Ulysses Cospin - Cosmic Ray and Solar Particle Investigation Bundle Ulysses Jupiter Encounter Cospin Kiel Electron Telescope (KET) Raw Data Description PSD3 DATA_SET_ID = ULY-J-COSPIN-KET-3-RDR-RAW-HIRES-V1.0 ORIGINAL DATA_SET_NAME = ULY JUP COSPIN KIEL ELE TEL HIRES RAW PARTICLE COUNT RATES START_TIME = 1992-01-24T23:59:49.000 STOP_TIME = 1992-02-17T23:58:16.000 PDS3 DATA_SET_RELEASE_DATE = 1998-05-01 PRODUCER_FULL_NAME = HORST KUNOW DATA DESCRIPTION ================ Data Overview ============= Electron rates and Alpha and proton intensities as described below. Data ==== COSPIN-KET RECORD FORMAT RECORD FORMAT for TYYDOY.TAB implicit real(k) character*40 time read(1,'(a24,31(1x,1pe9.2))') time,cov,k1, k21,k22,k23,k24,k25,k26,k27,k28, k3,k34,k12,k10,k2,k33,k29,k31,k30, k13,k14,k15,k16,k17,k18,k19,k20, k11,k32,a01,d10 PARAMETER LIST: TIME: spacecraft event time in the format yyyy-mm-ddThh:mm:ss.sssZ COV: accumulation time in seconds K1: protons (2.7-5.4 MeV) K[21-28]:protons (5.4-23.1 MeV) sectors 1 to 8 K3: protons (34.1-125.0 MeV) K34: protons (125.0-320.0 MeV) nominal, forward penetrating protons (125.0-250.0 MeV), backward penetrating protons (160.0-260.0 MeV) K12: protons (260.0-2200.0 MeV) nominal, forward penetrating protons (250.0-2200.0 MeV), backward penetrating protons (260.0-2200.0 MeV) K10: protons (>2100.0 MeV) nominal protons (>2200.0 MeV) K2: helium (6.0-20.4 MeV/n) K33: helium (34-125 MeV/n) K29: helium (125.0-320.0 MeV/n) nominal forward penetrating helium (125.0-155.0 MeV/n), backward penetrating helium (155.0-225.0 MeV/n) K31: helium (320.0-2100.0 MeV/n) nominal forward penetrating helium (250.0-2100.0 MeV/n), backward penetrating helium (250.0-2100.0 MeV/n) K30: helium (>2000.0 MeV) K[13-20]:electrons (2.5-7.0 MeV) sectors 1 to 8 K11: electrons (7.0-170.0 MeV) K32: electrons (>170.0 MeV) A01: counting rate of Anticoincidence D10: counting rate of D1 FLUX UNITS: (/cm^2/s/sr/MeV) RATE UNITS: (/s) valid for all electron channels TIME RESOLUTION: 10 minutes, for Jovian Encounter Period time resolution is varying, see Parameter COV and note 11. below. NOTES: Electron data are Rates not Intensities. RTG corrections included, except for electrons flag of -9.99e+10 if intensity can not be determined IMPORTANT: 1. Only rates are given for the electrons, since no simple estimate of the intensities can be done. Intensities must derived from Pulse-Height 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, during quiet times flux is mostly set to -9.99e+10. 3. On 10 min averages some of the channels have limitations because of RTG background subtraction on this short time scale. 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). Channel Intensity K[21-28]: 1.2e-4 P4: 1.0e-3 DO NOT MAKE LONGER ACCUMULATION AVERAGES WITH THESE CHANNELS BY USING PERIODS WITH A LOT OF FILL DATA (-9.99e+10) !!!!!!! 4. A first order 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 back- ground. 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. Additional Correction introduced for K3, K34, K33, K31 9. Determination of the intensities of K29 needs a PHA correction on longer accumulation periods (several hours). 10. Time periods when KET is not working nominally have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter. 11. 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: COV == Accumulation time in seconds !!!!! References: ======== Ferrando, P., R. Ducros, C. Rastoin, A. Raviart, C. Raymond, H. Kunow, R. Mueller-Mellin, M. Sierks, and G. Wibberenz, Observations of Jovian Electrons by the Ulysses Electron Telescope, Proc. 22nd Int. Cosmic Ray Conf. (Dublin), 3, 366, 1991. Ferrando, P., R. Ducros, C. Rastoin, and A. Raviart, Jovian Electron Jets in Interplanetary Space, Planet. Space Sci, 41(11/12), 839, 1993. (https://doi.org/10.1016/0032-0633(93)90091-F) Ferrando, P., R. Ducros, C. Rastoin, A. Raviart, H. Kunow, R. Mueller-Mellin, H. Sierks, and G. Wibberenz, Propagation of Jovian Electrons In and Out or the Ecliptic, Adv. Space Res., 13(6), 107, 1993. Heber, B., A. Raviart, W. Droege, R. Ducros, P. Ferrando, H. Kunow, R. Mueller-Mellin, C. Rastoin, C. Roehrs, H. Sierks, and G. Wibberenz, High Energy Cosmic Ray Nuclei Results on Ulysses: 1. Mission Overview, Space Sci. Rev., 72 (1/2), 391, 1995. Kunow, H., R. Mueller-Mellin, H. Sierks, G. Wibberenz, A. Raviart, R. Ducros, P. Ferrando, and L. Treguer, The Kiel Electron Telescope On Board Ulysses, Proc. 22nd Int. Cosmic Ray Conf. (Dublin), 2, 503, 1991. Rastoin, C., R. Ducros, P. Ferrando, and A. Raviart, The 10-hour Modulation of the Jovian Electron Spectrum in Interplanetary Space - Ulysses Observations, Proc. 23rd Int. Cosmic Ray Conf. (Calgary), 3, 346, 1993. Simpson, J.A., J.D. Anglin, A. Balogh, M. Bercovitch, J.M. Bouman, E.E. Budzinski, J.R. Burrows, R. Carvell, J.J. Connell, R. Ducros, P. Ferrando, J. Firth, M. Garcia-Munoz, J. Henrion, R.J. Hynds, B. Iwers, R. Jacquet, H. Kunow, G. Lentz, R.G. Marsden, R.B. McKibben, R. Mueller-Mellin, D.E. Page, M. Perkins, A. Raviart, T.R. Sanderson, H. Sierks, L. Treguer, A.J. Tuzzolino, K.-P. Wenzel, and G. Wibberenz, The Ulysses cosmic ray and solar particle investigation, Astron. Astrophys. Suppl. Set: 92, 365-399, 1992. Zhang, M., R.B. McKibben, and J.A. Simpson, Relativistic Electron Flux Anisotropies in the Dusk-Side Jovian Magnetosphere: A Test for Source Location and Escape Mechanism, Planet. Space Sci, 41(11/12), 1029, 1993. (https://doi.org/10.1016/0032-0633(93)90107-D)