Data Set Overview
      =================
      Instrument P.I.       : James W. Warwick
      Data Supplier         : Michael L. Kaiser
      Data sampling rate    : 48 seconds
      Data Set Start Time   : 1979-04-25T00:00:00.000Z
      Data Set Stop Time    : 1979-08-04T23:04:00.000Z

      This data set consists of edited browse data derived from an
      original data set obtained from the Voyager 2 Planetary Radio
      Astronomy (PRA) instrument in the vicinity of Jupiter. Data
      are provided for 70 instrument channels covering the range
      from 1.2 kHz to 1326 kHz in uniform 19.2 kHz steps, each 1 kHz
      wide. Data are included for the period 1979-04-25 00:00:00.000
      through 1979-08-04 23:04:00.000. In order to produce this data
      set from the original raw PRA data, several steps have been
      taken:

      1. The PRA operates in a variety of modes; data from modes in
      which the receiver does not scan rapidly through its frequency
      range have been removed;
      2. The data have been calibrated as best we know how;
      3. The data have been split into Left Hand Circular (LHC) and
      Right Hand Circular (RHC) components;
      4. The data have been binned into 48-second intervals.

      Thus, values at a given channel are separated in time by an
      increment of 48 seconds; each 48-second time interval has
      associated with it a value for LHC polarization and one for
      RHC polarization.

      During data gaps, the entire record is absent from the
      data set; that is, missing records have not been zero-filled
      or otherwise marked. Bad data within a record is indicated by
      the value zero, which cannot otherwise occur.

      Each datum is returned as a 16-bit quantity; it represents the
      mean power received in the given channel at the specified time
      and polarization. The returned quantity is the value in mB
      about a reference flux density. To convert a returned quantity
      to flux, use the formula:

      flux   = 7.0x10^(-22)x10^(mB/1000) W m-2 Hz-1

      Parameters
      ==========

      Data Set Parameter 'RADIO WAVE SPECTRUM'
      ----------------------------------------
      Data Set Parameter Name        : RADIO WAVE SPECTRUM
      Data Set Parameter Unit        : MILLIBEL
      Sampling Parameter Name        : TIME
      Sampling Parameter Unit        : SECOND
      Sampling Parameter Resolution  : 0.001
      Sampling Parameter Interval    : 48
      Minimum Available Sampling Int : 12
      Noise Level                    : 2400

      A set of derived parameters consisting of power fluxes at
      various contiguous frequencies over a range of frequencies.
      Millibels may be converted to watts/m**2/Hz by using the
      formula for flux indicated above.

      Source Instrument Parameters
      ============================
      Instrument Host ID              : VG2
      Data Set Parameter Name         : RADIO WAVE SPECTRUM
      Instrument Parameter Name       : WAVE FLUX DENSITY
                                        ELECTRIC FIELD WAVEFORM
                                        ELECTRIC FIELD COMPONENT
                                        MAGNETIC FIELD COMPONENT
                                        WAVE ELECTRIC FIELD INTENSITY
                                        WAVE MAGNETIC FIELD INTENSITY
      Important Instrument Parameters : 1 (for all parameters)

      Data Coverage
      =============
Filename   Records               Start                 Stop
-------------------------------------------------------------------
Volume ID: VG_1502
PRA.DAT  128633   1979-04-25T00:00:00.000Z  1979-08-04T23:04:00.000Z

Confidence Level Overview
      =========================
      This data set includes all the available low-rate scanning
      mode data for the frequency range below 1326 kHz for the time
      interval covered. Known bad data have been set to zero. Data
      which appear to exceed the Full Scale Deflection (FSD) of the
      instrument (i.e. the most intense signal which can be measured
      reliably) have also been set to a zero (should they occur).
      Planetary Radio Astronomy (PRA) suffers from interference from
      many other instruments aboard the spacecraft. No attempt had
      been made to remove these interferences in this data set. Two
      obvious examples are the 136 and 193 kHz channels which are
      nearly always contaminated by interference.

      The separation into LHC and RHC polarization components is
      performed on the basis of the polarization of the incoming
      wave as perceived by the instrument. This takes into account
      neither the antenna transfer function nor the spacecraft
      orientation with respect to the source. In general, the
      mapping of perceived polarization back to emitted polarization
      cannot be solved without a knowledge of both of these factors,
      as well as a knowledge of the type of polarization coming from
      the source region (e.g. is it linear or circularly
      polarized?).

      Most planetary emissions are circularly polarized. Below is a
      table showing the response of the experiment to a low frequency
      (100 kHz) LHC wave. The response does not change much up to
      about 5 MHz.

      The coordinate system used is: THETA == 0 is along the MAG
      boom; PHI == 0 is the bisector of the two PRA antennas. The
      third column is the apparent value of the left hand component
      as perceived by the receiver. That is, a value of +1.0
      indicates that the incoming LHC wave is correctly detected as
      a pure LHC wave. A value of -1.0 will be detected as being of
      the correct strength, but incorrect polarity. A value of, say,
      0.6 indicates that the total energy is split 60% into the
      apparent LHC component and 40% into the apparent RHC component.