NASA Logo, National Aeronautics and Space Administration
CDAWeb
+ FEEDBACK
CDAWeb banner

CDAWeb Served Heliophysics Datasets Beginning with 'I'

I1_AV2_OTT: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I1_AV2_QUI: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I1_AV2_ULA: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I1_AV_ALL: ISIS-1 Topside sounder ionograms, all stations merged into a single dataset - R.F. Benson (NASA GSFC)
I1_AV_KER: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I1_AV_KSH: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I1_AV_KWA: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I1_AV_ODG: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I1_AV_ORR: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I1_AV_OTT: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I1_AV_QUI: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I1_AV_RES: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I1_AV_SNT: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I1_AV_SOD: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I1_AV_TRO: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I1_AV_ULA: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I1_AV_WNK: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I1_NEPROF_TOPS: ISIS-1 CRC Electron Density Profiles - J. E. Jackson (Communication Research Centre (CRC), Ottawa)
I2_AV_ACN: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_ADL: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_AME: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_BRZ: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_BUR: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_CNA: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_KER: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_KRU: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_KSH: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_KWA: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_LAU: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_ODG: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_ORR: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_OTT: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_QUI: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_RES: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_SNT: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_SOD: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_SOL: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_SYO: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_TRO: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_ULA: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_AV_WNK: ISIS Topside Sounder Ionogram - R.F. Benson (NASA GSFC)
I2_NEPROF_TOPIST: ISIS-2 TOPIST produced electron density profiles, of highest quality (quality flag = 2 and 3 - X. Huang and B. Reinisch (University of MassachusettsLowell)
I2_NEPROF_TOPS: ISIS-2 CRC Electron Density Profiles - J. E. Jackson (Communication Research Centre (CRC), Ottawa)
I7_R0_LEPEDEA: Link to IMP7 LEPEDEA Energy-Time Spectrograms in GIF format at the University of Iowa. - L. A. Frank (University of Iowa)
I8_15SEC_MAG: IMP-8 Fluxgate Magnetometer, 15.36-Second Resolution Data - A. Szabo / R.P. Lepping (NASA GSFC)
I8_320MSEC_MAG: IMP-8 Fluxgate Magnetometer, 320 msec Resolution Data - Adam Szabo, Joe King and Natalia Papitashvili (NASA GSFC)
I8_H0_GME: IMP-8 GME 30-min Fluxes (SEP optimal bands) - R.E. McGuire (SPDF (code632), NASA's GSFC)
I8_H0_MITPLASMA: IMP-8 MIT Plasma Investigation, High Resolution Definitive Data - A. Lazarus (MIT)
I8_OR_GIFWALK: Links to IMP-8 and multi-mission orbit plots - Polar-Wind-Geotail Ground System (NASA GSFC)
I8_OR_SSC: IMP-8 orbital position (multiple coordinate systems, from April 2003 updated I8 orbit model) - SSC ( SPDF/GSFC)
I8_R0_LEPEDEA: Link to IMP8 LEPEDEA Energy-Time Spectrograms in GIF format at the University of Iowa. - L. A. Frank (University of Iowa)
IA_K0_ENF: Interball Auroral Probemeasurements of spectra and anisotropy of electrons SKA-3, Key Parameters - Yu. Galperin, R. Kovrazhkin, A. Kuzmin, F. Shuiskaya (IKI RAN, Russia)
IA_K0_EPI: Interball Auroral Energetic Particle Instruments, Key Parameters - DOK-2: K.Kudela (DOK-2: Institute of experimental physics Slovak Acad. Sci., Kosize, Slovakia )
IA_K0_ICD: Interball Auroral Probe Ion Composition Experiment PROMICS, Key Parameters - I.Sandahl (IRF, Kiruna, Sweden)
IA_K0_MFI: Interball Auroral probe Magnetic Field, Key Parameters - V.Petrov (IZMIRAN,Troitsk, Russia. )
IA_OR_DEF: Interball Tail Orbital Data, Key Parameters - V.Prokhorenko (Space Research Inst., Russian Acad. Sci., Moscow, Russia. )
IBEX_H3_ENA_HI_R10_CG_NOSP_ANTIRAM_1YR: IBEX-Hi Release-10; Compton-Getting, no Survival-Probability, antiram-direction 1-year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_CG_NOSP_ANTIRAM_7YR: IBEX-Hi Release-10; Compton-Getting, no Survival-Probability, antiram-direction 7-year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_CG_NOSP_OMNI_6MO: IBEX-Hi Release-10; Compton-Getting, no Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_CG_NOSP_OMNI_7YR: IBEX-Hi Release-10; Compton-Getting, no Survival-Probability, omni-direction 7-year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_CG_NOSP_RAM_1YR: IBEX-Hi Release-10; Compton-Getting, no Survival-Probability, ram-direction 1-year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_CG_NOSP_RAM_7YR: IBEX-Hi Release-10; Compton-Getting, no Survival-Probability, ram-direction 7-year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_CG_SP_ANTIRAM_1YR: IBEX-Hi Release-10; Compton-Getting, Survival-Probability, AntiRAMdirectional 1-year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_CG_SP_ANTIRAM_7YR: IBEX-Hi Release-10; Compton-Getting, Survival-Probability, antiram-direction 7-year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_CG_SP_OMNI_6MO: IBEX-Hi Release-10; Compton-Getting, Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_CG_SP_OMNI_7YR: IBEX-Hi Release-10; Compton-Getting, Survival-Probability, omni-direction 7-year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_CG_SP_RAM_1YR: IBEX-Hi Release-10; Compton-Getting, Survival-Probability, RAMdirectional 1-year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_CG_SP_RAM_7YR: IBEX-Hi Release-10; Compton-Getting, Survival-Probability, ram-direction 7-year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_NOCG_NOSP_ANTIRAM_1YR: IBEX-Hi Release-10; no Compton-Getting, no Survival-Probability, antiram-direction 1-year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_NOCG_NOSP_ANTIRAM_7YR: IBEX-Hi Release-10; no Compton-Getting, no Survival-Probability, antiram-direction 7-year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_NOCG_NOSP_OMNI_6MO: IBEX-Hi Release-10; no Compton-Getting, no Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_NOCG_NOSP_OMNI_7YR: IBEX-Hi Release-10; no Compton-Getting, no Survival-Probability, omni-direction 7-year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_NOCG_NOSP_RAM_1YR: IBEX-Hi Release-10; no Compton-Getting, no Survival-Probability, ram-direction 1-year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_NOCG_SP_ANTIRAM_1YR: IBEX-Hi Release-10; no Compton-Getting, Survival-Probability, antiram-direction 1-year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_NOCG_SP_ANTIRAM_7YR: IBEX-Hi Release-10; no Compton-Getting, Survival-Probability, antiram-direction 7-year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_NOCG_SP_OMNI_6MO: IBEX-Hi Release-10; no Compton-Getting, Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_NOCG_SP_OMNI_7YR: IBEX-Hi Release-10; no Compton-Getting, Survival-Probability, omni-direction 7-year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R10_NOCG_SP_RAM_1YR: IBEX-Hi Release-10; no Compton-Getting, Survival-Probability, ram-direction 1-year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R12_MAGNETOSPHERE_24MIN: IBEX-Hi Release-12; Count Data for Magnetospheric Imaging. - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R13_CG_NOSP_ANTIRAM_1YR: IBEX-Hi Release-13; Compton-Getting, no Survival-Probability, antiram-direction 1-year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R13_CG_NOSP_RAM_1YR: IBEX-Hi Release-13; Compton-Getting, no Survival-Probability, ram-direction 1-year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_HI_R14_PRESS-SLOPE_CG_NOSP_RAM_3YR: IBEX-Hi Release-14; Compton-Getting, no Survival-Probability, ram-direction 3-year-Average West Ecliptic Pressure andFlux Power-Law Slope Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_LO_R09_PARK_OMAP_3YR: IBEX-Lo Release-09; Park et al. 2015) 3-year combined heavy neutral maps: m1-to-m6 (map1 + map2 + map3 + map4 + map5 + map6) West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_LO_R09_PARK_OMAP_3YR-EVEN-MAPS: IBEX-Lo Release-09; Park et al. 2015) 3-year combined heavy neutral even maps: m2m4m6 (map2 + map4 + map6) West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_LO_R09_PARK_OMAP_3YR-ODD-MAPS: IBEX-Lo Release-09; Park et al. 2015) 3-year combined heavy neutral odd maps: m1m3m5 (map1 + map3 + map5) West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_LO_R09_PARK_OMAP_6MO: IBEX-Lo Release-09; Park Oxygen Map Counting Rate 6-month-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_LO_R09_PARK_OMAP_STAT_3YR: IBEX-Lo Release-09; Park et al. (2015) 3-year combined heavy neutral maps: m1-to-m6 (map1 + map2 + map3 + map4 + map5 + map6) with statistical filtering - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_LO_R10_NOCG_NOSP_OMNI_6MO: IBEX-Lo Release-10; no Compton-Getting, no Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_LO_R10_NOCG_NOSP_OMNI_7YR: IBEX-Lo Release-10; no Compton-Getting, no Survival-Probability, Omnidirectional 7-Year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_LO_R10_NOCG_SP_OMNI_6MO: IBEX-Lo Release-10; no Compton-Getting, Survival-Probability, Omnidirectional 6-month-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IBEX_H3_ENA_LO_R10_NOCG_SP_OMNI_7YR: IBEX-Lo Release-10; no Compton-Getting, Survival-Probability, Omnidirectional 7-Year-Average West Ecliptic Maps - Dr. David J. McComas (Princeton University)
IG_K0_PCI: Interball Polar Cap Activity Index, Key Parameters - V.Sergeev (Institute of physics Univ. of St.-Peterburg St.-Peterburg, Russia )
IMAGE_M2_EUV: Imager for Magnetospause-to-Aurora Global Extreme Ultraviolet Imager Modified Data 2 - R. M. Katus (Eastern Michigan University)
IM_ELECTRON_DENSITY_RPI: RPI Dynamic Spectrogram, Electron Plasma, IMAGE Radio Plasma Imager (RPI) - B.W. Reinisch (UMLCAR)
IM_HK_ADS: Image Attitude Determination System Housekeeping - Dr. Jim Burch (Southwest Research Institute)
IM_HK_AST: Image Autonomous Star Tracker Housekeeping - Dr. Jim Burch (Southwest Research Institute)
IM_HK_COM: Image Communication Systems Housekeeping - Dr. Jim Burch (Southwest Research Institute)
IM_HK_FSW: IMAGE FSW - Dr. Jim Burch (Southwest Research Institute)
IM_HK_PWR: Image Power Systems Housekeeping - Dr. Jim Burch (Southwest Research Institute)
IM_HK_TML: Image Thermal Housekeeping - Dr. Jim Burch (Southwest Research Institute)
IM_K0_EUV: Ion Images, Key Parameters, IMAGE Extreme UltraViolet (EUV) experiment - W. Sandel (U/Arizona)
IM_K0_HENA: Image HIGH ENERGY NEUTRAL ATOM IMAGER Key Parameter - Dr. Don Mitchell (APL)
IM_K0_LENA: Image LOW ENERGY NEUTRAL ATOM IMAGER Key Parameter - Dr. Tom Moore (GSFC)
IM_K0_MENA: Image MEDIUM ENERGY NEUTRAL ATOM IMAGER Key Parameter - Dr. Craig Pollock (SwRI)
IM_K0_RPI: RPI Plasmagram/Echomap, Key Parameters, IMAGE Radio Plasma Imager (RPI) - B.W. Reinisch (UMLCAR)
IM_K0_SIE: Image Spectrographic Imaging Camera Key parameter - S. Mende (UC/Berkeley/SSL)
IM_K0_SIP: Image Spectrographic Imaging Camera Key parameter - S. Mende (UC/Berkeley/SSL)
IM_K0_WIC: Image Wide-Band Imaging Camera Key parameter - S. Mende (UC/Berkeley/SSL)
IM_K1_RPI: RPI Dynamic Spectrogram, Key Parameters, IMAGE Radio Plasma Imager (RPI) - B.W. Reinisch (UMLCAR)
IM_OR_DEF: IMAGE Definitive Orbit - Dr. Jim Burch (Southwest Research Institute)
IM_OR_GIFWALK: Link to IMAGE orbit plots - Polar-Wind-Geotail Ground System (NASA GSFC)
IM_OR_PRE: IMAGE Predicted Orbit - Dr. Jim Burch (Southwest Research Institute)
ISEE-3_HELIO1DAY_POSITION: Position in heliocentric coordinates from SPDF Helioweb - Natalia Papitashvili (NASA/GSFC/SPDF)
ISEE-3_MAGPLASMA_2MIN_MAGNETIC_FIELD_PLASMA: 2 min averaged magnetic field and plasma - Edward Smith (JPL NASA)
ISEE-3_MAG_1MIN_MAGNETIC_FIELD: 1 min averaged magnetic field - Edward Smith (JPL NASA)
ISEE1_4SEC_MFI: 12-sec avg vector magnetic field at 4-sec intervals - C. T. Russell (UCLA)
ISEE1_60SEC_MFI: 60-sec vector magnetic field - C. T. Russell (UCLA)
ISEE1_H0_FE: ISEE1_Fast Electrons - K. Ogilvie (GSFC Code 690)
ISEE1_H1_FPE: ISEE 1_H1_FPE / Proton Fluid Parameters 6 RE - Bow Shock - S. Bame & J. Gosling (LANL)
ISEE1_H2_FPE: ISEE 1_H2_FPE / Solar Wind 24-sec Ion Moments - S. Bame & J. Gosling (LANL)
ISEE1_PWI_SA: ISEE-1 PWI: Spectrum Analyzer (SA) - Donald Gurnett (University Iowa)
ISEE1_PWI_SA-RAPID-E: ISEE-1 PWI: Spectrum Analyzer (SA) rapid samples - Donald Gurnett (University Iowa)
ISEE1_PWI_SFR-E: ISEE-1 PWI: Sweep Frequency Receiver (SFR) - Donald Gurnett (University Iowa)
ISEE2_4SEC_MFI: 12-sec avg vector magnetic field at 4-sec intervals - C. T. Russell (UCLA)
ISEE2_60SEC_MFI: 60-sec vector magnetic field - C. T. Russell (UCLA)
ISEE2_H1_FPE: ISEE 2_H1_FPE / Proton Fluid Parameters 6 RE - Bow Shock - G. Paschmann (MPE)
ISS_27DAY-AVERAGES_AMS-02: AMS-02 proton flux (p), helium flux (He), p/He flux ratio, electron flux (e-), positron flux (e+) and e+/e- flux ratio at Bartels rotation time resolution - Prof. V. Bindi (University of Hawaii at Manoa)
ISS_DOSANL_TEPC: Experiment Data, ISS TEPC (from ASCII DOS.TXT file) - Edward Semones (NASA Space Radiation Analysis Group/Johnson Space Center)
ISS_SP_FPMU: ISS FPMU Summary Plasma Densities and Temperatures [Contact Rob.Suggs@nasa.gov for support and use.] - R. Suggs (NASA Marshall Space Flight Center)
IT_H0_MFI: Interball-Tail 6 sec vector magnetic field data - M.Nozdrachev (IKI, Moscow, Russia)
IT_K0_AKR: Interball Tail Probe AKR Radioemission flux, Key Parameters - V.Kurilchik (Sternberg Astronomical Inst.,Moscow State University, 119899, Universitetsky pr., 13 Moscow, Russia)
IT_K0_COR: Interball Tail Probe CORALL ion moments, Key Parameters - Yu.Yermolaev (Space Research Inst., Russian Acad. Sci., Moscow, Russia)
IT_K0_ELE: Interball Tail probe ELECTRON instrument, Key Parameters - J.-A. Sauvaud (CESR, BP 4346, 31029, Toulouse, France )
IT_K0_EPI: Interball Tail Energetic Particle Instruments, Key Parameters - DOK-2: K.Kudela (DOK-2: Institute of experimental physics Slovak Acad. Sci., Kosize, Slovakia )
IT_K0_ICD: Interball Tail Probe Ion Composition Experiment PROMICS, Key Parameters - I.Sandahl (IRF, Kiruna, Sweden)
IT_K0_MFI: Interball Tail probe Magnetic Field, Key Parameters - S.Romanov (Space Research Inst., Russian Acad. Sci., Moscow, Russia. )
IT_K0_VDP: Interball Tail probe VDP instrument, Key Parameters - J.Safrankova (Charles University, Prague, Czech Republic )
IT_K0_WAV: Interball Tail probe Magnetic Field, Key Parameters - S.Romanov (Space Research Inst., Russian Acad. Sci., Moscow, Russia. )
IT_OR_DEF: Interball Tail Orbital Data, Key Parameters - V.Prokhorenko (Space Research Inst., Russian Acad. Sci., Moscow, Russia. )
IT_OR_GIFWALK: Links to Interball-Tail and multi-mission orbit plots - Polar-Wind-Geotail Ground System (NASA GSFC)

I1_AV2_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 673). 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 https://spdf.gsfc.nasa.gov/isis/isis-status.html 
Modification History
created December 2017
 
Dataset in CDAWeb
Back to top
I1_AV2_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 673). 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 https://spdf.gsfc.nasa.gov/isis/isis-status.html 
Modification History
created December 2017
 
Dataset in CDAWeb
Back to top
I1_AV2_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 673). 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 https://spdf.gsfc.nasa.gov/isis/isis-status.html 
Modification History
created December 2017
 
Dataset in CDAWeb
Back to top
I1_AV_ALL (spase://VSPO/NumericalData/ISIS1/SFS/Ionogram/PT29S)
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
 
Dataset in CDAWeb
Back to top
I1_AV_KER (spase://VSPO/NumericalData/ISIS1/SFS/AverageIonogram/KerguelenIsland/PT29S)
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
 
Dataset in CDAWeb
Back to top
I1_AV_KSH (spase://VSPO/NumericalData/ISIS1/SFS/AverageIonogram/Kashima/PT29S)
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
 
Dataset in CDAWeb
Back to top
I1_AV_KWA (spase://VSPO/NumericalData/ISIS1/SFS/AverageIonogram/Kwajalein/PT29S)
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
 
Dataset in CDAWeb
Back to top
I1_AV_ODG (spase://VSPO/NumericalData/ISIS1/SFS/AverageIonogram/Ouagadougou/PT29S)
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
 
Dataset in CDAWeb
Back to top
I1_AV_ORR (spase://VSPO/NumericalData/ISIS1/SFS/AverageIonogram/Orroral/PT29S)
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
 
Dataset in CDAWeb
Back to top
I1_AV_OTT (spase://VSPO/NumericalData/ISIS1/SFS/AverageIonogram/Ottawa/PT29S)
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
 
Dataset in CDAWeb
Back to top
I1_AV_QUI (spase://VSPO/NumericalData/ISIS1/SFS/AverageIonogram/Quito/PT29S)
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
 
Dataset in CDAWeb
Back to top
I1_AV_RES (spase://VSPO/NumericalData/ISIS1/SFS/AverageIonogram/ResoluteBay/PT29S)
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
 
Dataset in CDAWeb
Back to top
I1_AV_SNT (spase://VSPO/NumericalData/ISIS1/SFS/AverageIonogram/Santiago/PT29S)
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
 
Dataset in CDAWeb
Back to top
I1_AV_SOD (spase://VSPO/NumericalData/ISIS1/SFS/AverageIonogram/Sodankyla/PT29S)
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
 
Dataset in CDAWeb
Back to top
I1_AV_TRO (spase://VSPO/NumericalData/ISIS1/SFS/AverageIonogram/Tromso/PT29S)
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
 
Dataset in CDAWeb
Back to top
I1_AV_ULA (spase://VSPO/NumericalData/ISIS1/SFS/AverageIonogram/Fairbanks/PT29S)
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
 
Dataset in CDAWeb
Back to top
I1_AV_WNK (spase://VSPO/NumericalData/ISIS1/SFS/AverageIonogram/Winkfield/PT29S)
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
 
Dataset in CDAWeb
Back to top
I1_NEPROF_TOPS (spase://VSPO/NumericalData/ISIS1/SFS/TOPS)
Description
This data set, provided by the Communications Research Centre (CRC) in Ottawa,
Canada, consists of electron density profiles for the ionosphere above the F2
maximum (topside ionosphere). The data were computed from the orginal ionograms
using Jackson's method (Jackson, Proceedings of the IEEE., p. 960, June 1969).
ISIS-1 was launched on 1969-01-30 into an elliptical orbit (500-3500km) with an
inclination of 88.4 degrees and ISIS-2 was launched on 1971-04-01 into an
circular orbit at 1400 km with an inclination of 88.1 degrees.
Both satellites were fully instrumented ionospheric observatories including
sweep- and fixed-frequequency ionosondes, a VLF receiver, energetic and soft
particle detectors, an ion mass spectrometer, an electrostatic analyzer, an
Langmuir probe, a beacon transmitter, a cosmic noise experiment and ISIS 2 also
carried two photometers. A tape recorder with 1-h capacity was included on both
satellites. Data were also collected during overflights of several telemetry
stations. The telemetry stations were in areas that provided primary data
coverage near the 80-deg-W meridian and in areas near Hawaii, Singapore,
Australia, the UK, Norway, India, Japan, Antarctica, New Zealand, and Central
Africa.
 
Dataset in CDAWeb
Back to top
I2_AV_ACN (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/AscensionIsland/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_ADL (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/TerreAdelie/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_AME (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/Ahmedabad/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_BRZ (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/Brazzaville/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_BUR (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/Johannesburg/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_CNA (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/LasPalmas/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_KER (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/KerguelenIsland/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_KRU (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/Kourou/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_KSH (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/Kashima/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_KWA (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/Kwajalein/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_LAU (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/Lauder/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_ODG (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/Ouagadougou/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_ORR (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/Orroral/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_OTT (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/Ottawa/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_QUI (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/Quito/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_RES (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/ResoluteBay/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_SNT (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/Santiago/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_SOD (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/Sodankyla/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_SOL (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/FalklandIslands/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_SYO (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/SyowaBase/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_TRO (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/Tromso/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_ULA (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/Fairbanks/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_AV_WNK (spase://VSPO/NumericalData/ISIS2/SFS/AverageIonogram/Winkfield/PT22S)
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
 
Dataset in CDAWeb
Back to top
I2_NEPROF_TOPIST (spase://VSPO/NumericalData/ISIS2/SFS/TOPIST)
Description
ISIS 2 was an ionospheric observatory instrumented with a sweep- and a
fixed-frequency ionosonde, a VLF receiver, energetic and soft particle
detectors, an ion mass spectrometer, an electrostatic probe, a retarding
potential analyzer, a beacon transmitter, a cosmic noise experiment, and two
photometers. Two long crossed-dipole antennas (73 and 18.7 m) were used for the
sounding, VLF, and cosmic noise experiments.
The spacecraft was spin-stabilized to about 2 rpm after antenna deployment.
There were two basic orientation modes for the spacecraft, cartwheel and
orbit-aligned. The spacecraft operated approximately the same length of time in
each mode, remaining in one mode typically 3 to 5 months. The cartwheel mode
with the axis perpendicular to the orbit plane was made available to provide ram
and wake data for some experiments for each spin period, rather than for each
orbit period. Attitude and spin information was obtained from a three-axis
magnetometer and a sun sensor. Control of attitude and spin was possible by
means of magnetic torquing.
The experiment package also included a programmable tape recorder with a one
hour capacity. For non-recorded observations, data from satellite and
subsatellite regions were telemetered when the spacecraft was in the line of
sight of a telemetry station. Telemetry stations were located so that primary
data coverage was near the 80-deg-W meridian and near Hawaii, Singapore,
Australia, England, France, Norway, India, Japan, Antarctica, New Zealand, and
Central Africa. NASA support of the ISIS project was terminated on October 1,
1979.  
A significant amount of experimental data, however, was acquired after this date
by the Canadian project team. ISIS 2 operations were terminated in Canada on
March 9, 1984. The Radio Research Laboratories (Tokyo, Japan) then requested and
received permission to reactivate ISIS 2. Regular ISIS 2 operations were started
from Kashima, Japan, in early August 1984. ISIS 2 was deactivated effective 24,
1990. A data restoration effort began in the late 1990s and successfully saved a
considerable portion of the high-resolution data before the telemetry tapes were
discarted.
The data set was generated from the averaged ionogram binary data (SPIO-00318)
recorded by the Topside Sounder. The data are obtained with the TOPIST program,
which analyzes the data, automatically scales the ionogram traces and
resonances, and inverts the traces into an electron density profile. The same
program is available for use to hand-scale the data if desired. Output data
items include spacecraft position, electron density profile, assessment of
quality, resonance and cut-off frequencies, and both the O-trace and X-trace.
 
Dataset in CDAWeb
Back to top
I2_NEPROF_TOPS (spase://VSPO/NumericalData/ISIS2/SFS/TOPS)
Description
This data set, provided by the Communications Research Centre (CRC) in Ottawa,
Canada, consists of electron density profiles for the ionosphere above the F2
maximum (topside ionosphere). The data were computed from the orginal ionograms
using Jackson's method (Jackson, Proceedings of the IEEE., p. 960, June 1969).
ISIS-1 was launched on 1969-01-30 into an elliptical orbit (500-3500km) with an
inclination of 88.4 degrees and ISIS-2 was launched on 1971-04-01 into an
circular orbit at 1400 km with an inclination of 88.1 degrees.
Both satellites were fully instrumented ionospheric observatories including
sweep- and fixed-frequequency ionosondes, a VLF receiver, energetic and soft
particle detectors, an ion mass spectrometer, an electrostatic analyzer, an
Langmuir probe, a beacon transmitter, a cosmic noise experiment and ISIS 2 also
carried two photometers. A tape recorder with 1-h capacity was included on both
satellites. Data were also collected during overflights of several telemetry
stations. The telemetry stations were in areas that provided primary data
coverage near the 80-deg-W meridian and in areas near Hawaii, Singapore,
Australia, the UK, Norway, India, Japan, Antarctica, New Zealand, and Central
Africa.
 
Dataset in CDAWeb
Back to top
I7_R0_LEPEDEA
Description
No TEXT global attribute value.
 
Dataset in CDAWeb
Back to top
I8_15SEC_MAG (spase://VSPO/NumericalData/IMP8/MAG/PT15.36S)
Description
This 15.36s data set was created in 2008-9 at GSFC/SPDF from a newly created
320ms data set, with some gaps filled with data from the prior 15.36s data set. 
Full documentation may be found at
ftp://nssdcftp.gsfc.nasa.gov/spacecraft_data/imp/imp8/mag/15s_ascii_v3/00_IMP8_1
5s_data_docum.txt.  Creation of the new 320ms and 15.36s data sets was done by
N. Papitashvili and J. King, with guidance from Adam Szabo. 
Modification History
Master CDF made 02/16/10 by N. E. Papitashvili, SPDF Modified to revised form
v03 on 02/16/10.
 
Dataset in CDAWeb
Back to top
I8_320MSEC_MAG (spase://VSPO/NumericalData/IMP8/MAG/PT0.32S)
Description
For detailed documentation on the creation of this data set see
ftp://omniweb.gsfc.nasa.gov/imp8/mag/320ms_ascii/cleaned/doc/imp8_mag_320ms_proc
.txt
 
Dataset in CDAWeb
Back to top
I8_H0_GME (spase://VSPO/NumericalData/IMP8/GME/PT30M)
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
 
Dataset in CDAWeb
Back to top
I8_H0_MITPLASMA (spase://VSPO/NumericalData/IMP8/PLS/PT01M)
Description
See online MIT documentation
Modification History
 CDF versions created August 2004
 
Dataset in CDAWeb
Back to top
I8_OR_GIFWALK
Description
Pre-generated PWG plots
 
Dataset in CDAWeb
Back to top
I8_OR_SSC (spase://VSPO/NumericalData/IMP8/Ephemeris/PT12M)
Description
GROUP 1    Satellite   Resolution   Factor
            imp8          720         1
           Start Time           Stop Time 
           2004   1 00:00       2004 182 24:00   
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      -        -        -           -        -           -   
GSE LT       YES      -        -        -           -        -           -   
GSM X        YES      -        -        -           -        -           -   
GSM Y        YES      -        -        -           -        -           -   
GSM Z        YES      -        -        -           -        -           -   
GSM Lat      YES      -        -        -           -        -           -   
GSM 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: Earth radii with 2 place(s).
Modification History
Originated 03/14/96
 
Dataset in CDAWeb
Back to top
I8_R0_LEPEDEA
Description
No TEXT global attribute value.
 
Dataset in CDAWeb
Back to top
IA_K0_ENF (spase://VSPO/NumericalData/Interball-2/SK3/KP/PT120S)
Description
Measurements of spectra and anisotropy of electrons witin energy ranges 20-40
keV from two time-of-flight detectors EM-1-1 and EM-1-2. The field of view of
these detectors are directed oppositely and perpendicular to the satellite 
rotation axis. 
Data description:  http://www.iki.rssi.ru/inte rball.html  
Modification History
created Sep 1998
 
Dataset in CDAWeb
Back to top
IA_K0_EPI (spase://VSPO/NumericalData/Interball-2/DOK2A/KP/PT120S)
Description
No TEXT global attribute value.
Modification History
created Apr 1997
 
Dataset in CDAWeb
Back to top
IA_K0_ICD (spase://VSPO/NumericalData/Interball-2/PROMICS3/KP/PT120S)
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 Sep 1998
 
Dataset in CDAWeb
Back to top
IA_K0_MFI (spase://VSPO/NumericalData/Interball-2/IMAP3/PT120S)
Description
Full description: http://www.iki.rssi.ru/interball.html 
Full description: http://www.iki.rssi.ru/interball.html 
Modification History
created May 1997
 
Dataset in CDAWeb
Back to top
IA_OR_DEF (spase://VSPO/NumericalData/Interball-2/Ephemeris/PT120S)
Description
Full description: http://www.iki.rssi.ru/interball.html 
Full description: http://www.iki.rssi.ru/interball.html 
Modification History
created May 1997
edited global attributes Apr 1996
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_CG_NOSP_ANTIRAM_1YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/CG/NOSP/ANTIRAM/1yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 one-year IBEX-Hi map data for the first
seven years, 2009-2015, in the form of antiram-direction fluxes with corrections
for spacecraft motion (cg: Compton-Getting) but with no corrections (sp) for ENA
survival probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is
associated with two consecutive maps;
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as
hvset_noSP_antiram_cg_yearN for N=1,7, includes pixel map data from antiram
direction, CG, noSP, 1 year cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_CG_NOSP_ANTIRAM_7YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/CG/NOSP/ANTIRAM/7yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 seven-year IBEX-Hi map data for
2009-2015, in the form of antiram-direction fluxes with corrections for
spacecraft motion (cg: Compton-Getting) but with no corrections (sp) for ENA
survival probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is
associated with two consecutive maps;
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as
hvset_noSP_antiram_cg_ single, includes pixel map data from antiram direction,
CG, noSP, 7 year cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_CG_NOSP_OMNI_6MO (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/CG/noSP/Omni/6mo)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 (6 months-cadence) IBEX-Hi map data for
the first seven years, 2009-2015, in the form of omnidirectional ENA (hydrogen)
fluxes with Compton-Getting correction (cg) of flux spectra for spacecraft 
motion and no correction (nosp) for ENA survival probability between 1 and 100
AU. 
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015): 
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as
hvset_cg_mapN for N=1,14, includes pixel map data from all directions
(omnidirectional), CG, no SP, 6 month cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_CG_NOSP_OMNI_7YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/CG/NOSP/OMNI/7yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 seven-year IBEX-Hi map data for
2009-2015, in the form of omni-direction fluxes with corrections for spacecraft
motion (cg: Compton-Getting) but with no corrections (sp) for ENA survival
probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is
associated with two consecutive maps;
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as hvset_cg_
single, includes pixel map data from omni direction, CG, noSP, 7 year cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_CG_NOSP_RAM_1YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/CG/NOSP/RAM/1yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 one-year IBEX-Hi map data for the first
seven years, 2009-2015, in the form of ram-direction fluxes with corrections for
spacecraft motion (cg: Compton-Getting) but with no corrections (sp) for ENA
survival probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is
associated with two consecutive maps;
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as
hvset_noSP_ram_cg_yearN for N=1,7, includes pixel map data from RAM direction
(ram-direction), CG, noSP, 1 year cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_CG_NOSP_RAM_7YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/CG/NOSP/RAM/7yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 seven-year IBEX-Hi map data for
2009-2015, in the form of ram-direction fluxes with corrections for spacecraft
motion (cg: Compton-Getting) but with no corrections (sp) for ENA survival
probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is
associated with two consecutive maps;
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as
hvset_noSP_ram_cg_ single, includes pixel map data from ram direction, CG, noSP,
7 year cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_CG_SP_ANTIRAM_1YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/CG/SP/AntiRAM/1yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 (1-year-cadence) IBEX-Hi map data for
the first seven years, 2009-2015, in the form of anti-RAM-directional fluxes
with corrections for spacecraft motion (cg: Compton-Getting) and with
corrections (sp) for ENA survival probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is
associated with two consecutive maps;
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as
hvset_tabular_antiram_cg_yearN for N=1,7, includes pixel map data from antiRAM
direction (antiRAMdirectional), CG, SP, 1 year cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_CG_SP_ANTIRAM_7YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/CG/SP/ANTIRAM/7yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 seven-year IBEX-Hi map data for
2009-2015, in the form of antiram-direction fluxes with corrections for
spacecraft motion (cg: Compton-Getting) and with corrections (sp) for ENA
survival probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is
associated with two consecutive maps;
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as
hvset_tabular_antiram_cg_single, includes pixel map data from antiram direction,
CG,SP, 7 year cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_CG_SP_OMNI_6MO (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/CG/SP/Omni/6mo)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 (6 months-cadence) IBEX-Hi map data for
the first seven years, 2009-2015, in the form of omnidirectional fluxes with
corrections (cg) for spacecraft motion (Compton-Getting) and corrections (sp)
for ENA survival probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015): 
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as
hvset_cg_tabular_mapN for N=1,14, includes pixel map data from all directions
(omnidirectional), CG, SP, 6 month cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_CG_SP_OMNI_7YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/CG/SP/OMNI/7yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 seven-year IBEX-Hi map data for
2009-2015, in the form of omni-direction fluxes with corrections for spacecraft
motion (cg: Compton-Getting) and with corrections (sp) for ENA survival
probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is
associated with two consecutive maps;
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as
hvset_cg_tabular_ single, includes pixel map data from omni direction, CG,SP, 7
year cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_CG_SP_RAM_1YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/CG/SP/RAM/1yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 (1-year-cadence) IBEX-Hi map data for
the first seven years, 2009-2015, in the form of RAM-directional fluxes with
corrections for spacecraft motion (cg: Compton-Getting) and with corrections
(sp) for ENA survival probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is
associated with two consecutive maps;
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as
hvset_tabular_ram_cg_yearN for N=1,7, includes pixel map data from RAM direction
(RAMdirectional), CG, SP, 1 year cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_CG_SP_RAM_7YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/CG/SP/RAM/7yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 seven-year IBEX-Hi map data for
2009-2015, in the form of ram-direction fluxes with corrections for spacecraft
motion (cg: Compton-Getting) and with corrections (sp) for ENA survival
probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is
associated with two consecutive maps;
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as
hvset_tabular_ram_cg_single, includes pixel map data from ram direction, CG,SP,
7 year cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_NOCG_NOSP_ANTIRAM_1YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/NOCG/NOSP/ANTIRAM/1yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 one-year IBEX-Hi map data for the first
seven years, 2009-2015, in the form of antiram-direction fluxes with no
corrections for spacecraft motion (nocg: no Compton-Getting) and with no
corrections (nosp) for ENA survival probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is
associated with two consecutive maps;
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as
hvset_noSP_antiram_yearN for N=1,7, includes pixel map data from antiram
direction, CG, noSP, 1 year cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_NOCG_NOSP_ANTIRAM_7YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/NOCG/NOSP/ANTIRAM/7yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 seven-year IBEX-Hi map data for
2009-2015, in the form of antiram-direction fluxes with no corrections for
spacecraft motion (nocg: Compton-Getting) and with no corrections (nosp) for ENA
survival probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is
associated with two consecutive maps;
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as
hvset_noSP_antiram_single, includes pixel map data from antiram direction, noCG,
noSP, 7 year cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_NOCG_NOSP_OMNI_6MO (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/noCG/noSP/Omni/6mo)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 (6 months-cadence) IBEX-Hi map data for
the first seven years, 2009-2015, in the form of omnidirectional fluxes without
any corrections (nocg) for spacecraft motion (Compton-Getting) and ENA survival
probability (nosp) between 1 and 100 AU.
3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015): 
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as hvset_mapN
for N=1,14, includes pixel map data from all directions (omnidirectional), no
CG, no SP, 6 month cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_NOCG_NOSP_OMNI_7YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/NOCG/NOSP/OMNI/7yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 seven-year IBEX-Hi map data for
2009-2015, in the form of omni-direction fluxes with no corrections for
spacecraft motion (nocg: Compton-Getting) and with no corrections (nosp) for ENA
survival probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is
associated with two consecutive maps;
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as
hvset_single, includes pixel map data from omni direction, noCG, noSP, 7 year
cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_NOCG_NOSP_RAM_1YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/NOCG/NOSP/RAM/1yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 one-year IBEX-Hi map data for the first
seven years, 2009-2015, in the form of ram-direction fluxes with no corrections
for spacecraft motion (nocg: no Compton-Getting) and with no corrections (nosp)
for ENA survival probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is
associated with two consecutive maps;
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as
hvset_noSP_ram_yearN for N=1,7, includes pixel map data from antiram direction,
CG, noSP, 1 year cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_NOCG_SP_ANTIRAM_1YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/NOCG/SP/ANTIRAM/1yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 one-year IBEX-Hi map data for the first
seven years, 2009-2015, in the form of antiram-direction fluxes with no
corrections for spacecraft motion (nocg: no Compton-Getting) and with
corrections (sp) for ENA survival probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is
associated with two consecutive maps;
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as
hvset_tabular_noSP_antiram_yearN for N=1,7, includes  pixelmap data from anti
ramdirection, noCG, SP, 1 year cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_NOCG_SP_ANTIRAM_7YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/NOCG/SP/ANTIRAM/7yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 seven-year IBEX-Hi map data for
2009-2015, in the form of antiram-direction fluxes with no corrections for
spacecraft motion (nocg: Compton-Getting) but with corrections (sp) for ENA
survival probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is
associated with two consecutive maps;
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as
hvset_tabular_antiram_single, includes pixel map data from antiram direction,
noCG, SP, 7 year cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_NOCG_SP_OMNI_6MO (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/noCG/SP/Omni/6mo)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 (6 months-cadence) IBEX-Hi map data for
the first seven years, 2009-2015, in the form of omnidirectional fluxes with no
corrections for spacecraft motion (Compton-Getting) but with corrections (sp)
for ENA survival probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015): 
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as
hvset_tabular_mapN for N=1,14, includes pixel map data from all directions
(omnidirectional), no CG, SP, 6 month cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_NOCG_SP_OMNI_7YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/NOCG/SP/OMNI/7yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 seven-year IBEX-Hi map data for
2009-2015, in the form of omni-direction fluxes with no corrections for
spacecraft motion (nocg: Compton-Getting) but with corrections (sp) for ENA
survival probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is
associated with two consecutive maps;
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as
hvset_tabular_single, includes pixel map data from omni direction, noCG, noSP, 7
year cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R10_NOCG_SP_RAM_1YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R10/NOCG/SP/RAM/1yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 one-year IBEX-Hi map data for the first
seven years, 2009-2015, in the form of ram-direction fluxes with no corrections
for spacecraft motion (nocg: no Compton-Getting) and with corrections (sp) for
ENA survival probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015); each year is
associated with two consecutive maps;
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: This particular data set, denoted in the original ascii files as
hvset_tabular_noSP_ram_yearN for N=1,7, includes  pixelmap data from
ramdirection, noCG, SP, 1 year cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R12_MAGNETOSPHERE_24MIN (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R12/Mag/24min)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2018. 
2: This data set is from the IBEX-Hi Release 12 Count Data for Magnetospheric
Imaging. This release provides data for various IBEX orbits from 23 (2009-03-26)
to 207b (2013-05-30). The data include 21 orbits from IBEX-Hi 6-degree histogram
ENA count data, which is primarily what have been used in IBEX magnetospheric
studies.
3. The data consist of IBEX-Hi Count Data for Magnetospheric Imaging during
instrument pointing in spin angle 0 - 360 degrees between the north and south
Ecliptic poles. Spin angle zero corresponds to the north Ecliptic pole. Counts
come from IBEX-Hi energy bands 2-6 in numerical data form corresponding to
energy bins 2-6: 2) ~0.71, 3) ~1.11, 4) ~1.74, 5) ~2.73, 6) ~4.3 keV. Background
counts have not been removed. Counts are separated into 6-degree latitudinal
bins, with each # angle label representing the center of the bin. Details of the
data and enabled science from Release 12 are given in the following journal
publications: McComas et al. 2011,2012b; Fuselier et al. 2010, 2015; Petrinec et
al. 2011; Ogasawara et al. 2013, 2019; and Dayeh et al. 2015Data Location:
http://ibex.swri.edu/ibexpublicdata/Data_Release_12/index.htmlContact: Maher
Dayeh, Southwest Research Institute, San Antonio, TX maldayeh@swri.edu 
Orbit Start and End Times:
23: 2009-03-26 21:09:00.318 to 2009-04-03 16:07:51.743
24: 2009-04-03 12:10:21.253 to 2009-04-11 08:15:09.669
25: 2009-04-11 05:06:40.967 to 2009-04-18 22:05:11.125
27: 2009-04-26 08:27:40.916 to 2009-05-04 05:31:06.519
28: 2009-05-04 02:02:57.673 to 2009-05-11 21:13:47.596
29: 2009-05-11 17:27:02.484 to 2009-05-19 19:27:18.831
51: 2009-10-26 08:19:34.905 to 2009-11-03 02:38:01.730
52: 2009-11-02 22:34:07.792 to 2009-11-10 19:03:55.230
53: 2009-11-10 15:46:22.161 to 2009-11-18 10:58:17.674
55: 2009-11-25 23:44:19.069 to 2009-12-03 11:26:37.151
56: 2009-12-03 08:22:31.792 to 2009-12-10 22:03:52.604
57: 2009-12-10 18:55:33.969 to 2009-12-18 06:58:47.247
72: 2010-04-04 11:17:28.386 to 2010-04-12 09:13:51.008
74: 2010-04-19 14:09:01.851 to 2010-04-27 03:44:14.913
77: 2010-05-12 01:33:51.796 to 2010-05-19 20:43:01.583
78: 2010-05-19 17:33:48.047 to 2010-05-27 13:02:03.396
103: 2010-11-26 07:56:05.324 to 2010-12-04 04:11:44.879
187a: 2012-11-21 00:17:13.430 to 2012-11-25 00:40:26.707
188b: 2012-12-03 12:46:18.859 to 2012-12-08 00:44:50.846
206a: 2013-05-13 23:15:27.433 to 2013-05-17 12:19:58.215
207b: 2013-05-26 12:21:08.868 to 2013-05-30 23:14:44.989
For the first two and a half years of science operations (through Orbit 127),
IBEX's orbital period was ~7.5 days and the spin axis was repointed once each
orbit (around perigee), leading to bands of sky viewing centered 7.5 apart. In
June 2011, over Orbits 128 and 129, IBEX was maneuvered into a previously
unknown, long-term stable lunar synchronous orbit with apogee still ~50 RE
(McComas et al. 2011a). Since then, IBEX's orbital period has been ~9.1 days
(one-third of the lunar sidereal period of 27.3 days). Orbit numbers from 130
onward are split into two segments, 'a' and 'b'. Furthermore, starting in orbit
segment 184a, the IBEX team modified the IBEX-Hi energy step sequence and
eliminated the lowest energy step (ESA1) in exchange for doubling the
statistical sampling of ESA3 (center energy ~1.1 keV).
Modification History
The IBEX Release 12 data 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R13_CG_NOSP_ANTIRAM_1YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R13/CG/NOSP/ANTIRAM/1yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2018. 
2: This data set is from the Release 13 one-year IBEX-Hi map data for the nine
years, 2009-2018, in the form of antiram-direction fluxes with corrections for
spacecraft motion (cg: Compton-Getting) but with no corrections (sp) for ENA
survival probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 13 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 13 map numbers (1-20) with mission year
(1-10), orbits (11-431bb), and dates (12/25/2008-12/26/2018); each year is
associated with two consecutive maps;
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
Map 15: year 8, orbits 311a-330b, dates 12/24/2015-06/23/2016
Map 16: year 8, orbits 331a-351a, dates 06/24/2016-12/26/2016
Map 17: year 9, orbits 351b-371a, dates 12/26/2016-06/25/2017
Map 18: year 9, orbits 371b-391a, dates 06/25/2017-12/25/2017
Map 19: year 10, orbits 391a-411b, dates 12/25/2017-06/28/2018
Map 20: year 10, orbits 412a-431b, dates 06/29/2018-12/26/2018
8: This particular data set, denoted in the original ascii files as
hvset_noSP_antiram_cg_yearN for N=8, includes pixel map data from antiram
direction, CG, noSP, 1 year cadence. 
Modification History
The Release 13 data extend through Map 20 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R13_CG_NOSP_RAM_1YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Hi/R13/CG/NOSP/RAM/1yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 14
releases of IBEX-HI and/or IBEX-LO data covering 2009-2018. 
2: This data set is from the Release 13 one-year IBEX-Hi map data for the nine
years, 2009-2018, in the form of ram-direction fluxes with corrections for
spacecraft motion (cg: Compton-Getting) but with no corrections (sp) for ENA
survival probability between 1 and 100 AU.  
3. The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Hi energy bands 2-6 in
numerical data form. Energy channels 2-6 have FWHM ranges of 0.52-0.95,
0.84-1.55, 1.36-2.50, 1.99-3.75, 3.13-6.00 keV, respectively. The corresponding
center-point energies are 0.71, 1.11, 1.74, 2.73, and 4.29 keV. Details of the
data and enabled science from Release 10 are given in the following journal
publication:
4: McComas, D. J., et al. (2017), Seven Years of Imaging the Global Heliosphere
with IBEX, Astrophys. J. Supp. Ser., 229(2), 41 (32 pp.), 
5: http://doi.org/10.3847/1538-4365/aa66d8  
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 13 map numbers (1-20) with mission year
(1-10), orbits (11-431bb), and dates (12/25/2008-12/26/2018); each year is
associated with two consecutive maps;
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
Map 15: year 8, orbits 311a-330b, dates 12/24/2015-06/23/2016
Map 16: year 8, orbits 331a-351a, dates 06/24/2016-12/26/2016
Map 17: year 9, orbits 351b-371a, dates 12/26/2016-06/25/2017
Map 18: year 9, orbits 371b-391a, dates 06/25/2017-12/25/2017
Map 19: year 10, orbits 391a-411b, dates 12/25/2017-06/28/2018
Map 20: year 10, orbits 412a-431b, dates 06/29/2018-12/26/2018
8: This particular data set, denoted in the original ascii files as
hvset_noSP_ram_cg_yearN for N=8, includes pixel map data from antiram direction,
CG, noSP, 1 year cadence. 
Modification History
The Release 13 data extend through Map 20 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_HI_R14_PRESS-SLOPE_CG_NOSP_RAM_3YR (spase://VSPO/NumericalData /IBEX/H3/ENA/Hi/R14/GDFRibbonPressSlope/CGNOSPRAM/3yr )
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 15
releases of IBEX-HI and/or IBEX-LO data covering 2009-2018. 
2: This data set is derived from the Release 14 three-year IBEX-Hi map data with
two-year overlaps to adjacent maps, 2009-2011, 2010-2012, 2011-2013, and so
forth through 2015-2017 from ram-direction fluxes with corrections for
spacecraft motion (cg: Compton-Getting) but with no corrections (sp) for ENA
survival probability between 1 and 100 AU. The data set parameters include
line-of-sight (LOS) integrated pressures separately computed from the Global
Distributed Flux (GDF), the ribbon flux, and the total of both LOS pressures.
Additionally there are signal/noise ratios for the GDF, ribbon, and total
pressures. Finally, there are power-law slope and values for the GDF
differential flux, also including signal/noise of the slope.  
3: The data consist of ram-direction sky maps in Solar Ecliptic Longitude (east
and west) and Latitude angles for the above parameters. 
4: Details of the data and enabled science from Release 14 are given in the
following journal publication: Schwadron, N. A., et al. (2018), Time Dependence
of the IBEX Ribbon and the Globally Distributed Energetic Neutral Atom Flux
Using the First 9 Years of Observations
https://iopscience.iop.org /article/10.3847/1538-4365/aae48e/meta
5: The following codes are used to define dataset types in the multiple IBEX
data releases:  
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
6: This particular dataset denoted in the original ascii files as:
-- GDFPressure: Globally Distributed Flux Line-of-Sight Integrated Pressure in
pdyne-au/cm^2
-- GDFSlope: Power-Law Slope of the differential flux spectrum for the Globally
Distributed Flux
-- GDFSlopeSN: Signal/Noise ratio of the GDF differential flux power-law slope
where noise represents uncertainty 
-- GDFSN: Globally Distributed Flux Signal/Noise, where Noise is defined as the
uncertainty and the Signal is GDF Line-of-Sight -integrated pressure
-- RibbonPressure: Ribbon Line-of-Sight Integrated Pressure in pdyne-au/cm^2
-- RibbonSN: Ribbon Signal/Noise, where Noise is defined as the uncertainty and
the Signal is GDF  Line-of-Sight -integrated pressure
-- TotPressure: Total Pressure in ENA maps including both the GDF and Ribbon.
Line-of-Sight Integrated Pressure in pdyne-au/cm^2
-- TotSN: Total Pressure Signal-to-Noise where noise represents uncertainty and
signal represents the total LOS-integrated pressure
Modification History
The Release 14 data extend through Map 20 and contain modifications and updates
of Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release
7. The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_LO_R09_PARK_OMAP_3YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Lo/R09/Park/Omap/3yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 15
releases of IBEX-HI and/or IBEX-LO data covering 2008-2017. 
2: This data set is from the Park et al. (2015) subset of Release 9 for IBEX-Lo
Heavy Neutral Maps data for combination and averaging of six-month maps 1-6 into
three-year maps for each energy channel during 2008-2011 in the form of counting
rates and supporting parameters. 
3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles from the measured direct events identified as 'Oxygen',
which are registered between 50 ns and 100 ns in TOF2; i.e. 50ns<=TOF2<=100ns
(Park et al. 2015). Because there are no sputtering, corrections, the
'Oxygen'.events may include O, Ne, and other heavier elements. The single O maps
are produced by Pipeline code. There are energy bands 5-8 in numerical data
form. Energy channels 5-8 have FWHM center-point energies at 0.209, 0.439,
0.872, 1.821 keV, respectively. Details of the data and enabled science from
this part ofRelease 9 are given in the following journal publication:
4: J. Park et al., Statistical Analysis of the Heavy Neutral Atoms Measured by
IBEX. The Astrophysical Journal Supplement Series, 220:34 (13pp), 2015 October.
http://dx.doi.org/10.1088/0067-0049/220/2/34 
5. The following list associates Release 9 map numbers (1-6) with mission year
(1-3), orbits (11-150a), and dates (12/25/2008-12/24/2011): 
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
6: The energy resolution is delta-E/E = 0.8 for all channels:
Energy channel 1: center energy = 0.015 keV
Energy channel 2: center energy = 0.029 keV
Energy channel 3: center energy = 0.055 keV
Energy channel 4: center energy = 0.11 keV
Energy channel 5: center energy = 0.209 keV
Energy channel 6: center energy = 0.439 keV
Energy channel 7: center energy = 0.872 keV
Energy channel 8: center energy = 1.821 keV
7: This particular data set, denoted in the original ascii files as comb-ot-m1m6
includes combined IBEX-Lo heavy neutral pixel maps data (map1 + map2 + map3 +
map4 + map5 + map6) from all directions 
Modification History
The Release 9 data contains Maps 1 - 6. The present CDF data set was converted
from the originally archived data in ascii list format but otherwise includes no
changes in the data. The original data are given in 30 rows for Solar Ecliptic
Latitude and 60 columns for Solar Ecliptic East Longitude. The accompanying
documentation described the row latitude data as starting from the north
Ecliptic pole (+90 degrees) and decreasing in value to the south Ecliptic pole
(-90 degrees). During preparation of the data set in CDF format, SPDF discovered
that the correct order was increasing from row 1 for the South Ecliptic pole to
row 30 for the north Ecliptic pole. East longitude is defined correctly for the
column order but we have instead used west longitude to better represent the
outward-looking viewpoint from IBEX to the outer heliosphere as typically used
in IBEX team plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_LO_R09_PARK_OMAP_3YR-EVEN-MAPS (spase://VSPO/NumericalData/IBEX/H3/ENA/Lo/R09/Park/Omap/3yreven)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 15
releases of IBEX-HI and/or IBEX-LO data covering 2008-2017. 
2: This data set is from the Park et al. (2015) subset of Release 9 for IBEX-Lo
Heavy Neutral Maps (6 months-cadence) data from combined even maps (2,4,6)
during 2009-2011 in the form of counting rates and supporting parameters. 
3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles from the measured direct events identified as 'Oxygen',
which are registered between 50 ns and 100 ns in TOF2; i.e. 50ns<=TOF2<=100ns
(Park et al. 2015). Because there are no sputtering, corrections, the
'Oxygen'.events may include O, Ne, and other heavier elements. The single O maps
are produced by Pipeline code. There are energy bands 5-8 in numerical data
form. Energy channels 5-8 have FWHM center-point energies at 0.209, 0.439,
0.872, 1.821 keV, respectively. Details of the data and enabled science from
this part ofRelease 9 are given in the following journal publication:
4: J. Park et al., Statistical Analysis of the Heavy Neutral Atoms Measured by
IBEX. The Astrophysical Journal Supplement Series, 220:34 (13pp), 2015 October.
http://dx.doi.org/10.1088/0067-0049/220/2/34 
4. The following list associates Release 9 map numbers (1-6) with mission year
(1-3), orbits (11-150a), and dates (12/25/2008-12/24/2011): 
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
5: The energy resolution is delta-E/E = 0.8 for all channels:
Energy channel 1: center energy = 0.015 keV
Energy channel 2: center energy = 0.029 keV
Energy channel 3: center energy = 0.055 keV
Energy channel 4: center energy = 0.11 keV
Energy channel 5: center energy = 0.209 keV
Energy channel 6: center energy = 0.439 keV
Energy channel 7: center energy = 0.872 keV
Energy channel 8: center energy = 1.821 keV
6: This particular data set, denoted in the original ascii files as
comb-ot-m2m4m6 includes combined IBEX-Lo heavy neutral pixel even maps data
(map2 + map4 + map6) from all directions 
Modification History
The Release 9 data contains Maps 1 - 6. The present CDF data set was converted
from the originally archived data in ascii list format but otherwise includes no
changes in the data. The original data are given in 30 rows for Solar Ecliptic
Latitude and 60 columns for Solar Ecliptic East Longitude. The accompanying
documentation described the row latitude data as starting from the north
Ecliptic pole (+90 degrees) and decreasing in value to the south Ecliptic pole
(-90 degrees). During preparation of the data set in CDF format, SPDF discovered
that the correct order was increasing from row 1 for the South Ecliptic pole to
row 30 for the north Ecliptic pole. East longitude is defined correctly for the
column order but we have instead used west longitude to better represent the
outward-looking viewpoint from IBEX to the outer heliosphere as typically used
in IBEX team plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_LO_R09_PARK_OMAP_3YR-ODD-MAPS (spase://VSPO/NumericalData/IBEX/H3/ENA/Lo/R09/Park/Omap /3yrodd)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 15
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Park et al. (2015) subset of Release 9 for IBEX-Lo
Heavy Neutral Maps (6 months-cadence) data from combined odd maps (1,3,5) during
2008-2011 in the form of counting rates and supporting parameters. 
3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles from the measured direct events identified as 'Oxygen',
which are registered between 50 ns and 100 ns in TOF2; i.e. 50ns<=TOF2<=100ns
(Park et al. 2015). Because there are no sputtering, corrections, the
'Oxygen'.events may include O, Ne, and other heavier elements. The single O maps
are produced by Pipeline code. There are energy bands 5-8 in numerical data
form. Energy channels 5-8 have FWHM center-point energies at 0.209, 0.439,
0.872, 1.821 keV, respectively. Details of the data and enabled science from
this part ofRelease 9 are given in the following journal publication:
4: J. Park et al., Statistical Analysis of the Heavy Neutral Atoms Measured by
IBEX. The Astrophysical Journal Supplement Series, 220:34 (13pp), 2015 October.
http://dx.doi.org/10.1088/0067-0049/220/2/34 
5. The following list associates Release 9 map numbers (1-6) with mission year
(1-3), orbits (11-150a), and dates (12/25/2008-12/24/2011): 
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
6: The energy resolution is delta-E/E = 0.8 for all channels:
Energy channel 1: center energy = 0.015 keV
Energy channel 2: center energy = 0.029 keV
Energy channel 3: center energy = 0.055 keV
Energy channel 4: center energy = 0.11 keV
Energy channel 5: center energy = 0.209 keV
Energy channel 6: center energy = 0.439 keV
Energy channel 7: center energy = 0.872 keV
Energy channel 8: center energy = 1.821 keV
7: This particular data set, denoted in the original ascii files as
comb-ot-m1m3m5 includes combined IBEX-Lo heavy neutral pixel odd maps data (map1
+ map3 + map5) from all directions 
Modification History
The Release 9 data contains Maps 1 - 6. The present CDF data set was converted
from the originally archived data in ascii list format but otherwise includes no
changes in the data. The original data are given in 30 rows for Solar Ecliptic
Latitude and 60 columns for Solar Ecliptic East Longitude. The accompanying
documentation described the row latitude data as starting from the north
Ecliptic pole (+90 degrees) and decreasing in value to the south Ecliptic pole
(-90 degrees). During preparation of the data set in CDF format, SPDF discovered
that the correct order was increasing from row 1 for the South Ecliptic pole to
row 30 for the north Ecliptic pole. East longitude is defined correctly for the
column order but we have instead used west longitude to better represent the
outward-looking viewpoint from IBEX to the outer heliosphere as typically used
in IBEX team plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_LO_R09_PARK_OMAP_6MO (spase://VSPO/NumericalData/IBEX/H3/ENA/Lo/R09/Park/OMap/6mo)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 15
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Park et al. (2015) subset of the Release 9 The
IBEX-Lo Heavy Neutral Maps (6 months-cadence) data in the form of direct event
counts, counting rates and other supporting data
3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles from the measured direct events identified as 'Oxygen',
which are registered between 50 ns and 100 ns in TOF2; i.e. 50ns<=TOF2<=100ns
(Park et al. 2015). Because there are no sputtering corrections, the
'Oxygen'.events may include O, Ne, and other heavier elements. The single O maps
are produced by Pipeline code. There are energy bands 5-8 in numerical data
form. Energy channels 5-8 have FWHM center-point energies at 0.209, 0.439,
0.872, 1.821 keV, respectively. Details of the data and enabled science from
Release 9 are given in the following journal publication: 
4: J. Park et al., Statistical Analysis of the Heavy Neutral Atoms Measured by
IBEX. The Astrophysical Journal Supplement Series, 220:34 (13pp), 2015 October.
http://dx.doi.org/10.1088/0067-0049/220/2/34 
5. The following list associates Release 9 map numbers (1-6) with mission year
(1-3), orbits (11-150a), and dates (12/25/2008-12/24/2011): 
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
8: The energy resolution is delta-E/E = 0.8 for all channels:
Energy channel 1: center energy = 0.015 keV
Energy channel 2: center energy = 0.029 keV
Energy channel 3: center energy = 0.055 keV
Energy channel 4: center energy = 0.11 keV
Energy channel 5: center energy = 0.209 keV
Energy channel 6: center energy = 0.439 keV
Energy channel 7: center energy = 0.872 keV
Energy channel 8: center energy = 1.821 keV
6: This particular data set, denoted in the original ascii files as lvset_o_mapN
for N=1,6, includes pixel map data from all directions at 6 month cadence. 
Modification History
The Release 9 data contains Maps 1 - 6. The present CDF data set was converted
from the originally archived data in ascii list format but otherwise includes no
changes in the data. The original data are given in 30 rows for Solar Ecliptic
Latitude and 60 columns for Solar Ecliptic East Longitude. The accompanying
documentation described the row latitude data as starting from the north
Ecliptic pole (+90 degrees) and decreasing in value to the south Ecliptic pole
(-90 degrees). During preparation of the data set in CDF format, SPDF discovered
that the correct order was increasing from row 1 for the South Ecliptic pole to
row 30 for the north Ecliptic pole. East longitude is defined correctly for the
column order but we have instead used west longitude to better represent the
outward-looking viewpoint from IBEX to the outer heliosphere as typically used
in IBEX team plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_LO_R09_PARK_OMAP_STAT_3YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Lo/R09/Park/Omap/stat/3yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 15
releases of IBEX-HI and/or IBEX-LO data covering 2008-2017. 
This data set is from the Park et al. (2015) subset of Release 9 for IBEX-Lo
Heavy Neutral Maps, mostly of oxygen, averaged over three years, 2008-2011, from
combination of IBEX-Lo maps 1 to 6. There are four types of maps derived from
different statistical filtering approaches: signal/noise filtering, confidence
limit method (CLM), cluster analysis method (CLM), and CLUSTER with signal/noise
filtering, all as described in Park et al. (2015). Map data for the first two
approaches are in counts/second and for the last two in counts/hour (Cluster
ID).
3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles from the measured direct events identified as 'Oxygen',
which are registered between 50 ns and 100 ns in TOF2; i.e. 50ns<=TOF2<=100ns
(Park et al. 2015). Because there are no sputtering, corrections, the
'Oxygen'.events may include O, Ne, and other heavier elements. The single O maps
are produced by Pipeline code. There are energy bands 5-8 in numerical data
form. Energy channels 5-8 have FWHM center-point energies at 0.209, 0.439,
0.872, 1.821 keV, respectively. Details of the data and enabled science from
this part of Release 9 are given in the following journal publication:
4: J. Park et al., Statistical Analysis of the Heavy Neutral Atoms Measured by
IBEX. The Astrophysical Journal Supplement Series, 220:34 (13pp), 2015 October.
http://dx.doi.org/10.1088/0067-0049/220/2/34 
5. The following list associates Release 9 map numbers (1-6) with mission year
(1-3), orbits (11-150a), and dates (12/25/2008-12/24/2011): 
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
6: The energy resolution is delta-E/E = 0.8 for all channels:
Energy channel 1: center energy = 0.015 keV
Energy channel 2: center energy = 0.029 keV
Energy channel 3: center energy = 0.055 keV
Energy channel 4: center energy = 0.11 keV
Energy channel 5: center energy = 0.209 keV
Energy channel 6: center energy = 0.439 keV
Energy channel 7: center energy = 0.872 keV
Energy channel 8: center energy = 1.821 keV
7: This particular data set, denoted in the original ascii files as comb-ot-m1m6
includes combined IBEX-Lo heavy neutral pixel maps data (map1 + map2 + map3 +
map4 + map5 + map6)  for counting rates from all directions 
Modification History
The Release 9 data contains Maps 1 - 6. The present CDF data set was converted
from the originally archived data in ascii list format but otherwise includes no
changes in the data. The original data are given in 30 rows for Solar Ecliptic
Latitude and 60 columns for Solar Ecliptic East Longitude. The accompanying
documentation described the row latitude data as starting from the north
Ecliptic pole (+90 degrees) and decreasing in value to the south Ecliptic pole
(-90 degrees). During preparation of the data set in CDF format, SPDF discovered
that the correct order was increasing from row 1 for the South Ecliptic pole to
row 30 for the north Ecliptic pole. East longitude is defined correctly for the
column order but we have instead used west longitude to better represent the
outward-looking viewpoint from IBEX to the outer heliosphere as typically used
in IBEX team plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_LO_R10_NOCG_NOSP_OMNI_6MO (spase://VSPO/NumericalData/IBEX/H3/ENA/Lo/R10/noCG/noSP/Omni/6mo)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 15
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 (6 months-cadence) IBEX-Lo map data for
the first seven years, 2009-2015, in the form of omnidirectional fluxes without
any corrections (nocg) for spacecraft motion (Compton-Getting) and ENA survival
probability (nosp) between 1 and 100 AU.
3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 5-8 in
numerical data form. Energy channels 5-8 have FWHM center-point energies at
0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled
science from Release 10 are given in the following journal publication:
4: S.A. Fuselier et al., The IBEX-Lo Sensor. Space Sci Rev (2009) 146:
117...147; DOI 10.1007/s11214-009-9495-8
5: https://link.springer.com/article/10.1007/s11214-009-9495-8 
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015): 
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: The energy resolution is delta-E/E = 0.8 for all channels:
Energy channel 1: center energy = 0.015 keV
Energy channel 2: center energy = 0.029 keV
Energy channel 3: center energy = 0.055 keV
Energy channel 4: center energy = 0.11 keV
Energy channel 5: center energy = 0.209 keV
Energy channel 6: center energy = 0.439 keV
Energy channel 7: center energy = 0.872 keV
Energy channel 8: center energy = 1.821 keV
9: This particular data set, denoted in the original ascii files as lvset_h_mapN
for N=1,14, includes pixel map data from all directions (omnidirectional), no
CG, no SP, 6 month cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_LO_R10_NOCG_NOSP_OMNI_7YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Lo/R10/noCG/noSP/Omni/7yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 15
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 (7-year-average of 6-month-cadence maps)
IBEX-Lo map data for the first seven years, 2009-2015, in the form of
omnidirectional fluxes without any corrections for spacecraft motion (nocg)
(Compton-Getting) and with no applied ENA survival probability correction (nosp)
between 1 and 100 AU.
3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 5-8 in
numerical data form. Energy channels 5-8 have FWHM center-point energies at
0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled
science from Release 10 are given in the following journal publication:
4: S.A. Fuselier et al., The IBEX-Lo Sensor. Space Sci Rev (2009) 146:
117...147; DOI 10.1007/s11214-009-9495-8
5: https://link.springer.com/article/10.1007/s11214-009-9495-8 
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015): 
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: The energy resolution is delta-E/E = 0.8 for all channels:
Energy channel 1: center energy = 0.015 keV
Energy channel 2: center energy = 0.029 keV
Energy channel 3: center energy = 0.055 keV
Energy channel 4: center energy = 0.11 keV
Energy channel 5: center energy = 0.209 keV
Energy channel 6: center energy = 0.439 keV
Energy channel 7: center energy = 0.872 keV
Energy channel 8: center energy = 1.821 keV
9: This particular data set, denoted in the original ascii files as
lvset_h_single, includes pixel map data from all directions (omnidirectional),
no CG, SP, 7 year cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_LO_R10_NOCG_SP_OMNI_6MO (spase://VSPO/NumericalData/IBEX/H3/ENA/Lo/R10/noCG/SP/Omni/6mo)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 15
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 (6 months-cadence) IBEX-Lo map data for
the first seven years, 2009-2015, in the form of omnidirectional fluxes without
any corrections for spacecraft motion (nocg) (Compton-Getting) but with the
applied ENA survival probability correction (sp) between 1 and 100 AU.
3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 5-8 in
numerical data form. Energy channels 5-8 have FWHM center-point energies at
0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled
science from Release 10 are given in the following journal publication:
4: S.A. Fuselier et al., The IBEX-Lo Sensor. Space Sci Rev (2009) 146:
117...147; DOI 10.1007/s11214-009-9495-8
5: https://link.springer.com/article/10.1007/s11214-009-9495-8 
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015): 
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: The energy resolution is delta-E/E = 0.8 for all channels:
Energy channel 1: center energy = 0.015 keV
Energy channel 2: center energy = 0.029 keV
Energy channel 3: center energy = 0.055 keV
Energy channel 4: center energy = 0.11 keV
Energy channel 5: center energy = 0.209 keV
Energy channel 6: center energy = 0.439 keV
Energy channel 7: center energy = 0.872 keV
Energy channel 8: center energy = 1.821 keV
9: This particular data set, denoted in the original ascii files as
lvset_h_tabular_mapN for N=1,14, includes pixel map data from all directions
(omnidirectional), no CG, SP, 6 month cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IBEX_H3_ENA_LO_R10_NOCG_SP_OMNI_7YR (spase://VSPO/NumericalData/IBEX/H3/ENA/Lo/R10/noCG/SP/Omni/7yr)
Description
1: The Interstellar Boundary Explorer (IBEX) has operated in space since 2008
updating our knowledge of the outer heliosphere and its interaction with the
local interstellar medium. Start-time: 2008-12-25. There are currently 15
releases of IBEX-HI and/or IBEX-LO data covering 2009-2017. 
2: This data set is from the Release 10 (7-year-average of 6-month-cadence maps)
IBEX-Lo map data for the first seven years, 2009-2015, in the form of
omnidirectional fluxes without any corrections for spacecraft motion (nocg)
(Compton-Getting) but with the applied ENA survival probability correction (sp)
between 1 and 100 AU.
3: The data consist of all-sky maps in Solar Ecliptic Longitude (east and west)
and Latitude angles for ENA (hydrogen) fluxes from IBEX-Lo energy bands 5-8 in
numerical data form. Energy channels 5-8 have FWHM center-point energies at
0.209, 0.439, 0.872, 1.821 keV, respectively. Details of the data and enabled
science from Release 10 are given in the following journal publication:
4: S.A. Fuselier et al., The IBEX-Lo Sensor. Space Sci Rev (2009) 146:
117...147; DOI 10.1007/s11214-009-9495-8
5: https://link.springer.com/article/10.1007/s11214-009-9495-8 
6. The following codes are used to define dataset types:
cg = Compton-Getting corrections have been applied to the data to account for
the speed of the spacecraft relative to the direction of arrival of the ENAs. 
nocg = no Compton-Getting corrections 
sp = survival probability corrections have been applied to the data to account
for the loss of ENAs due to radiation pressure, photoionization and ionization
via charge exchange with solar wind protons as they stream through the
heliosphere. This correction scales the data out from IBEX at 1 AU to ~100 AU.
In the original data this mode is denoted as Tabular. 
noSP - no survival probability corrections have been applied to the data. 
omni = data from all directions. 
ram = data was collected when the spacecraft was ramming into the incoming ENAs.
antiram = data was collected when the spacecraft was moving away from the
incoming ENAs. 
7. The following list associates Release 10 map numbers (1-14) with mission year
(1-7), orbits (11-310b), and dates (12/25/2008-12/23/2015): 
Map 1: year 1, orbits 11-34, dates 12/25/2008-06/25/2009
Map 2: year 1, orbits 35-58, dates 06/25/2009-12/25/2009
Map 3: year 2, orbits 59-82, dates 12/25/2009-06/26/2010
Map 4: year 2, orbits 83-106, dates 06/26/2010-12/26/2010
Map 5: year 3, orbits 107-130a, dates 12/26/2010-06/25/2011
Map 6: year 3, orbits 130b-150a, dates 06/25/2011-12/24/2011
Map 7: year 4, orbits 150b-170a, dates 12/24/2011-06/22/2012
Map 8: year 4, orbits 170b-190b, dates 06/22/2012-12/26/2012
Map 9: year 5, orbits 191a-210b, dates 12/26/2012-06/26/2013
Map 10: year 5, orbits 211a-230b, dates 06/26/2013-12/26/2013
Map 11: year 6, orbits 231a-250b, dates 12/26/2013-06/26/2014
Map 12: year 6, orbits 251a-270b, dates 06/26/2014-12/24/2014
Map 13: year 7, orbits 271a-290b, dates 12/24/2014-06/24/2015
Map 14: year 7, orbits 291a-310b, dates 06/24/2015-12/23/2015
8: The energy resolution is delta-E/E = 0.8 for all channels:
Energy channel 1: center energy = 0.015 keV
Energy channel 2: center energy = 0.029 keV
Energy channel 3: center energy = 0.055 keV
Energy channel 4: center energy = 0.11 keV
Energy channel 5: center energy = 0.209 keV
Energy channel 6: center energy = 0.439 keV
Energy channel 7: center energy = 0.872 keV
Energy channel 8: center energy = 1.821 keV
9: This particular data set, denoted in the original ascii files as
lvset_h_tabular_single, includes pixel map data from all directions
(omnidirectional), no CG, SP, 7 year cadence. 
Modification History
The Release 10 data extend through Map 14 and contain modications and updates of
Maps 1-2 from Release 2, Maps 1-6 from Release 4, and Maps 1-10 from Release 7.
The present CDF data set was converted from the originally archived data in
ascii list format but otherwise includes no changes in the data. The original
data are given in 30 rows for Solar Ecliptic Latitude and 60 columns for Solar
Ecliptic East Longitude. The accompanying documentation described the row
latitude data as starting from the north Ecliptic pole (+90 degrees) and
decreasing in value to the south Ecliptic pole (-90 degrees). During preparation
of the data set in CDF format, SPDF discovered that the correct order was
increasing from row 1 for the South Ecliptic pole to row 30 for the north
Ecliptic pole. East longitude is defined correctly for the column order but we
have instead used west longitude to better represent the outward-looking
viewpoint from IBEX to the outer heliosphere as typically used in IBEX team
plots. 
 
Dataset in CDAWeb
Back to top
IG_K0_PCI (spase://VSPO/NumericalData/Interball/PC_Index/KeyParameter/K0/PT5M)
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 May 1996
 
Dataset in CDAWeb
Back to top
IMAGE_M2_EUV
Description
Katus, R. M., D. L. Gallagher, M. W. Liemohn,A. M. Keesee, and L. K. Sarno?Smith
(2015), Statistical storm time examination of MLT dependent plasmapause location
derived from IMAGE EUV,J. Geophys. Res. Space Physics, 120, 5545?5559,
doi:10.1002/2015JA021225.
 
Dataset in CDAWeb
Back to top
IM_ELECTRON_DENSITY_RPI (spase://VSPO/NumericalData/IMAGE/RPI/PT1M)
Description
The electron density values listed in this file are derived from the IMAGE Radio
Plasma Imager (B.W. Reinisch, PI) data using an automatic fitting program
written by Phillip Webb with manual correction.
The electron number densities were produced using an automated procedure (with
manual correction when necessary) which attempted to self-consistently fit an
enhancement in the IMAGE RPI Dynamic Spectra to either 1) the Upper Hybrid
Resonance band, 2) the Z-mode or 3) the continuum edge. The automatic algorithm
works by rules determined by comparison of the active and passive RPI data
[Benson et al., GRL, vol. 31, L20803, doi:10.1029/2004GL020847, 2004].
The manual data points are not from frequencies chosen freely by a human. Rather
the human specifies that the computer should search for a peak or continuum edge
in a certain frequency region. Thus even the manual points are determined, in
part, by the automatic algorithms. Of course that does not guarantee that the
data points are right, but it does eliminate some human bias.
 
Dataset in CDAWeb
Back to top
IM_HK_ADS (spase://VSPO/NumericalData/IMAGE/HK/CDAWeb/PT24H)
Description
tbs
Modification History
tbs
 
Dataset in CDAWeb
Back to top
IM_HK_AST (spase://VSPO/NumericalData/IMAGE/HK/CDAWeb/PT24H)
Description
tbs
Modification History
tbs
 
Dataset in CDAWeb
Back to top
IM_HK_COM (spase://VSPO/NumericalData/IMAGE/HK/CDAWeb/PT24H)
Description
tbs
Modification History
tbs
 
Dataset in CDAWeb
Back to top
IM_HK_FSW (spase://VSPO/NumericalData/IMAGE/HK/CDAWeb/PT24H)
Description
tbs
Modification History
tbs
 
Dataset in CDAWeb
Back to top
IM_HK_PWR (spase://VSPO/NumericalData/IMAGE/HK/CDAWeb/PT24H)
Description
tbs
Modification History
tbs
 
Dataset in CDAWeb
Back to top
IM_HK_TML (spase://VSPO/NumericalData/IMAGE/HK/CDAWeb/PT24H)
Description
tbs
Modification History
tbs
 
Dataset in CDAWeb
Back to top
IM_K0_EUV (spase://VSPO/DisplayData/IMAGE/EUV/PT600S)
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
 
Dataset in CDAWeb
Back to top
IM_K0_HENA (spase://VSPO/DisplayData/IMAGE/HENA/124S)
Description
No TEXT global attribute value.
 
Dataset in CDAWeb
Back to top
IM_K0_LENA (spase://VSPO/DisplayData/IMAGE/LENA/PT124S)
Description
No TEXT global attribute value.
 
Dataset in CDAWeb
Back to top
IM_K0_MENA (spase://VSPO/DisplayData/IMAGE/MENA/PT124S)
Description
No TEXT global attribute value.
 
Dataset in CDAWeb
Back to top
IM_K0_RPI (spase://VSPO/NumericalData/IMAGE/RPI/PT24H)
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_k0_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;
 
Dataset in CDAWeb
Back to top
IM_K0_SIE (spase://VSPO/DisplayData/IMAGE/FUV/SIE/PT124S)
Description
electrons
SKT version 24-July-2000 
Mende et al: Far Ultraviolet Imaging from the IMAGE Spacecraft,Space Sciences
Review 1999  
 
Dataset in CDAWeb
Back to top
IM_K0_SIP (spase://VSPO/DisplayData/IMAGE/FUV/SIP/PT124S)
Description
Protons
SKT version 24-July-2000
Mende et al: Far Ultraviolet Imaging from the IMAGE Spacecraft,Space Sciences
Review 1999  
 
Dataset in CDAWeb
Back to top
IM_K0_WIC (spase://VSPO/DisplayData/IMAGE/FUV/WIC/PT124S)
Description
No TEXT global attribute value.
 
Dataset in CDAWeb
Back to top
IM_K1_RPI (spase://VSPO/NumericalData/IMAGE/RPI/DS/PT5M)
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_k1_rpi_00000000_v01
 
Dataset in CDAWeb
Back to top
IM_OR_DEF (spase://VSPO/NumericalData/IMAGE/Orbit/Definitive/PT120S)
Description
tbs
Modification History
tbs
 
Dataset in CDAWeb
Back to top
IM_OR_GIFWALK
Description
Pre-generated PWG plots
 
Dataset in CDAWeb
Back to top
IM_OR_PRE (spase://VSPO/NumericalData/IMAGE/Orbit/Predict/PT120S)
Description
tbs
Modification History
tbs
 
Dataset in CDAWeb
Back to top
ISEE-3_HELIO1DAY_POSITION
Description
No TEXT global attribute value.
 
Dataset in CDAWeb
Back to top
ISEE-3_MAGPLASMA_2MIN_MAGNETIC_FIELD_PLASMA (spase://VSPO/NumericalData/ISEE3/Merged/MAG_SWP/CDF/PT2M)
Description
These files provides access to a field/plasma-merged 2-min ISEE3 data setcreated
at NSSDC as part of preparing ISEE3 data for new OMNI. Input to the data set
were 1-min MAG magnetic field data, 24-splasma data, and daily spacecraft
position data, all obtained from
theftp://spdf.gsfc.nasa.gov/pub/data/isee/isee3/ from which needed documentation
may be found. The annual files of this ASCII data set may be accessed at FTP
siteftp://spdf.gsfc.nasa.gov/pub/data/isee/isee3/2_min_merged_mag_plasma/as
well.
Time span: Mag field: 1978-09-11 - 1982-10-12           Plasma: 1978-09-11 -
1980-02-19
Note that Magntic Field is given in SE- Spacecraft-centered Solar-Ecliptic
coordinate system. 
 
Dataset in CDAWeb
Back to top
ISEE-3_MAG_1MIN_MAGNETIC_FIELD (spase://VSPO/NumericalData/ISEE3/MAG/CDF/PT1M)
Description
This data set contains averaged 1-minute magnetic field data converted from
simple ASCII records. It was created at NSSDC from a more complex,
multi-resolution data set (NSSDC ID = SPHE-00673; Old ID = 78-079A-02D) provided
by the Principal Investigator team and now available
fromftp://nssdcftp.gsfc.nasa.gov/spacecraft_data/isee/isee3/magnetic_fields/1min
_ascii/
The coordinate system for the B-field components is the JPL-defined I,S
coordinate system (origin at the spacecraft): I is the unit vector in the
direction of the ISEE-3 spin axis (positive in the northward direction), and S
is the unit vector from the spacecraft to the sun. The z-axis is parallel to to
I, the y-axis to the cross-product I x S, and the x-axis to Y x Z. The I,S
coordinate system is approximately the same as the Solar Ecliptic (SE) system
since the spacecraft z-axis (the spin axis) is maintained within 0.5 degree of
perpendicular to the ecliptic plane. (SE is defined the same way as GSE, but
with the spacecraft [point of observation] substituted for Earth).  
For years 1984-1990 we added spacecraft position in HGI coordinate
The HGI coordinates are Sun-centered and inertially fixed with respect to an 
X-axis directed along the intersection line of theecliptic and solar equatorial 
planes, and defines zero of the longitude, HGI_LONG. The solar equator plane  is
inclined at 7.25degrees from the ecliptic. This direction was towards ecliptic 
longitude of 74.367 deg on 1 January 1900 at 12:00 UT; because of the precession
of the Earth"s equator, this longitude increases by 1.4 deg/century.  The Z-axis
is directed perpendicular to and northward of the solar equator, and the Y-axis
completes the right-handed set.  The longitude, HGI_LONG increase from zero in
the X-direction towards Y-direction.The latitude HG_LAT increases to +90 deg
towards  the north pole, and to -90 deg towardsm south pole. 
Note that here present values averaged in 1-minute, e.g. <B>^2 may be not equal
<B^2)>.
 
Dataset in CDAWeb
Back to top
ISEE1_4SEC_MFI (spase://VSPO/NumericalData/ISEE1/MAG/PT4S)
Description
C. T. Russell (IEEE Trans. Geoscience Electronics, GE-16, 239-242, 1978). This
publication is available online at
http://www-ssc.igpp.ucla.edu/personnel/russell/papers/ISEE_fluxgate/.
 
Dataset in CDAWeb
Back to top
ISEE1_60SEC_MFI (spase://VSPO/NumericalData/ISEE1/MAG/PT1M)
Description
C. T. Russell (IEEE Trans. Geoscience Electronics, GE-16, 239-242, 1978). This
publication is available online at
http://www-ssc.igpp.ucla.edu/personnel/russell/papers/ISEE_fluxgate/.
 
Dataset in CDAWeb
Back to top
ISEE1_H0_FE (spase://VSPO/NumericalData/ISEE1/VES/PT18S)
Description
This enhanced CDF master was generated by NSSDC, with input from R. Fitzenreiter
and A. F.-Vinas, to make useable a bare-bones CDF data set provided earlier to
NSSDC. This current CDF master version, Oct. 5, 2007, is used for making a CDF
by selecting only certain variables from those available in the original
bare-bones CDF.
Modification History
Velocity units were changed to km/sec, and Hi, Mid, & Lowest energy 
channels above SC potential were change from velocity to the corresponding 
energy value in eV..
 
Dataset in CDAWeb
Back to top
ISEE1_H1_FPE (spase://VSPO/NumericalData/ISEE1/FPE/PT1M)
Description
These experimenter-supplied, fast plasma proton fluid parameter data were
originally written in BCD character code, but were converted to EBCDIC
characters during restoration to new media. Data coverage includes the region
from 6 earth radii out to (but excluding) the bow shock. The reasons for
selecting this area of coverage are that the solar wind ion distributions are
too cold to be adequately resolved by this instrument, and inside the region of
6 earth radii the fast plasma data would be contaminated by the energetic
particle background. The physical records on the tapes are blocked with 50
88-byte logical records. The first record of each file is a header containing
data identification information, orbit number, and start and end times for the
file. Each data record contains universal time (in year, day of year, and
seconds of day), orbit number, spacecraft position in solar ecliptic
coordinates, number density, energy density, a flag indicating the energy range
covered, components of the two-dimensional bulk velocity in spacecraft
coordinates, and the average two-dimensional temperature. Time resolution is 60
seconds, but the distributions were obtained over 3 or 6 seconds..Los Alamos
Magnetospheric Plasma Analyzer (MPA) [Bame et al., .Rev. Sci. Inst., in press
1993]. ...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 suspect because of unreliable
.location info. .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 suspect because of unreliable
.location info. .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 suspect because of unreliable
.location info. .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 suspect because of unreliable
.location info. 
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 suspect because of unreliable 
location info. 
Modification History
This is a revised version of the data; the PI team re-processed the data and
provided this replacement version in July 1986. The new version can be verified
by the wording in the header information, which contains "...FPE 2D IONS 85.
LANL/MPE,..." in the revised version....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 .New Dict keys added sep95
.Added new global attr. and variables from M.Kessel Oct 98.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
.New Dict keys added sep95 .Added new global attr. and variables from M.Kessel
Oct 98.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 .New Dict keys added sep95 .Added new global attr. and
variables from M.Kessel Oct 98.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 .New Dict keys added sep95 .Added
new global attr. and variables from M.Kessel Oct 98
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 
New Dict keys added sep95 
Added new global attr. and variables from M.Kessel Oct 98
 
Dataset in CDAWeb
Back to top
ISEE1_H2_FPE (spase://VSPO/NumericalData/ISEE1/FPE/PT24S)
Description
These data are high temporal resolution solar wind ion moments derived from
measurements obtained by the Los Alamos X-Fan Solar Wind Ion Experiment (SWE) on
ISEE-1. The original magnetic tape contained 7 files, 1 for each of the solar
wind seasons for the spacecraft (roughly July through December) from 1977
through 1983. The temporal resolution of these data is 24 seconds in high data
rate and 48 seconds in low data rate. Each data record in these files contains
the date (YYMMDD), universal time in seconds, universal time in HHMMSS, the
proton density (cm-3), flow speed (km/sec), flow azimuth (degs., with 0 degrees
corresponding to flow from the sun [corrected for aberration] and positive
azimuths corresponding to flow toward dawn), flow latitude (degs., with positive
latitudes corresponding to flow toward the south), the minimum proton
temperature (degrees K), the maximum proton temperature (degrees K), and the
alpha/proton fraction (alpha fraction = 0.00 means no determination made). The
data providers did not attempt to cross-calibrate density values with those from
other experiments. However, they expected that density values will tend to be
too low in later years because of detector degradation. Cross-calibration using,
for example, IMP-derived values would be a useful exercise. Please note also
that many of these measurements were obtained within the foreshock region where
the solar wind flow is affected by waves in the foreshock. 
Reference: Los
Alamos Magnetospheric Plasma Analyzer (MPA) [Bame et al., ISEE-1 and ISEE-2 fast
plasma experiment and the ISEE-1 solar wind experiment, IEEE Trans. Geosci.
Electron., GE-16, 216, 1978]. 
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 suspect
because of unreliable 
location info. 
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 suspect
because of unreliable 
location info. 
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 suspect because of unreliable 
location info. 
Modification History
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 
New Dict keys added sep95 
Added new global attr. and variables from M.Kessel Oct 98
 
Dataset in CDAWeb
Back to top
ISEE1_PWI_SA (spase://VSPO/NumericalData/ISEE1/PWE/SA/PT1S)
Description
'The ISEE-1 and -2 Plasma Wave Investigation' D. A. Gurnett, F. L. Scarf, R. W.
Fredricks, and E. J. Smith, IEEE Transactions on Geoscience Electronics, Vol.
GE-16, p. 225-230, 1978.
 
Dataset in CDAWeb
Back to top
ISEE1_PWI_SA-RAPID-E (spase://VSPO/NumericalData/ISEE1/PWE/SA/PT0.125S)
Description
'The ISEE-1 and -2 Plasma Wave Investigation' D. A. Gurnett, F. L. Scarf, R. W.
Fredricks, and E. J. Smith, IEEE Transactions on Geoscience Electronics, Vol.
GE-16, p. 225-230, 1978.
 
Dataset in CDAWeb
Back to top
ISEE1_PWI_SFR-E (spase://VSPO/NumericalData/ISEE1/PWE/SFR/PT32S)
Description
'The ISEE-1 and -2 Plasma Wave Investigation' D. A. Gurnett, F. L. Scarf, R. W.
Fredricks, and E. J. Smith, IEEE Transactions on Geoscience Electronics, Vol.
GE-16, p. 225-230, 1978.
 
Dataset in CDAWeb
Back to top
ISEE2_4SEC_MFI (spase://VSPO/NumericalData/ISEE2/MAG/PT4S)
Description
C. T. Russell (IEEE Trans. Geoscience Electronics, GE-16, 239-242, 1978). This
publication is available online at
http://www-ssc.igpp.ucla.edu/personnel/russell/papers/ISEE_fluxgate/.
 
Dataset in CDAWeb
Back to top
ISEE2_60SEC_MFI (spase://VSPO/NumericalData/ISEE2/MAG/PT1M)
Description
C. T. Russell (IEEE Trans. Geoscience Electronics, GE-16, 239-242, 1978). This
publication is available online at
http://www-ssc.igpp.ucla.edu/personnel/russell/papers/ISEE_fluxgate/.
 
Dataset in CDAWeb
Back to top
ISEE2_H1_FPE (spase://VSPO/NumericalData/ISEE2/FPE/PT1M)
Description
These experimenter-supplied, fast plasma proton fluid parameter data were
originally written in BCD character code, but were converted to EBCDIC
characters during restoration to new media. Data coverage includes the region
from 6 earth radii out to (but excluding) the bow shock. The reasons for
selecting this area of coverage are that the solar wind ion distributions are
too cold to be adequately resolved by this instrument, and inside the region of
6 earth radii the fast plasma data would be contaminated by the energetic
particle background. The physical records on the tapes are blocked with 50
88-byte logical records. The first record of each file is a header containing
data identification information, orbit number, and start and end times for the
file. Each data record contains universal time (in year, day of year, and
seconds of day), orbit number, spacecraft position in solar ecliptic
coordinates, number density, energy density, a flag indicating the energy range
covered, components of the two-dimensional bulk velocity in spacecraft
coordinates, and the average two-dimensional temperature. Time resolution is 60
seconds, but the distributions were obtained over 3 or 6 seconds..Los Alamos
Magnetospheric Plasma Analyzer (MPA) [Bame et al., .Rev. Sci. Inst., in press
1993]. ...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 suspect because of unreliable
.location info. .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 suspect because of unreliable
.location info. .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 suspect because of unreliable
.location info. .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 suspect because of unreliable
.location info. .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 suspect because of unreliable
.location info. 
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 suspect because of unreliable 
location info. 
Modification History
This is a revised version of the data; the PI team re-processed the data and
provided this replacement version in July 1986. The new version can be verified
by the wording in the header information, which contains "...FPE 2D IONS 85.
LANL/MPE,..." in the revised version....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 .New Dict keys added sep95
.Added new global attr. and variables from M.Kessel Oct 98.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
.New Dict keys added sep95 .Added new global attr. and variables from M.Kessel
Oct 98.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 .New Dict keys added sep95 .Added new global attr. and
variables from M.Kessel Oct 98.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 .New Dict keys added sep95 .Added
new global attr. and variables from M.Kessel Oct 98.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 .New Dict
keys added sep95 .Added new global attr. and variables from M.Kessel Oct 98
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 
New Dict keys added sep95 
Added new global attr. and variables from M.Kessel Oct 98
 
Dataset in CDAWeb
Back to top
ISS_27DAY-AVERAGES_AMS-02 (spase://VSPO/NumericalData/ISS/AMS-02/P27D)
Description
No TEXT global attribute value.
 
Dataset in CDAWeb
Back to top
ISS_DOSANL_TEPC (spase://VSPO/NumericalData/ISS/TEPC/PT10S)
Description
TEPC serrial number = 1003
TEPC Analysis SoftwareVersion Number = 3.1 
 
Dataset in CDAWeb
Back to top
ISS_SP_FPMU (spase://VSPO/NumericalData/ISS/FPMU/PT1S)
Description
ISS FPMU 1-sec Ionosphere Summary Wide Langmuir Probe (WLP) Density and Narrow
Langmuir Probe (NLP) Temperature Records
 
Dataset in CDAWeb
Back to top
IT_H0_MFI (spase://VSPO/NumericalData/Interball-1/MIFM/PT6S)
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/
 
Dataset in CDAWeb
Back to top
IT_K0_AKR (spase://VSPO/NumericalData/Interball-1/AKR2/KP/PT120S)
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
 
Dataset in CDAWeb
Back to top
IT_K0_COR (spase://VSPO/NumericalData/Interball-1/CORALL/PT120S)
Description
No TEXT global attribute value.
Modification History
created July 1996
 
Dataset in CDAWeb
Back to top
IT_K0_ELE (spase://VSPO/NumericalData/Interball-1/ELECTRON/PT120S)
Description
No TEXT global attribute value.
Modification History
created Mar 1996
 
Dataset in CDAWeb
Back to top
IT_K0_EPI (spase://VSPO/NumericalData/Interball-1/DOK2-SKA-2/PT2M)
Description
No TEXT global attribute value.
Modification History
created Mar 1996
 
Dataset in CDAWeb
Back to top
IT_K0_ICD (spase://VSPO/NumericalData/Interball-1/PROMICS3/PT120S)
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
 
Dataset in CDAWeb
Back to top
IT_K0_MFI (spase://VSPO/NumericalData/Interball-1/MIFM/PT120S)
Description
No TEXT global attribute value.
Modification History
created  Oct 2003
 
Dataset in CDAWeb
Back to top
IT_K0_VDP (spase://VSPO/NumericalData/Interball-1/VDP/PT2M)
Description
No TEXT global attribute value.
Modification History
created Feb 1997
 
Dataset in CDAWeb
Back to top
IT_K0_WAV (spase://VSPO/NumericalData/Interball-1/MIFM/PT2M)
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
 
Dataset in CDAWeb
Back to top
IT_OR_DEF (spase://VSPO/NumericalData/Interball-1/Ephemeris/PT2M)
Description
No TEXT global attribute value.
Modification History
created Jul 1998
 
Dataset in CDAWeb
Back to top
IT_OR_GIFWALK
Description
Pre-generated PWG plots
 
Dataset in CDAWeb
Back to top
NASA Logo - nasa.gov