OBJECT = DATA_SET DATA_SET_ID = "ICE-C-EPAS-3-RDR-GIACOBIN-ZIN-V1.0" OBJECT = DATA_SET_INFORMATION DATA_SET_NAME = "ICE ENERGETIC PARTICLE ANISOTROPY SPECTROMETE R DATA V1.0" DATA_SET_COLLECTION_MEMBER_FLG = Y START_TIME = 1985-09-08T00:43:22.000Z STOP_TIME = 1985-09-14T20:40:01.000Z DATA_SET_RELEASE_DATE = UNK PRODUCER_FULL_NAME = "INTERNATIONAL HALLEY WATCH" DETAILED_CATALOG_FLAG = N DATA_SET_DESC = " \v Data Set Overview ================= \v 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) " CONFIDENCE_LEVEL_NOTE = " \v Confience Level Overview ======================== \v N/A" END_OBJECT = DATA_SET_INFORMATION OBJECT = DATA_SET_TARGET TARGET_NAME = "GIACOBINI-ZINNER" END_OBJECT = DATA_SET_TARGET OBJECT = DATA_SET_HOST INSTRUMENT_HOST_ID = ICE INSTRUMENT_ID = EPAS END_OBJECT = DATA_SET_HOST OBJECT = DATA_SET_REFERENCE_INFORMATION REFERENCE_KEY_ID = "ESA-SP1066" END_OBJECT = DATA_SET_REFERENCE_INFORMATION END_OBJECT = DATA_SET END