CCSD3ZF0000100000001NJPL3IF0PDSX00000001
PDS_VERSION_ID                     = PDS3

RECORD_TYPE                        = STREAM
OBJECT                             = DATA_SET
  DATA_SET_ID                      = "ULY-J-COSPIN-HFT-3-RDR-FLUX-HIRES-V1.0"

  OBJECT                           = DATA_SET_INFORMATION
    DATA_SET_NAME                  = "ULY JUP COSPIN HIGH FLUX TELESCOPE HIGH
RES. ION FLUX"
    DATA_SET_COLLECTION_MEMBER_FLG = N
    START_TIME                     = 1992-01-25T00:00:13.216Z
    STOP_TIME                      = 1992-02-18T00:02:41.450Z
    DATA_SET_RELEASE_DATE          = 1998-05-01
    PRODUCER_FULL_NAME             = "J. DAVID ANGLIN"
    DETAILED_CATALOG_FLAG          = "N"
    DATA_OBJECT_TYPE               = "TIME SERIES"
    DATA_SET_DESC                  = "

      Data Set Overview
      =================
      This data set contains ion flux data recorded by the COSPIN
      High Flux Telescope (HFT) during the Ulysses Jupiter encounter
      1992-Jan-25 to 1992-Feb-18.

      Record format is essentially as follows:

       END TIME    RATENAME   LENGTH OF   DEAD TIME   COUNTS
      OF INTERVAL              INTERVAL    FACTOR

      Fields are space separated.

      Ratenames are ASCII strings indicating channel, mode etc.
      Records with bad data have been removed.  'C' is appended to
      the ratename when instrument is in calibrate mode.  See
      [SIMPSONETAL1992A] for channel energy ranges.

      End times are in the format yyyy-mm-ddThh:mm:ss.sssZ (UTC).

      Interval times are in milliseconds.

      The dead time factor is either 1 (non-sectored data) or 32
      (sectored data).

      The flux of whatever the channel responds to is given by:
      FLUX = 1000*DTF*COUNTS/LOI/0.0322 (counts/cm**2/s/sr)

      While C and spreadsheets can easily read these files, it is
      difficult to read these files in some programming languages
      (e.g., FORTRAN or IDL) because of the variable length strings
      in the first field.  These files are easily manipulated using
      the UNIX awk and grep tools.

      [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]

(the following table is adapted from [SIMPSONETAL1992A])  

TABLE 9. High flux telescope data channels.

--------------------------------------------------------------------
Name  Discri-  Primary  Energy   Species   Geo-     Avg.     Sectors
      minator  Parti-   Range*     for    metric  Time Res-
      Discri-  cle     (MeV(/n))  Range   Factor   olution
      minator  Type               Energy  (cm^2
       Level                               sr)
--------------------------------------------------------------------
        J0     Z>=1   0.28-7.0   Protons
        J1     Z>=1   0.50-2.27  Protons
        J2     Z>=1   0.76-1.37  Protons          16/readout
F1**    J4     Z>=2   0.36-3.9   Helium   0.033  256 for same   --
        J6     Z>=2   0.51-2.26  Helium           disc. level
        J8     Z>=2   0.64-1.66  Helium
        J10    Z>=2   0.78-1.35  Helium

F2      Lo     Z>=1   0.29-6.7   Protons  0.033       16        --
        Hi     Z>=1   0.55-1.35  Protons

F2s             [same as for F2]                      32        8
                                                             sampled
                                                             from 32
                                                     128        32

F3             Z>=2   0.68-1.56  Helium   0.033                 --
F4             Z>=3   0.8-4.9    Carbon   0.033                 --
F5             Z>=12  0.8-34**   Iron     0.033                 --
--------------------------------------------------------------------
*  Energy ranges from range-energy relations
** F1 steps through 16 discriminator levels in sequence in standard
   flight mode"

    CONFIDENCE_LEVEL_NOTE          = "

      Confidence Level Overview
      =========================
      The user of this data should consult [ANGLINETAL1997] for
      details regarding the operation of the HFT instrument in the
      Jupiter environment. In particular,  the calculation of ion
      fluxes is model dependent since each HFT rate channel responds
      to a range of ion species. The rate channels also contain a
      small background rate arising from cosmic rays, radioactive
      decay and other phenomena. This background has not been
      subtracted from the observed data. The deadtime parameter does
      not correct for electronic deadtime at high counting rates.

      Files containing corrected deadtimes have been included in
      this data set for days 38-39."
  END_OBJECT                       = DATA_SET_INFORMATION

  OBJECT                           = DATA_SET_TARGET
    TARGET_NAME                    = JUPITER
  END_OBJECT                       = DATA_SET_TARGET

  OBJECT                           = DATA_SET_HOST
    INSTRUMENT_HOST_ID             = ULY
    INSTRUMENT_ID                  = "COSPIN-HFT"
  END_OBJECT                       = DATA_SET_HOST

  OBJECT                           = DATA_SET_REFERENCE_INFORMATION
    REFERENCE_KEY_ID               = "ANGLINETAL1997"
  END_OBJECT                       = DATA_SET_REFERENCE_INFORMATION
  OBJECT                           = DATA_SET_REFERENCE_INFORMATION
    REFERENCE_KEY_ID               = "SIMPSONETAL1992A"
  END_OBJECT                       = DATA_SET_REFERENCE_INFORMATION
  OBJECT                           = DATA_SET_REFERENCE_INFORMATION
    REFERENCE_KEY_ID               = "ZHANGETAL1995"
  END_OBJECT                       = DATA_SET_REFERENCE_INFORMATION
  
END_OBJECT                         = DATA_SET

END