File: ULYCOS_KETA_10M_FMT.txt Version: U. Kiel ------------------------------------------------------------------------ !!! This data set was reingested from launch as of 12/22/97. JFC !!! COSPIN-KET RECORD FORMAT (REFERENCE: A&A,92,2 page 384, table 10) LOCATION: ESTUDS::DKA500:[UDS.COSPIN.KET]UCOSKETA90296.DAT;1 For all electron channels we have to make PHA corrections. Such corrections are not possible on a ten minute average basis. The analysis described in Heber (PHD, 1997) shows that for the analysis of quiet time periods most of the KET proton and helium channels have also to be PHA corrected. Thus only rate files will be available on ten minute averages. Note: You can calculate proton and helium intensities during solar or interplanetary events using the geometrical factors given below. UDS REPRESENTATIVE: B. HEBER (bheber@kernphysik.uni-kiel.de) RECORD FORMAT: IMPLICIT REAL(K) DIMENSION K21_28(8),K13_20(8) C FIXED FORMAT READ(40,'(6I5)'),(IT(I),I=1,5),ICOV READ(40,'(10G11.3)') . K1,K21_28,P4 READ(40,'(10G11.3)') . K3,K34,K12,K10,K2,K33,K29,K31,K30,K13 READ(40,'(10G11.3)') . K14_20,E4,K11,K32 READ(40,'(6G11.3)') D10,D20,C10,C20,S20,A01 PARAMETER LIST: IYEAR: year IDOY: day of year IHOUR: hour IMIN: minute ISEC: second ICOV: data coverage in % K1: protons (2.7-5.4 MeV) K21_28: " (5.4-23.1 MeV) sectors 1 to 8 P4: " (5.4-23.1 MeV) K3: " (34.1-125.0 MeV) K34: " (125.0-320.0 MeV) K12: " (320.0-2100.0 Mev) K10: " (>2100.0 MeV) K2: helium (6.0-20.4 MeV) K33: " (34.2-125.0 MeV) K29: " (125.0-320.0 MeV) K31: " (320.0-2100.0 MeV) K30: " (>2100.0 MeV) K13_20: electrons (2.5-7.0 MeV) sectors 1 to 8 E4: electrons (2.5-7.0 MeV) K11: " (7.0-170.0 MeV) K32: " (>170.0 MeV) D10: single detector counts D1 (semiconductor detector) D20: single detector counts D2 ( " ) C10: single detector counts C1 (Cherenkov) C20: single detector counts C2 (Cherenkov) S20: single detector counts S2 (Scintilator) A01: single detector counts A (Anticoincidence) FLUX UNITS: (/s) TIME RESOLUTION: 10 minutes NOTES: KIEL ELECTRON TELESCOPE README 17.10.1994 ======================================================================== COSPIN-KET RECORD FORMAT (REFERENCE: A&A,92,2 page 384, table 10) TIME RESOLUTION: 10 minutes, for Jovian Encounter Period time resolution is varying, see Parameter COV and note 11. below. NOTES: flag of -707 if intensity can not be determined ============ IMPORTANT: ============ 1. Only rates are given, since no simple estimate of the intensities can be done. Intensities must derived from PulsHeight Analysis. 2. Background Fluxes of K1 are a combination of components, including a high RTG background rate. This channel should be used only during event times. 3. On 10 min averages some of the channels have limitations of RTG background. Time periods with lower fluxes are available from the PI. Very slowly increases are a sign that background levels are reached (few percent per year). ============================================================= DO NOT MAKE LONGER ACCUMULATION AVERAGES WITH THESE CHANNELS BY USING PERIODS WITH A LOT OF BACKGROUND DATA !!!!!!!!! ============================================================= 4. No correction of the counting rates in K3, K34 and K33 is made. If you are looking at low fluxes especially in K33, please ask for data on a longer accumulation period. =============================================================== GET LOW FLUX VALUES FROM THE PI ON LONGER ACCUMULATION PERIODS =============================================================== 5. Fluxes of K11, K13_K20 and E4 below 2.0e-4, 2.5e-3 are a combination of different components including RTG background. The exact amount of background relative to real electrons are unknown. =============================================================== Levels below 3.0e-3, 2.5e-3 should not be considered. =============================================================== 6. Fluxes of K32 are contaminated by high energy protons. Reliable fluxes needs an PHA correction on longer accumulation periods. 7. Changes in geometrical Factor G = (counting rate)/(Intensity) K3 70.0 K34 152.0 K12 3300.0 K33 70.0 K29 88.0 K31 3200.0 8. Determination of the intensities of K29 needs a PHA correction on longer accumulation periods (several hours). 9. Timeperiods when KET is not working nominally has been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter. 10. Data for the Jovian encounter are available on a 4 min bases. Only a 0. order dead time correction is given. Data when the photomultiplier are off are available from the PI. For this Time period the coverage gives the accumulation times. ================================================= Caution: Very high fluxes for KET !!!! HERE: ICOV == Accumulation time in seconds !!!!! =================================================