Plasma Wave Instrument Waveform Analyzer
Units are microVolt/Hz**0.5.
Data Set Contact: R Hess, 
NASA Goddard Spaceflight Center, 
Greenbelt, Maryland, USA.
Principal Investigator: R J Macdowall, 
NASA Goddard Spaceflight Center, 
Greenbelt, Maryland, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 291-316 (1992).
Relevant Web Sites: 
http://urap.gsfc.nasa.gov/www/home.html


Modification History
TBD




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UY_M1_BAI
Description
This data set contains 1 hour 
averages of the ion density, 
temperature and velocity data from the 
Ulysses Solar Wind Observations Over 
the Poles of the Sun instrument. 
Density units are /cm3, temperature 
units are K, velocity units are km/s. 
Data Set Contact: B E Goldstein, 
NASA Ames Research Center, USA. 
Principal Investigator: D J McComas, 
Southwest Research Institute, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 237-265 (1992).
Relevant Web Sites: 
http://sst.lanl.gov/nis-projects/swoops/


Modification History
TBD




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UY_M1_EPA
Description
This data set contains 1 hour averages 
of the proton and electron 
flux data from the Ulysses 
Energetic Particle Composition
Experiment. 
Flux units are /cm2/s/sr. 
Data Set Contact: M Bruns, 
Max Planck Institut fur Aeronomie, 
Lindau, Germany.
Principal Investigator: E Keppler, 
Max Planck Institut fur Aeronomie, 
Lindau, Germany.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 317-331 (1992).
Relevant Web Sites: 
http://www.mpae.gwdg.de/mpae_projects/ULYSSES/EPAC.html


Modification History
Data version 1: Original ASCII source data.
Data version 2: Applies to 1996 CDFs onwards, 
which have been replaced with (or now use) 
ASCII source files generated with a program 
which does not remove low event rate data, 
as was the case for version 1 data. Pre-1996 
files are not reprocessed/replaced as version 2 
as no useful low event rate data exists pre-1996.
For further details contact M. Bruns, 
Max Planck Institut fur Aeronomie, 
Lindau, Germany




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UY_M1_LF15
Description
This data set contains 1 hour spin
averaged count rates of the electron and 
ion data from the Ulysses Heliosphere
Instrument for Spectra, Composition 
and Anisotropy at Low Energies 
(HI-SCALE) Low Energy Foil Spectrometer 
at 150 degrees to the spacecraft spin axis.
Count rate units are /s. 
Data Set Contact: T P Armstrong, 
Department of Physics & Astronomy, 
University of Kansas, USA.
Principal Investigator: L J Lanzerotti, 
Bell Laboratories, Lucent Technologies, 
Murray Hill, NJ, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 349-363 (1992).
Relevant Web Sites: 
http://sd-www.jhuapl.edu/Ulysses/
http://kuspa1.phsx.ukans.edu:8000/~ulysses/index.html


Modification History
TBD




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UY_M1_LF60
Description
This data set contains 1 hour spin
averaged count rates of the electron and 
ion data from the Ulysses Heliosphere
Instrument for Spectra, Composition 
and Anisotropy at Low Energies 
(HI-SCALE) Low Energy Foil Spectrometer 
at 60 degrees to the spacecraft spin axis.
Count rate units are /s. 
Data Set Contact: T P Armstrong, 
Department of Physics & Astronomy, 
University of Kansas, USA.
Principal Investigator: L J Lanzerotti, 
Bell Laboratories, Lucent Technologies, 
Murray Hill, NJ, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 349-363 (1992).
Relevant Web Sites: 
http://sd-www.jhuapl.edu/Ulysses/
http://kuspa1.phsx.ukans.edu:8000/~ulysses/index.html


Modification History
TBD




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UY_M1_LM12
Description
This data set contains 1 hour spin
averaged count rates of the ion data 
from the Ulysses Heliosphere Instrument 
for Spectra, Composition and Anisotropy 
at Low Energies (HI-SCALE) Low Energy 
Magnetic Spectrometer at 120 degrees to 
the spacecraft spin axis.
Count rate units are /s. 
Data Set Contact: T P Armstrong, 
Department of Physics & Astronomy, 
University of Kansas, USA.
Principal Investigator: L J Lanzerotti, 
Bell Laboratories, Lucent Technologies, 
Murray Hill, NJ, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 349-363 (1992).
Relevant Web Sites: 
http://sd-www.jhuapl.edu/Ulysses/
http://kuspa1.phsx.ukans.edu:8000/~ulysses/index.html


Modification History
TBD




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UY_M1_LM30
Description
This data set contains 1 hour spin
averaged count rates of the ion data 
from the Ulysses Heliosphere Instrument 
for Spectra, Composition and Anisotropy 
at Low Energies (HI-SCALE) Low Energy 
Magnetic Spectrometer at 30 degrees to 
the spacecraft spin axis.
Count rate units are /s. 
Data Set Contact: T P Armstrong, 
Department of Physics & Astronomy, 
University of Kansas, USA.
Principal Investigator: L J Lanzerotti, 
Bell Laboratories, Lucent Technologies, 
Murray Hill, NJ, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 349-363 (1992).
Relevant Web Sites: 
http://sd-www.jhuapl.edu/Ulysses/
http://kuspa1.phsx.ukans.edu:8000/~ulysses/index.html


Modification History
TBD




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UY_M1_LMDE
Description
This data set contains 1 hour spin
averaged count rates of the deflected 
electron data from the Ulysses Heliosphere 
Instrument for Spectra, Composition and 
Anisotropy at Low Energies (HI-SCALE) 
Low Energy Magnetic Spectrometer at 30 
degrees to the spacecraft spin axis.
Count rate units are /s. 
Data Set Contact: T P Armstrong, 
Department of Physics & Astronomy, 
University of Kansas, USA.
Principal Investigator: L J Lanzerotti, 
Bell Laboratories, Lucent Technologies, 
Murray Hill, NJ, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 349-363 (1992).
Relevant Web Sites: 
http://sd-www.jhuapl.edu/Ulysses/
http://kuspa1.phsx.ukans.edu:8000/~ulysses/index.html


Modification History
TBD




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UY_M1_SWI
Description
This data set contains 3.5 hour 
averages of the solar wind ion density 
ratio (to O6+), velocity and 
temperature from the Ulysses Solar Wind 
Ion Composition Spectrometer.
Velocity units are km/s. 
Temperature units are K. 
Data Set Contact: R von Steiger, 
International Space Science Institute, 
Bern, Switzerland.
Principal Investigators: J Geiss, 
International Space Science Institute,
Bern, Switzerland, and G Gloeckler, 
University of Maryland, College Park, 
Maryland, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 267-289 (1992).
Relevant Web Sites: 
http://space.umd.edu/UMD_sensors/uls_swics.html


Modification History
TBD




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UY_M1_VHM
Description
This data set contains 1 hour averages 
of the magnetic field components (RTN) 
and field magnitude from the Vector 
Helium Magnetometer.
Units are nT.
Data Set Contact: R J Forsyth,
The Blackett Laboratory, 
Imperial College, London, UK.
Principal Investigator: A Balogh, The 
Blackett Laboratory, Imperial College, 
London, UK.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 221-236 (1992).
Relevant Web Sites: 
http://www.sp.ph.ic.ac.uk/Ulysses/


Modification History
TBD




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UY_M1_WART
Description
This data set contains 1 hour spin
averaged count rates of the proton and 
ion data from the Ulysses Heliosphere
Instrument for Spectra, Composition 
and Anisotropy at Low Energies 
(HI-SCALE) Composition Aperture
Telescope at 60 degrees to the 
spacecraft spin axis.
Count rate units are /s. 
Data Set Contact: T P Armstrong, 
Department of Physics & Astronomy, 
University of Kansas, USA.
Principal Investigator: L J Lanzerotti, 
Bell Laboratories, Lucent Technologies, 
Murray Hill, NJ, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 349-363 (1992).
Relevant Web Sites: 
http://sd-www.jhuapl.edu/Ulysses/
http://kuspa1.phsx.ukans.edu:8000/~ulysses/index.html


Modification History
TBD




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UY_M1_WRTD
Description
This data set contains 1 hour spin
averaged count rates of the 
ion data from the Ulysses Heliosphere
Instrument for Spectra, Composition 
and Anisotropy at Low Energies 
(HI-SCALE) Composition Aperture
Telescope at 60 degrees to the 
spacecraft spin axis (WARTD).
Count rate units are /s. 
Data Set Contact: T P Armstrong, 
Department of Physics & Astronomy, 
University of Kansas, USA.
Principal Investigator: L J Lanzerotti, 
Bell Laboratories, Lucent Technologies, 
Murray Hill, NJ, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 349-363 (1992).
Relevant Web Sites: 
http://sd-www.jhuapl.edu/Ulysses/
http://kuspa1.phsx.ukans.edu:8000/~ulysses/index.html


Modification History
TBD




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UY_SP_LET
Description
This data set contains 10 minute 
averages of the ion and electron 
flux data from the Ulysses 
Cosmic Ray and Solar Particle 
Investigation Low Energy Telescope. 
Flux units are /cm2/s/sr/Mev. 
Data Set Contact: T R Sanderson, 
Solar System Division, ESA/ESTEC.
Principal Investigator: R B McKibben, 
Laboratory for Astrophysics and Space 
Research, Enrico Fermi Institute, 
University of Chicago, USA.
Reference: Astron. Astrophys. Suppl. 
Ser., 92(2), 365-399 (1992).
Relevant Web Sites: 
ftp://odysseus.uchicago.edu/WWW/Simpson/Ulysses.html
http://helio.estec.esa.nl/ssd/let.html


Modification History
TBD




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VI_C9_VI00
Description
Derived from VI00 in the CDAW9 database
Data for all CDAW9 events A-E.


Modification History
Converted to CDAWeb Feb 2000




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VI_C9_VI01
Description
Derived from VI01 in CDAW9 DB.
These North Pole UV auroral images (N2+ LBH bands and some O+ for Event C,  projected to 120 km
altitude, centered at 85 degrees mag.latitude) can be best seen from within the NACS software by
selecting the Mapped Image Plot option in Graphics. Recommended settings for the parameters in this
option are:  
1.  Choose MLAT,MLON,TCNT for X,Y,Z. 2.  Choose Nearest1 algorithm and 100 gridpoints. 3.  Choose
Orthographic projection, 90 for the pole, magnification of 3,       and set MAPDATA to 10 to turn
off continent outlines. 4.  You may change the plotted range of intensities from default values. 5. 
Select times that include the start time of the desired image. 6.  Fill in the plot Title,
save_filename, Username, etc., and SELERASE 'on'. 
The geomagnetic coordinates are eccentric dipole (IGRF 1985).  No dayglow corrections have been
applied.  The ungridded images are also available on the MAC, via NCSA Image.  A program is
available (9/91), to run on a Sun workstation, which displays the ungridded images, saves values of
selected points, and presents a mapped gridded image on request (geographic or geomagnetic).


Modification History
Converted to CDAWeb Feb 2000




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VI_C9_VI04
Description
Derived from VI04 in CDAW9 database.
Data for all CDAW9 eventst A-E


Modification History
Converted to CDAWeb Feb 2000




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VI_C9_VI05
Description
Derived from vi05 in CDAW9 DB.
Data for all CDAW9 events A-E
This CDF contains the data for every third energy value of this experiment. Energy steps
0,3,6,9,12,15,18,21,24,27,30, and 32 were included.  This CDF has a very fine time resolution of
0.15 seconds, and is therefore quite large.  It takes a large amount of time to plot more than about
an hour of data for any parameter.


Modification History
converted to CDAWeb Feb 2000




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VI_C9_VI06
Description
Derived from CC01 in CDAW9 DB.
Data for all CDAW9 events A-E
Geomagnetic field measurements with the IGRF80 field model subtracted


Modification History
Converted to CDAWeb Feb 2000




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VI_C9_VI2B
Description
Derived from VI2b in CDAW9 DB.
Data for all CDAW9 events A-E.
  .


Modification History
Converted to CDAWeb Feb 2000




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VI_C9_VI2D
Description
Derived from CC01 in CDAW9 DB.
Data for CDAW9 events A,C,E
Electron density obtained with relaxation sounder of HF instrument cluster    
Depending on the orbit, the time resolutio is 72 seconds or 2 minutes.For Event A, it is 2 minutes;
for Events C and E, it is 72 seconds.


Modification History
Converted to CDAWeb Feb 2000




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VI_C9_VI2F
Description
Data derived from VI2F in CDAW9 DB.
Data for CDAW9 events A,C,E
Data obtained by the Swept Frequency Analyzers of the HF instrument cluster


Modification History
Converted to CDAWeb Feb 2000




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VI_C9_VI2S
Description
Derived from vi2s in CDAW9 DB.
Data for all CDAW9 events A-E
  .


Modification History
Converted to CDAWeb Feb 2000




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VI_C9_VI3H
Description
Derived from VI3H in CDAW9 DB.
Data for CDWA9 events A & C.
Two antenna beams, 80 m tip-to-top 
Due to the very large data volume, for best response time when plotting power density vs time the
user should use filtering to select a single frequency index (which is constant), rather than the
frequency range (which is time-varying and requires much longer to search).  
Both VI3H and VI3L have identical parameters, basically the power spectral density as a function of
frequency.  The instrument has 3 operating modes, and switches from one to another at various times.
  
VI3H (Higher frequencies) contains Mode 1 and 2 data:      Mode 1:  from 10 to 214 Hz in 14 ranges  
    Mode 2:  from 10 to 428 Hz in 17 ranges. 
VI3L (Lower frequencies) contains Mode 3 data:      Mode 3:  from 0.4 to 10 Hz in 13 frequency
ranges. 
Because the instrument changes modes continuously, there is 2-second resolution in both VI3H and
VI3L, but never the same time for H and for L. 
For plotting a power density spectrum, the user should plot the power density, using filtering to
select the time interval.  Or, the Animation feature can be used, animating on, e.g., IMINUTE, which
would then produce a composite of all the spectra for each minute of time.  When using Animation for
this, one might want to set the controls to ORDER on either the vertical or the horizontal
parameter, or use SCATTER plot instead of VECTOR, to avoid drawing extraneous lines from the end of
one spectrum to the beginning of the next one.


Modification History
Converted to CDAWeb Feb 2000




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VI_C9_VI3L
Description
Derived from VI3L in CDAW9 DB.
Data for CDAW9 events A & C.
Two antenna beams, 80 m tip-to-top 
Due to the very large data volume, for best response time when plotting power density vs time the
user should use filtering to select a single frequency index (which is constant), rather than the
frequency range (which is time-varying and requires much longer to search).  
Both VI3H and VI3L have identical parameters, basically the power spectral density as a function of
frequency.  The instrument has 3 operating modes, and switches from one to another at various times.
  
VI3H (Higher frequencies) contains Mode 1 and 2 data:      Mode 1:  from 10 to 214 Hz in 14 ranges  
    Mode 2:  from 10 to 428 Hz in 17 ranges. 
VI3L (Lower frequencies) contains Mode 3 data:      Mode 3:  from 0.4 to 10 Hz in 13 frequency
ranges. 
Because the instrument changes modes continuously, there is 2-second resolution in both VI3H and
VI3L, but never the same time for H and for L. 
For plotting a power density spectrum, the user should plot the power density, using filtering to
select the time interval.  Or, the Animation feature can be used, animating on, e.g., IMINUTE, which
would then produce a composite of all the spectra for each minute of time.  When using Animation for
this, one might want to set the controls to ORDER on either the vertical or the horizontal
parameter, or use SCATTER plot instead of VECTOR, to avoid drawing extraneous lines from the end of
one spectrum to the beginning of the next one.


Modification History
Converted to CDAWeb Feb 2000




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VI_C9_VI5W
Description
Derived from CC01 in CDAW9 DB.
Data for all CDAW9 events A-E.
Energy channels are binned
For time history: plot a flux vs. time, filtering on VI5WELEN or VI5WINEN to select channel.  Energy
spectrum: make XY plot VI5WEFLX vs VI5WELEN (for electrons), with filter on desired time. Animate
for several spectra per interval.
These CDFs contain electron and ion (mostly proton) data from the Viking-3 hot plasma experiment. 
The full resolution dataset contains 36 electron energy channels and 32 ion energy channels.  The
energy of each channel depends on the detector mode; two electron modes (one of which had only 32
energy channels) and three ion modes occurred during the CDAW-9 events. Because of the large
quantity of data, 9 contiguous energy bins were defined for each detector; the energy at the
low-energy bin edge is given in the variables VI5WELEN for electrons and VI5WINEN for ions.  The
highest bin edge is 40 keV for both detectors.  The 9 fluxes in the arrays VI5WEFLX and VI5WIFLX are
the average of the fluxes in each bin.  Electron fluxes measured near 1 keV are subject to
interference, and have been omitted. 
To examine the time history of the data, plot one flux channel vs time, using a filter on VI5WELEN
or VI5WINEN to select the channel.  To see an energy spectrum, make an XY plot VI5WEFLX vs VI5WELEN
(for electrons), with a filter on the desired time.  For more than one spectrum in a time interval
(spectra are available every 1.2 s), use the Animation feature.


Modification History
Converted to CDAWeb Feb 2000




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VI_C9_VIMD
Description
Derived from VIMD in CDAW9 DB by S. Kayser
Data for all CDAW9 events A-E


Modification History
Converted to CDAWeb Feb 2000




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VI_ED_AI
No TEXT global attribute.


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WI_AT_DEF
Description
TBS


Modification History
6/13/91 - Original Implementation
9/18/91 - Modified for new attitude file format changes.  ICCR 881
2/11/92 - Used the variable name TIME and type CDF_INT4 and size 3 instead of 
EPOCH, CDF_EPOCH and 1 for the time tags.  CCR 490
6/1/92 - Added global attributes TITLE, PROJECT, DISCIPLINE, SOURCE_NAME, 
DATA_VERSION, and MODS; added variable attributes VALIDMIN, VALIDMAX, 
LABL_PTR_1, and MONOTON; added variables EPOCH and LABEL_TIME; 
changed variable name TIME to TIME_PB5.  CCR 1066
11/07/92 - use cdf variable Epoch and Time_PB5
6/8/93 - Added global attributes ADID_ref and Logical_file_id.  CCR 1092
7/5/94 - CCR ISTP 1852, updated CDHF skeleton to CDF standards - JT
9/20/94 - Added global attributes GCI_RA_ERR and GCI_DECL_ERR.  CCR 1932
11/7/94 - Merged CCR 1852 changes and corrected errors 
made in CCR 1852.  ICCR 1884
12/7/94 - Modified MODS and LABLAXIS to follow ISTP standards.  ICCR 1885




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WI_AT_PRE
Description
TBS


Modification History
6/13/91 - Original Implementation
9/18/91 - Modified for new attitude file format changes.  ICCR 881
2/11/92 - Used the variable name TIME and type CDF_INT4 and size 3 instead of 
EPOCH, CDF_EPOCH and 1 for the time tags.  CCR 490
6/1/92 - Added global attributes TITLE, PROJECT, DISCIPLINE, SOURCE_NAME, 
DATA_VERSION, and MODS; added variable attributes VALIDMIN, VALIDMAX, 
LABL_PTR_1, and MONOTON; added variables EPOCH and LABEL_TIME; 
changed variable name TIME to TIME_PB5.  CCR 1066
11/07/92 - use cdf variable Epoch and Time_PB5
6/8/93 - Added global attributes ADID_ref and Logical_file_id.  CCR 1092
7/5/94 - CCR ISTP 1852, updated CDHF skeleton to CDF standards - JT
9/20/94 - Added global attributes GCI_RA_ERR and GCI_DECL_ERR.  CCR 1932
11/7/94 - Merged CCR 1852 changes and corrected errors 
made in CCR 1852.  ICCR 1884
12/7/94 - Modified MODS and LABLAXIS to follow ISTP standards.  ICCR 1885




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WI_ED_MFI
Description
References:                                                                     
1. Panetta P. (GSFC), GGS WIND MFI Operator's Manual, September 15, 1992.   
2. Computer Sciences Corporation, Data Format Control Document (DFCD) Between   
The International Solar-Terrestrial Physics (ISTP) Program Information          
Processing Division Ground Data Processing System and The ISTP Mission          
Investigators, CSC/TR-91/6014, 560-1DFD/0190, July 1992.                        
3. Behannon, K. W., International Solar Terrestrial Physics (ISTP) Program      
Investigator Data Analysis Requirements For WIND and GEOTAIL Spacecraft         
Magnetometer Experiment, September 1987.


Modification History
Initial Release 7/12/93 
Created by M. Peredo 9/15/95 
for magnetopause skimming 
events study.


Variable Notes

Magnetic field magnitude
Average of the magnitudes


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WI_H0_3DP
Description
Wind 3dp




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WI_H0_MFI
Description
WIND MFI Composite data file.  This file contains multiple time resolution data.
1 Minute data averages                                                          
3 Second data averages                                                          
1 Hour   data averages                                                          
WIND MFI Instrument turn on 11/12/1994                                          
References:                                                                     
1. Lepping, R. P., et al., The WIND Magnetic Field Investigation, p. 207 in     
The Global Geospace Mission, ed. by C. T. Russell, Kluwer,1995                  
2. Panetta, P. (GSFC), GGS WIND MFI Operator's Manual, September 15, 1992.      
3. Computer Sciences Corporation, Data Format Control Document (DFCD) Between   
The International Solar-Terrestrial Physics (ISTP) Program Information          
Processing Division Ground Data Processing System and The ISTP Mission          
Investigators, CSC/TR-91/6014, 560-1DFD/0190, July 1992.                        
4. Behannon, K. W., International Solar Terrestrial Physics (ISTP) Program      
Investigator Data Analysis Requirements For WIND and GEOTAIL Spacecraft         
Magnetometer Experiment, September 1987.                                        
5. National Space Science Data Center, CDF User's Guide, Version 2.3.0,         
October 1, 1992.                                                                
6. Mish, W. H., International Solar-Terrestrial Physics (ISTP) Key Parameter    
Generation Software (KPGS) Standards & Conventions, September 1992.             
7. Mish, W. H., IMP F and G Phase I Magnetic Field Analysis, April 1972


Modification History
 10/28/94 Initial release                    
 01/28/97 Z-variable Release add Z correction
 02/20/97 Change file name from sp to h0


Variable Notes

Magnetic field magnitude (1 min)
Average of the magnitudes (F1)
RMS magnitude (1 min)
RMS of the magnitudes (F1 RMS)
Magnetic field magnitude (3 sec)
Average of the magnitudes (F1)
RMS magnitude (3 sec)
RMS of the magnitudes (F1 RMS)
Magnetic field magnitude (1 hour)
Average of the magnitudes (F1)
RMS magnitude (1 hour)
RMS of the magnitudes (F1 RMS)


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WI_H0_SWE
Description
Explanatory notes:
The electron moments included in this data set are derived from the velocity moments integration of
solar wind electron distributions measured by the WIND/SWE VEIS instrument (see Ogilvie et al.,
"SWE, a comprehensive plasma instrument for the WIND spacecraft", Space Sci. Rev., 71, 55, 1955).
Moments parameters are computed from 3s measurements which are spaced either 6s or 12s in time. 
Plots should therefore not exceed a time range of 2 or 3 hours in order to display the details of
this high resolution data.  The moments parameters which will be of value to most users of this data
set are the electron temperature, the electron temperature anisotropy, and the electron heat flux
vector. These quantities are reliable and citable with caution, meaning that the PI advises that the
user should discuss their interpretation with a member of the SWE science team before publishing. 
The following comments are intended to aid in the use and interpretation of the prime quantities of
this data set, the electron temperature, the electron temperature anisotropy, and the electron heat
flux. (All vector quantities are in GSE coordinates.) The temperature and temperature anisotropy are
normalized to the derived electron density and, therefore, are not sensitive to  the uncertainty in
the density determination as discussed below. The electron temperature is derived from the pressure
tensor divided by the electron density and the Boltzmann constant. The three eigenvalues of the
diagonalized temperature tensor are the temperature parallel to the tensor principal axis and the
two perpendicular components of the temperature. The temperature anisotropy is defined here as the
ratio of the parallel temperature to the average of the two perpendicular temperature components.
The electron temperature is one-third of the trace of the diagonalized temperature
tensor. Also included is the unit vector along the principal axis of the pressure tensor as well as
the cosine of the angle between the principal axis and the magnetic field vector. An indication that
the principal axis has been uniquely defined is that the temperature anisotropy is significantly
different from unity and that the principal axis and the magnetic field are nearly parallel or
anti-parallel.
The heat flux vector included here is significant only when the magnitude rises above the noise
level, i.e., above the level 0.002 to 0.005 ergs/cm/cm/s.  The heat flux may be low in magnitude
either due to a nearly isotropic distribution, due to electron counter-streaming, or due to a  low
counting rate of the instrument. An indicator of a significant net heat flux is that the heat flux
direction should track with the magnetic field direction. For this purpose, the cosine of the angle
between the heat flux vector and the magnetic field is included, and should be close to  -1 or  +1
in order for the heat flux to be significant. In some cases it will be necessary to use electron
pitch angle distributions (available on request from the SWE team) to decide whether low electron
flux or counterstreaming account for a low net heat flux. It is also strongly recommended that 3s
magnetic field data from the WIND/MFI experiment (not included in this data set) be used in
conjunction with the SWE electron heat flux data to ensure a correct interpretation of the heat
flux.
The electron density and electron bulk flow velocity are also included in this data set but no claim
is made for their accuracy. The electron flow velocity is usually within 10% to 20% of the solar
wind flow velocity derived from the SWE Faraday cup experiment and which are found in the SWE key
parameter data set. The electron density, however,  cannot be absolutely determined due to the
spacecraft potential and the fact that the electron instrument response has varied over time. The
electron density determination includes a first order attempt to determine the spacecraft potential
by imposing the charge neutrality condition on the derived electron density and Faraday cup ion
density. The electron density will be within a few percent of the solar wind density derived from
the Faraday cup early in the mission (1994-1997), while later in the mission (1998 and onward),
depending on the state of the instrument,  there will be times when the derived electron density
may be as much as a factor 2 too low. Although the electron density is not derived absolutely,
relative changes in electron density can usually be relied on. Both the electron density and
electron flow speed track with variations in the ion density and ion flow speed, respectively.
However, the user is strongly advised to use the SWE ion key parameters for the bulk plasma density
and flow speed.


Modification History
Skeleton created 1/19/2000
Started again 3/13/2001


Variable Notes

Electron Temperature, Te
Te = (trace of pressure tensor)/(electron density * Boltzman constant)/3 =
(2*Te_perp + Te_para)/3
Temperature anisotropy = Te_para / Te_perp
Te_perp = average of the perpendicular elements of the temperature tensor. 
Te_para = parallel component of the temperature tensor.
Electron average energy
Average energy = (3/2)Boltzmann constant * Te
Electron bulk velocity - magnitude 
See the global attribute TEXT.
Electron bulk velocity - elevation 
See the global attribute TEXT.
Electron bulk velocity - azimuth 
See the global attribute TEXT.
Electron density
See the global attribute TEXT.
Spacecraft Potential
Forst-order estimate only; se the global attribute TEXT.
Label for Time_PB5 (Jan 1 = Day 1)
Jan 1 = Day 1


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WI_H0_WAV
Description
SSR WAVES: The Radio and Plasma Wave Investigation on the WIND Spacecraft, Vol 71, pg 231-263,1995.



Secondary file - high resplasma density


Modification History
CODED JUNE 1996, C. MEETRE


Variable Notes

Electron density determined from insitu Fpe 'line'; position recognized by a neural network.
High resolution plasma densities:  actual resolution depends on instrument mode
and may vary.


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WI_H1_MFI
Description
WIND MFI 1 hour data averages
WIND MFI Instrument turn on 11/12/1994                                          
References:                                                                     
1. Lepping, R. P., et al., The WIND Magnetic Field Investigation, p. 207 in     
The Global Geospace Mission, ed. by C. T. Russell, Kluwer,1995                  
2. Panetta, P. (GSFC), GGS WIND MFI Operator's Manual, September 15, 1992.      
3. Computer Sciences Corporation, Data Format Control Document (DFCD) Between   
The International Solar-Terrestrial Physics (ISTP) Program Information          
Processing Division Ground Data Processing System and The ISTP Mission          
Investigators, CSC/TR-91/6014, 560-1DFD/0190, July 1992.                        
4. Behannon, K. W., International Solar Terrestrial Physics (ISTP) Program      
Investigator Data Analysis Requirements For WIND and GEOTAIL Spacecraft         
Magnetometer Experiment, September 1987.                                        
5. National Space Science Data Center, CDF User's Guide, Version 2.3.0,         
October 1, 1992.                                                                
6. Mish, W. H., International Solar-Terrestrial Physics (ISTP) Key Parameter    
Generation Software (KPGS) Standards & Conventions, September 1992.             
7. Mish, W. H., IMP F and G Phase I Magnetic Field Analysis, April 1972


Modification History
 10/28/94 Initial release                    
 01/28/97 Z-variable Release add Z correction
 02/20/97 Change file name from sp to h0


Variable Notes

Magnetic field magnitude (1 hour)
Average of the magnitudes (F1)
RMS magnitude (1 hour)
RMS of the magnitudes (F1 RMS)


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WI_H1_SWE
Description
SWE, a comprehensive plasma instrument for the WIND spacecraft, K.W.
Ogilvie, et al., Space Sci. Rev., 71, 55-77, 1995
Solar wind proton parameters, including anisotropic temperatures, derived by non-linear fitting of
the measurements and with moment techniques.
Data reported within this file do not exceed the limits of various parameters listed in the
following section.  There may be more valid data in the original dataset that requires additional
work to interpret but was discarded due to the limits.  In particular we have tried to exclude
non-solar wind data from these files. 
We provide the one sigma uncertainty for each parameter produced by the non-linear curve fitting
analysis either directly from the fitting or by propagating uncertainties for bulk speeds, flow
angles or any other derived parameter.
For the non-linear anisotropic proton analysis, a scalar thermal speed is produced by determining
parallel and perpendicular tmperatures, taking the trace, Tscalar = (2Tperp + Tpara)/3 and
converting the result back to athermal speed.  The uncertainties are also propagated through


Modification History
12/28/94, 3/4/96, by Alan J. Lazarus John T. Steinberg Daniel B. Berdichevsky.




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WI_H1_WAV
Description
 The Radio and Plasma Wave Investigation on the WIND Spacecraft, Sp.Sci.Rev.,Vol 71, pg, 
231-263,1995.


Modification History
CODED JAN,1999, SARDI


Variable Notes

Normalized receiver average voltage (RAD2, 1075-13825 kHz)
Working channels are about 20 of total 256 frequency channels.  Values for other
channels are interpolations
[LIST ONLY] Daily receiver minimum voltage (RAD2, 1075-13825 kHz, non-zero values show active freqs)
Zero value denotes channel average values are interpolated, not directly
measured


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WI_H9_MFI
Description


Modification History
Created by R.L. Kessel on 1/17/2001 - similar to k1 product  but this one is based on WI_H0_MFI data
Modified by RL Kessel on 7/16/2002 to mirror the Geotail ULF parameters




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WI_K0_3DP
Description
Electron flux energy levels: 
channel 1: 0.1-.4   keV      
channel 2: 0.4-1.8  keV      
channel 3: 1.9-8.0  keV      
channel 4: 9.0-30   keV      
channel 5: 20-48    keV      
channel 6: 43-138   keV      
channel 7: 127-225  keV      
Ion flux energy levels:      
channel 1: 0.07-.21 keV      
channel 2: 0.25-1.1 keV      
channel 3: 1.3-7    keV      
channel 4: 8-30     keV      
channel 5: 20-58    keV      
channel 6: 58-126   keV      
channel 7: 115-400  keV      
pfu == 1/(cm^2-s-sr-keV)     



Created : Nov, 1991, for 3dpa kpgs testing
Modified: May, 1992, to accomodate Standards and Conventions
Modified: Jan, 1993, as suggested by Kessel
Modified: Mar, 1993, as suggested by Kessel
Modified: Jun 7, 1994, for updated 3dpa telemetry specifications
Modified: Jun 9, 1994, as suggested by KITT
Modified: Jul 10, 1994
Modified: Apr  3, 1995, particle temperatures from K to eV
Modified: jun 12, 1995, particle flux scaling adjustments


Modification History
version 1.0, october 91   
version 1.0.1, summer 92  
version 1.0.2, january 93 
version 1.1,   june 94 
version 1.1.1, june 94 
version 1.1.2, june 94 
version 1.1.3, july 94 
version 1.2, april 95 
version 05, june 95


Variable Notes

Electron Flux at 7 energies (0.1-225 keV)
pfu=particle flux unit=1/(cm^2-s-sr-keV)
Ion flux at 7 energies (.07-400 keV)
pfu=particle flux unit=1/(cm^2-s-sr-keV)


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WI_K0_EPA
Description
Wind/EPACT Key Parameters
LEMT - Low Energy Matrix       Telescope        
APE - Alpha Proton            Electron          
This is a character attribute to hold some meta-data........


Modification History
Created May 10, 1995
Created May 18, 1995




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WI_K0_MFI
Description
References:                                                                     
1. Panetta P. (GSFC), GGS WIND MFI Operator's Manual, September 15, 1992.   
2. Computer Sciences Corporation, Data Format Control Document (DFCD) Between   
The International Solar-Terrestrial Physics (ISTP) Program Information          
Processing Division Ground Data Processing System and The ISTP Mission          
Investigators, CSC/TR-91/6014, 560-1DFD/0190, July 1992.                        
3. Behannon, K. W., International Solar Terrestrial Physics (ISTP) Program      
Investigator Data Analysis Requirements For WIND and GEOTAIL Spacecraft         
Magnetometer Experiment, September 1987.


Modification History
Initial Release 7/12/93 
Zvar Release 10/24/96 
Zvar Update  11/12/96




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WI_K0_SMS
Description
Time is for the start of the averaging interval. Computed are
 the avg alpha vel; avg C/O abundance ratio; avg carbon
 ionization temp in million degs K from C+6 & C+5 
(using the tbls of Arnaud & Rothenflug, 1985); 
the avg oxygen ionization temp from O+7 & O+6 in
million degs K (using tbls of Arnaud & Rothenflug, 1985)
Above avgs are made over 4 hrs.
He vel and He kinetic temp are computed every 3 min & are contained in the K1 CDF
References:                   Space Science Reviews 71:79-124, 1995,
 Kluwer Academic Publishers, Belgium  
Instrument consist of: Solar Wind Ion Composition 
Spectrometer (SWICS); high resolution mass  spectrometer (MASS); 
Supra-Thermal Ion Composition Spectrometer 
(STICS) & common DPU


Modification History
Version 01 Feb. 1996 - whm




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WI_K0_SPHA
Description
To be supplied


Modification History
12/17/92 - Original Implementation, CCR 87
6/14/94 - CCR ISTP 1852, updated CDHF skeleton to CDF standards - JT
11/9/94 - Correct errors made in ccr 1852.  CCR 1884




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WI_K0_SWE
Description
SWE, a comprehensive plasma instrument for the WIND spacecraft, K.W.
Ogilvie, et al., Space Sci. Rev., 71, 55-77, 1995


Modification History
12/28/94, 3/4/96, by Alan J. Lazarus John T. Steinberg Daniel B. Berdichevsky. 
Skeleton TABLE for plasma CDF SWE keyparameters, dbb, Jan., 1994.
Instr. qual. flags validmax setequal to +2147483647, 12/94. Qual. flags format changed to compatible
values with new validmax, jts and ajl, 12/94. 
Processing with instrument science modes 2 and 11 added, jts and dbb, 10/27/95. DICT_KEYs added ajl,
3/4/96.


Variable Notes

Velocity Quality Flag: 0=OK; 2 or 130 = caution; Other values NOT VALID
Velocity Quality Flag: 0=OK; 2=parabolic 3-point fit only; 130=parabolic 3-point
fit only, sensor 1 only, N/S angle zero degrees assumed; Other values NOT VALID
Proton thermal speed Quality Flag: 0=OK; 2 or 130 = caution; Other values NOT VALID
Proton thermal speed Quality Flag: 0=OK; 2=parabolic 3-point fit only;
130=parabolic 3-point fit only, sensor 1 only, N/S angle zero degrees assumed;
Other values NOT VALID
Proton Density Quality Flag: 0=OK; 2 or 130 = caution; Other values NOT VALID
Proton Density Quality Flag: 0=OK; 2=parabolic 3-point fit only; 130=parabolic
3-point fit only, sensor 1 only, N/S angle zero degrees assumed; Other values
NOT VALID


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WI_K0_WAV
Description
SSR WAVES: The Radio and Plasma Wave Investigation on the WIND Spacecraft, Vol 71, pg 231-263,1995.


Modification History
CODED MAY 1996, C. MEETRE


Variable Notes

Electric field average intensity in dB above background at 76 log-spaced frequencies (250-9.4e6 Hz).
background subtracted using 3% lower bound across each frequency band for entire
day - backgrounds given in variable E_Background. Data taken in spin plane only
Solar array current minimum for s/c
Solar array current from s/c HK correlates with photoelectric effect on antennas
Solar array current maximum for s/c
Solar array current from s/c HK correlates with photoelectric effect on antennas


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WI_OR_DEF
Description
TBS


Modification History
Originated Monday, May 13, 1991
Modified June 13, 1991 for version 2.1
Modified October 2,1991 for new global attributes, incr sizes
Modified 11/11/91 Add sun vector, replace space id with support id
Modified 1992 Feb 11 to use the variable name TIME and type CDF_INT4 instead of 
EPOCH and CDF_EPOCH for the time tags CCR 490
Modified 6/2/92 add project, discipline, source_name, data_version, title, and 
mods to global section; add validmin, validmax, labl_ptr_1 and monoton 
attributes to some variables; put epoch time back in, rename time to 
time_pb5; add label_time to variables
Modified 11/07/92 to use Epoch and Time_PB5 variable name
Modified 6/2/93 add ADID_ref and Logical_file_id
7/5/94 - CCR ISTP 1852 updated CDHF skeleton to CDF standards - JT
9/21/94 - Added 24 new global attributes to log the ephemeris 
comparison summary report from the definitive FDF orbit file.  CCR 1932
11/7/94 - Merged CCR 1852 changes and corrected errors 
made in CCR 1852.  ICCR 1884
12/7/94 - Modified MODS to follow ISTP standards.  ICCR 1885
01/05/95 - add heliocentric coordinate system.  CCR 1889
2/28/95 - added COMMENT1 and COMMENT2 for CCR




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WI_OR_PRE
Description
TBS


Modification History
Originated Monday, May 13, 1991
Modified June 13, 1991 for version 2.1
Modified October 2,1991 for new global attributes, incr sizes
Modified 11/11/91 Add sun vector, replace space id with support id
Modified 1992 Feb 11 to use the variable name TIME and type CDF_INT4 instead of 
EPOCH and CDF_EPOCH for the time tags CCR 490
Modified 6/2/92 add project, discipline, source_name, data_version, title, and 
mods to global section; add validmin, validmax, labl_ptr_1 and monoton 
attributes to some variables; put epoch time back in, rename time to 
time_pb5; add label_time to variables
Modified 11/07/92 to use Epoch and Time_PB5 variable name
Modified 6/2/93 add ADID_ref and Logical_file_id
7/5/94 - CCR ISTP 1852 updated CDHF skeleton to CDF standards - JT
9/21/94 - Added 24 new global attributes to log the ephemeris 
comparison summary report from the definitive FDF orbit file.  CCR 1932
11/7/94 - Merged CCR 1852 changes and corrected errors 
made in CCR 1852.  ICCR 1884
12/7/94 - Modified MODS to follow ISTP standards.  ICCR 1885
01/05/95 - add heliocentric coordinate system.  CCR 1889
2/28/95 - added COMMENT1 and COMMENT2 for CCR




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WI_OR_PRE
Description
TBS


Modification History
Originated Monday, May 13, 1991
Modified June 13, 1991 for version 2.1
Modified October 2,1991 for new global attributes, incr sizes
Modified 11/11/91 Add sun vector, replace space id with support id
Modified 1992 Feb 11 to use the variable name TIME and type CDF_INT4 instead of 
EPOCH and CDF_EPOCH for the time tags CCR 490
Modified 6/2/92 add project, discipline, source_name, data_version, title, and 
mods to global section; add validmin, validmax, labl_ptr_1 and monoton 
attributes to some variables; put epoch time back in, rename time to 
time_pb5; add label_time to variables
Modified 11/07/92 to use Epoch and Time_PB5 variable name
Modified 6/2/93 add ADID_ref and Logical_file_id
7/5/94 - CCR ISTP 1852 updated CDHF skeleton to CDF standards - JT
9/21/94 - Added 24 new global attributes to log the ephemeris 
comparison summary report from the definitive FDF orbit file.  CCR 1932
11/7/94 - Merged CCR 1852 changes and corrected errors 
made in CCR 1852.  ICCR 1884
12/7/94 - Modified MODS to follow ISTP standards.  ICCR 1885
01/05/95 - add heliocentric coordinate system.  CCR 1889
2/28/95 - added COMMENT1 and COMMENT2 for CCR




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XF_C9_XFI
Description
Derived from xfi in CDAW9 DB.
Data for CDAW9 events A-D.
added numerical station indices 1-8 in CDAWeb conversion  .


Modification History
Converted to CDAWeb Feb 2000




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XI_C9_XISY
Description
Derived from XISY in CDAW9 DB.
Data for all CDAW9 events A-E
Syowa and 3 conjugate Iceland stations; magnetometer, riometer, VLF


Modification History
converted to CDAWeb Feb 2000




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XK_C9_XKIR
Description
Derived from xkir in CDAW9 DB.
Data for CDAW9 events A & B only.
UHF Rcvr; 17 antenna positions (latitude scan) at 275 Km altitude. Per 30
EISCAT Radar Data is available from three stations. 
CDF mnemonic:
             XTMS             XKIR         XSOD                 
           Tromso           Kiruna      Sodankylae
               Norway           Sweden        Finland
----------------------------------------------------------------- 
Geographic Latitude/deg             69.58N           67.86N        67.37N 
Longitude/deg            19.21E           20.44E        26.65E   Corrected geomagnetic Latitude/deg 
           66.6N            64.9N         63.9N 
Longitude/deg           104.9E           104.2E        108.5E   Invariant Latitude/deg - 300km    
66.8N            65.1N         64.1N 
L-value - 300km           6.46             5.63          5.25 
Dip/deg - 300km          77.58            76.72         76.61      Altitude range/km       138 - 965
         275           275 
Geog. Lat. range/deg   60.1 - 79.2N    63.9 - 75.3N   63.9 - 75.3N 
Geog. Lon. range/deg    6.3 - 24.3E    13.5 - 22.7E   13.5 - 22.7E


Modification History
Added numerical index values to XKIR_IND/PO for initial   CDAWeb conversion Feb 2000.




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XS_C9_XSBR
Description
Derived from XSRA in CDAW9 DB.
Data for CDAW9 events A, B and C only.
SABRE = Sweden And Britain Radar Experiment Event A: Data only from 1900 to 2100 Event B: Data only
from 0100 to 0400 on 03-April-1986  Event C: Data only from 0000 to 0600


Modification History
Converted to CDAWeb Feb 2000




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XS_C9_XSOD
Description
Derived from XSOD in CDAW9 DB.
UHF Rcvr; 17 antenna positions (latitude scan) at 275 Km altitude. Per 30min.   
CDF mnemonic:             XTMS             XKIR         XSOD                           Tromso       
   Kiruna      Sodankylae                          Norway           Sweden        Finland
----------------------------------------------------------------- Geographic Latitude/deg           
 69.58N           67.86N        67.37N Longitude/deg            19.21E           20.44E       
26.65E  Corrected geomagnetic Latitude/deg             66.6N            64.9N         63.9N
Longitude/deg           104.9E           104.2E        108.5E  Invariant  Latitude/deg - 300km    
66.8N            65.1N         64.1N L-value - 300km           6.46             5.63          5.25
Dip/deg - 300km          77.58            76.72         76.61     Altitude range/km       138 - 965 
        275           275 Geog. Lat. range/deg   60.1 - 79.2N    63.9 - 75.3N   63.9 - 75.3N Geog.
Lon. range/deg    6.3 - 24.3E    13.5 - 22.7E   13.5 - 22.7E


Modification History
Added numerical indices to XSOD IND/PO in converting to CDAWeb Feb 2000.




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XS_C9_XSSH
Description
Derived from XSSH in CDAW9 DB.
Data for CDAW9 events A,B and E.
Ion Fractions Excluded from CDF. 
Variables that showed pervasively spurious values were not included in the CDF.


Modification History
Converted to CDAWeb Feb 2000




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XS_C9_XSSL
Description
Derived from XSSL in CDAW9 DB.
Data for CDAW9 events A, B and E only.
Direction # 4,5,6 unspecified  Electron Temperature Excluded.


Modification History
Converted to CDAWeb Feb 2000




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XS_C9_XSY1
Description
Derived from CC01 in CDAW9 DB.
Data for all CDAW9 events A-E.
Narrow beam steps through 11 points in N-S plane and 11 points in E-W plane.


Modification History
Converted to CDAWeb Feb 2000




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XT_C9_XTMS
Description
Derived from XTMS in CDAW9 DB.
Data for CDAW9 events A and B only.
UHF Trsm.& Recv.; Alt. scans (25) at each ant. pos. (17). Per 30 min. 
EISCAT Radar Data is available from three stations. 
 CDF mnemonic:             XTMS             XKIR         XSOD                           Tromso      
    Kiruna      Sodankylae                          Norway           Sweden        Finland
----------------------------------------------------------------- Geographic Latitude/deg           
 69.58N           67.86N        67.37N Longitude/deg            19.21E           20.44E       
26.65E  Corrected geomagnetic Latitude/deg             66.6N            64.9N         63.9N
Longitude/deg           104.9E           104.2E        108.5E  Invariant  Latitude/deg - 300km    
66.8N            65.1N         64.1N L-value - 300km           6.46             5.63          5.25
Dip/deg - 300km          77.58            76.72         76.61     Altitude range/km       138 - 965 
        275           275 Geog. Lat. range/deg   60.1 - 79.2N    63.9 - 75.3N   63.9 - 75.3N Geog.
Lon. range/deg    6.3 - 24.3E    13.5 - 22.7E   13.5 - 22.7E


Modification History
Converted to CDAWeb Feb 2000  
Added numerical indices to XTMS_IND/PO in conversion.




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XV_C9_XVIS
Description
Derived from XVIS in CDAW9 DB.


Modification History
Converted to CDAWeb Feb 2000.




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ZA_C9_ZAE
Description
Derived from ZAE in CDAW9 DB.
Data for all CDAW9 events A-E.


Modification History
Converted to CDAWeb Feb 2000




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ZC_C9_ZCF
Description
Derived from ZCF in CDAW9 DB.
  .


Modification History
Converted to CDAWeb Feb 2000




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ZE_C9_ZEI
Description
Derived from ZEI in CDAW9 DB.
Data for all CDAW9 events A-E . 
                         Corrected Geomagnetic      Geographic 
Station No.   Station     Latitude  Longitude     Latitude  Longitude 
    1          Soroya      67.3      107.9         70.5     22.22 
    2          Alta        66.6      107.8         69.9     22.96 
    3          Kautokeino  65.8      107.2         69.0     23.05 
    4          Muonio      64.7      106.7         68.0     23.53 
    5          Pello       63.6      106.0         66.9     24.08 
    6          Kilpisjarvi 66.0      105.4         69.1     20.70 
    7          Kevo        66.2      110.6         69.8     27.01


Modification History
Converted to CDAWeb Feb 2000




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ZF_C9_ZFI
Description
Derived from ZFI in CDAW9 DB.
                                          Geographic 
No. Code  Station Name      Components  Latitude  Longitude 
 1  AMD   Amderma              X,Y,Z     69.46     60.77  
 2  BLC   Baker Lake           X,Y,Z     64.33    -96.03   
 3  BRW   Barrow               X,Y,Z     71.30   -156.75     
 4  CBB   Cambridge Bay        X,Y,Z     69.10   -105.00     
 5  COL   College              X,Y,Z     64.87   -147.83     
 6  CPS   Cape Schmidt         X,Y,Z     68.92   -179.48     
 7  DIK   Dixon                X,Y,Z     73.55     80.57     
 8  ESK   Eskdalemuir          X,Y,Z     55.32     -3.20     
 9  FCC   Fort Churchill       X,Y,Z     58.80    -94.10     
11  GLL   Glenlea              X,Y,Z     49.63    262.87     
12  MBC   Mould Bay            X,Y,Z     76.30   -119.40     
13  MMK   Murmansk             X,Y,Z     68.25     33.08     
14  NAQ   Narssarssuaq         H,E,Z     61.20    -45.40     
15  OTT   Ottawa               X,Y,Z     45.40    -75.55     
16  PDB   Poste-de-la-Baleine  X,Y,Z     55.20    -77.70     
17  RES   Resolute Bay         X,Y,Z     64.70    -94.90     
18  SIT   Sitka                X,Y,Z     57.10   -135.30     
19  SOD   Sodankyla            X,Y,Z     67.37     26.63     
20  STJ   St. Johns            X,Y,Z     47.60    -52.60     
21  THL   Thule/Qanaq          H,E,Z     77.48    -69.17     
22  TIK   Tixie Bay            X,Y,Z     71.58    129.00     
23  VIC   Victoria             X,Y,Z     48.50   -123.40     
24  YEK   Yellowknife          X,Y,Z     62.43   -114.40


Modification History
Converted to CDAWeb Feb 2000




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ZH_C9_ZHA
Description
Derived from ZHA in CDAW9 DB.
Data for all CDAW9 events A-E.
Baseline: Z: 40000 nT, H: 19900 nT,  D: 1.5 deg W
These CDFs contain 15 sec averages of the H, D, and Z components measured by the Halley Station
magnetometer of the British Antarctic Survey.  One sec  resolution data is also available, but not
in CDF form.  The components are measured with respect to the following baseline: 
     Z: 40000 nT	H: 19900 nT	D: 1.5 deg W 
Halley Station is located at (75.5 S, 27 W), at L = 4.2.


Modification History
Converted to CDAWeb Feb 2000




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ZH_C9_ZHU
Description
Derived from ZHU in CDAW9 DB.
Data for all CDAW9 events A-E
This CDF was revised on August 2, 1990, to correct the sensitivity calibration.  The earlier version
assumed 1 nT per data count instead of the actual 0.006 nT per data count that is included in this 
revision.  All three components were corrected by the same factor.


Modification History
Corrected 8/2/90.
Converted to CDAWeb Feb 2000




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ZI_C9_ZIQ
Description
Derived from ZIQ in CDAW9 DB.
Data for all CDAW9 events A-E


Modification History
Converted to CDAWeb Feb 2000




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ZI_C9_ZIVA
Description
Derived from ZIVA in CDAW9 DB.
Data for CDAW9 event E only.
These magnetic H, D, and Z components are from the induction coil pulsation magnetometer at Ivalo
Station, Finland (IVA), at geographic coordinates  68.55 deg N, 27.27 deg E.  The 0.1s resolution
data have been corrected for frequency and phase response, and averaged over 1.0s.  An automatic
calibration signal starts every day at 1400 UT.


Modification History
Converted to CDAWeb Feb 2000




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ZK_C9_ZKIL
Description
Derived from ZKIL in CDAW9 DB.
Data for all CDAW9 events A-E
These magnetic H and D components are from the induction coil pulsation magnetometer at Kilpisjarvi
Station, Finland (KIL), at geographic coordinates 69d01m15s N, 20d52m21s E, L = 6.0.  The 0.1s
resolution data have been correc- ted for frequency and phase response, and averaged over 1.0s.  An
automatic calibration signal starts every day at 1400 UT.


Modification History
Converted to CDAWeb Feb 2000




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ZM_C9_ZMC
Description
Derived from ZMC in CDAW9 DB.
Data for all CDAW9 events A-E


Modification History
Converted to CDAWeb Feb 2000




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ZN_C9_ZNG
Description
Derived from ZNG in CDAW9 DB.
Data for all CDAW9 events A-E
Ground magnetometer data from 25 stations were supplied by the National  Geophysical Data Center
(NGDC).  Either HDZ or XYZ components are presented  from each station.  99999 is the flag for fill
values. There are no data for Event D from Fredericksburg or from Sitka.


Modification History
converted to CDAWeb Feb 2000




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ZO_C9_ZONA
Description
Derived from ZONA in CDAW9 DB.
Data for CDAW9 events C,D & E only.
Need Fourier analysis to calibrate


Modification History
Converted to CDAWeb Feb 2000




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ZR_C9_ZRG
Description
Derived from ZRG in CDAW9 DB.
Data for all CDAW9 events A-E


Modification History
Converted to CDAWeb Feb 2000




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ZR_C9_ZROV
Description
Derived from ZROV in CDAW9 DB.
Data for CDAW9 event E only.
These magnetic H, D, and Z components are from the induction coil pulsation magnetometer at
Rovaniemi Station, Finland (ROV), at geographic coordinates 66.77 deg N, 25.94 deg E.  The 0.1s
resolution data have been corrected for frequency and phase response, and averaged over 1.0s.  An
automatic calibration signal starts every day at 1400 UT.


Modification History
converted to CDAWeb Feb 2000




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ZS_C9_ZSA
Description
Derived from ZSA in CDAW9 DB.
120 sec. intervals; values=avgs. of 5 longitudes (18.0+18.5+19.0+19.5+20.0)


Modification History
Converted to CDAWeb Feb 2000




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ZS_C9_ZSI
Description
Derived from ZSI in CDAW9 DB.
Data for all CDAW9 events A-E


Modification History
converted to CDAWeb Feb 2000




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ZS_C9_ZSP
Description
Derived from ZSP in CDAW9 DB.
Data for all CDAW9 events A-E.


Modification History
converted to CDAWeb Feb 2000




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ZS_C9_ZSSR
Description
Derived from ZSSR in CDAW9 DB.
                            Geomagnetic dipole 
Station             Code      Coordinates            Institute 
                             PHI   LAMBDA   PSI 
Vize                VIZ   69.08   164.1   -17.16   AANII, O. A. Troshichev 
Uedinenie           UDN   66.9    165.3   -13.3    AANII, O. A. Troshichev 
Izvestia            IZV   65.4    164.9   -12.2    AANII, O. A. Troshichev 
Kotelny             KOT   64.9    194.8   -12.5    IFKIA, G. F. Krymsky 
Sopochanaya Karga   SKG   62.05   162.1   -11.57   AANII, O. A. Troshichev 
Norilsk             NOR   58.6    165.7    -7.88   SibIZMIR, G. A. Zherebtsov 
Uses coordinate system of the central magnetic dipole:        X = H cos(D-PSI)        Y = H
sin(D-PSI)        H = Ho + dH        D = Do + dD        PSI = The angle between the geographic and
geomagnetic meridians at the point of measurement.


Modification History
Converted to CDAWeb Feb 2000




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ZS_C9_ZSYM
Description
Derived from ZSYM in CDAW9 DB.
Data for all CDAW9 events A-E
5 mid-latitude stations.  Provisional values.


Modification History
converted to CDAWeb Feb 2000




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ZW_C9_ZWE
Description
Derived from ZWE in CDAW9 DB.
Data for CDAWeb events D & E only.
Time might be fast by as much as 30 s due to clock drift.


Modification History
converted to CDAWeb Feb 2000




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