Data Set Information
DATA_SET_NAME ICE ENERGETIC PARTICLE ANISOTROPY SPECTROMETER DATA V1.0
DATA_SET_ID ICE-C-EPAS-3-RDR-GIACOBIN-ZIN-V1.0
NSSDC_DATA_SET_ID
DATA_SET_TERSE_DESCRIPTION
DATA_SET_DESCRIPTION 
Data Set Overview:  In this G-Z dataset, observations from channels E1 to E5 (table below) are included since cometary ions were not detected in the higher energy channels. For each of these channels, particle counts are accumulated in eight azimuthal sectors of 45 deg. width in each telescope. The sectors are numbered from 1 to 8 anticlockwise when viewed from above the ecliptic, with Sector 1 centered on the sun- Earth line, i.e. it views in the sunward direction and detects ions streaming away from the Sun. At Giacobini-Zinner, a complete 3- dimensional distribution function was obtained at 32 s intervals during the main encounter phase, changing to 64 s at greater distances e.g. after 1830 UT on 12 September outbound.  	(The water-group energy ranges for channels E6-E8 have not been determined.)   		 Protons	 Water Group (Noise) E0: 21-35	keV	 35-65	keV(approx.) 	 E1: 35-56	keV	 65-95	keV 	 E2: 56-91	keV	 95-140 keV 	 E3: 91-147 keV	140-205 keV 	 E4: 147-238 keV	205-310 keV 	 E5: 238-384 keV	310-480 keV 	 E6: 384-620 keV 	 E7: 620-1000 keV	(From Hynds et al., 	 E8: 1000-1600 keV	Science 232, 361, 1986)
DATA_SET_RELEASE_DATE 3000-01-01T00:00:00.000Z
START_TIME 1985-09-08T12:43:22.000Z
STOP_TIME 1985-09-14T08:40:01.000Z
MISSION_NAME INTERNATIONAL COMETARY EXPLORER
MISSION_START_DATE 1983-12-22T12:00:00.000Z
MISSION_STOP_DATE N/A (ongoing)
TARGET_NAME GIACOBINI-ZINNER
TARGET_TYPE COMET
INSTRUMENT_HOST_ID ICE
INSTRUMENT_NAME ENERGETIC PARTICLE ANISOTROPY SPECTROMETER
INSTRUMENT_ID EPAS
INSTRUMENT_TYPE SPECTROMETER
NODE_NAME Small Bodies
ARCHIVE_STATUS ARCHIVED
CONFIDENCE_LEVEL_NOTE 
Confience Level Overview :  N/A
CITATION_DESCRIPTION Hynds, R.J., ICE ENERGETIC PARTICLE ANISOTROPY SPECTROMETER DATA V1.0, ICE-C-EPAS-3-RDR-GIACOBIN-ZIN-V1.0, NASA Planetary Data System, 1995.
ABSTRACT_TEXT In this G-Z dataset, observations from channels E1 to E5 (table below) are included since cometary ions were not detected in the higher energy channels. For each of these channels, particle counts are accumulated in eight azimuthal sectors of 45 deg. width in each telescope. The sectors are numbered from 1 to 8 anticlockwise when viewed from above the ecliptic, with Sector 1 centered on the sun- Earth line, i.e. it views in the sunward direction and detects ions streaming away from the Sun. At Giacobini-Zinner, a complete 3- dimensional distribution function was obtained at 32 s intervals during the main encounter phase, changing to 64 s at greater distances e.g. after 1830 UT on 12 September outbound.
PRODUCER_FULL_NAME INTERNATIONAL HALLEY WATCH
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