DATA_SET_DESCRIPTION |
Data Set Overview
=================
Raw data including single counter rates for the Semiconductor
Detector D1 and the Anticoincidence A.
Data
====
COSPIN-KET RECORD FORMAT
(REFERENCE: [SIMPSONETAL1992A] page 384, table 10)
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 !!!!!
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