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CDAWeb Served Heliophysics Datasets Beginning with 'F'

FAST_HR_DCB: High-resolution Fluxgate Magnetometer data for the FAST Mission - Robert Strangeway (UCLA)
FA_ESA_L2_EEB: FAST Electron Burst Distributions - J. P. McFadden (U.C. Berkeley Space Sciences Laboratory)
FA_ESA_L2_EEB_20090430074129: FAST Ion and Electron Particle Distributions - J. P. McFadden (U.C. Berkeley Space Sciences Laboratory)
FA_ESA_L2_EES: FAST Electron Survey Distributions - J. P. McFadden (U.C. Berkeley Space Sciences Laboratory)
FA_ESA_L2_EES_20090430074130: FAST Ion and Electron Particle Distributions - J. P. McFadden (U.C. Berkeley Space Sciences Laboratory)
FA_ESA_L2_IEB: FAST Ion Burst Distributions - J. P. McFadden (U.C. Berkeley Space Sciences Laboratory)
FA_ESA_L2_IEB_20090430074129: FAST Ion and Electron Particle Distributions - J. P. McFadden (U.C. Berkeley Space Sciences Laboratory)
FA_ESA_L2_IES: FAST Ion Survey Distributions - J. P. McFadden (U.C. Berkeley Space Sciences Laboratory)
FA_ESA_L2_IES_20090430074130: FAST Ion and Electron Particle Distributions - J. P. McFadden (U.C. Berkeley Space Sciences Laboratory)
FA_K0_ACF: FAST AC Fields - Key Parameters - C. Carlson (U.C. Berkeley)
FA_K0_TMS: FAST Energy Angle Mass Spectrograph - 5-s Survey/Key Parameters - E. Lund (UNH)
FM_K0_KILP: FMI Kilpisjarvi: All-Sky Camera Key Parameters - K. Kauristie (Finnish Meteorological Institute)

FAST_HR_DCB
Description
Calibrated fluxgate magnetometer data acquired by the Fast Auroral SnapshoT
Small Explorer (FAST). Data have been calibrated, despun, and detrended against
the International Geomagnetic Reference Field (IGRF), using IGRF coefficients
for the date of acquisition. Data are provided in several coordinate systems.
Non detrended data in spacecraft and Geocentric Equatorial Inertial coordinates
are also provided. Ephemeris data are provided.
Modification History
Initial CDF development 8/14/12
Version 1 release 03/07/13
Updated to CDF
version 3.5.0 12/26/13
 
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FA_ESA_L2_EEB
Description
ESA>Electrostatic Analyzer
 
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FA_ESA_L2_EEB_20090430074129
Description
ESA>Electrostatic Analyzer
Modification History
Rev-1 2015-07-28
 
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FA_ESA_L2_EES
Description
ESA>Electrostatic Analyzer
 
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FA_ESA_L2_EES_20090430074130
Description
ESA>Electrostatic Analyzer
Modification History
Rev-1 2015-07-28
 
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FA_ESA_L2_IEB
Description
ESA>Electrostatic Analyzer
 
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FA_ESA_L2_IEB_20090430074129
Description
ESA>Electrostatic Analyzer
Modification History
Rev-1 2015-07-28
 
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FA_ESA_L2_IES
Description
ESA>Electrostatic Analyzer
 
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FA_ESA_L2_IES_20090430074130
Description
ESA>Electrostatic Analyzer
Modification History
Rev-1 2015-07-28
 
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FA_K0_ACF
Description
none yet
Modification History
none yet
 
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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, 
published, Space Science Reviews, 
2001, volume 98, pages 197-291,  doi:10.1023/A:1013127607414. 
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: Particles, 1998, Geophysical Monograph Series, 
volume 102, pages 243-248.
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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