Data Set Overview
      =================
      Electron rates and Alpha and proton intensities as described
      below.

      Data
      ====
      COSPIN-KET RECORD FORMAT
      (REFERENCE: [SIMPSONETAL1992A], page 384, table 10)

      FORTRAN RECORD FORMAT for TYYDOY.TAB

           implicit real(k)
           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

      [please note that time-stamp and record format have been
       changed by the PDS/PPI Node for the sake of consistency with
       other data sets found on this volume]

      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)
        P4:    protons (5.4-23.1 MeV)
        E4:    electrons (2.5-7.0 MeV)

        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

           K21_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  !!!!!

Confidence Level Overview
      =========================
      Some confidence level information provided in Data Set
      Overview. For more information regarding the confidence
      level of this data set please contact:
        HORST KUNOW
        Institut fur Reine und Angewandte Kernphysik
        Universitat Kiel
        Otto-Hahn-Platz 1
        24118 Kiel
        GERMANY
        Phone:    49-431-880-2487
        SPAN/NSI: IFKKI::KUNOW