/*===========================================================================*/ /* Streamlined Data Set Template (combined EB and SC data sets) */ /*===========================================================================*/ /* Template: Data Set Template Rev: 1993-09-24 */ /* Note: Complete one for each data set. Identify multiple targets */ /* associated with the data set by repeating the 3 lines for the */ /* DATA_SET_TARGET object. Identify multiple hosts associated */ /* with the data set by repeating the 4 lines for the */ /* DATA_SET_HOST object. Identify multiple references associated */ /* with the data set by repeating the 3 lines of the */ /* DATA_SET_REFERENCE_INFORMATION object. */ /* Hierarchy: DATA_SET */ /* DATA_SET_INFORMATION */ /* DATA_SET_TARGET */ /* DATA_SET_HOST */ /* DATA_SET_REFERENCE_INFORMATION */ OBJECT = DATA_SET DATA_SET_ID = "VG1-SS-PWS-4-SUMM-SA1HOUR-V1.0" OBJECT = DATA_SET_INFORMATION DATA_SET_NAME = " VG1 SOLAR WIND PWS HOURLY AVERAGE SPECTRUM ANALYZER V1.0" DATA_SET_COLLECTION_MEMBER_FLG = N START_TIME = 1977-09-05 STOP_TIME = "N/A" DATA_SET_RELEASE_DATE = 1995-01-16 PRODUCER_FULL_NAME = "DR. WILLIAM S. KURTH" DETAILED_CATALOG_FLAG = N DATA_SET_DESC = " This data set consists of calibrated hourly averages and peak values of the wave electric field intensities from the Voyager 1 Plasma Wave Receiver spectrum analyzer obtained during the cruise portions of the Voyager 1 mission, including data acquired during the various encounters. For each hour, an average and peak field strength is determined for each of the 16 spectrum analyzer channels whose center frequencies range from 10 Hertz to 56.2 kiloHertz and which are logarithmically spaced in frequency, four channels per decade. The time associated with each set of intensities (16 channels) is the time of the beginning of the averaging interval. During data gaps where complete spectra are missing, no entries exist in the file, that is, the gaps are not zero-filled or tagged in any other way. When one or more channels are missing within a scan, the missing measurements are zero-filled. Values are in units of electric field strength (V/m). Spectral density units may be obtained by dividing the square of the electric field value by the nominal frequency bandwidth of the corresponding spectrum analyzer channel. Finally, power flux may be obtained by dividing the spectral density by the impedance of free space in ohms (376.73). The center frequencies and bandwidths of each PWS spectrum analyzer channel for the Voyager 1 PWS are given below: VOYAGER 1 PWS SPECTRUM ANALYZER Channel Center Frequency Bandwidth 1 10.0 Hz 2.99 Hz 2 17.8 Hz 3.77 Hz 3 31.1 Hz 7.50 Hz 4 56.2 Hz 10.1 Hz 5 100. Hz 13.3 Hz 6 178. Hz 29.8 Hz 7 311. Hz 59.5 Hz 8 562. Hz 106. Hz 9 1.00 kHz 133. Hz 10 1.78 kHz 211. Hz 11 3.11 kHz 298. Hz 12 5.62 kHz 421. Hz 13 10.0 kHz 943. Hz 14 17.8 kHz 2110. Hz 15 31.1 kHz 4210. Hz 16 56.2 kHz 5950. Hz Additional information about this dataset and the instrument which produced it can be found elsewhere in this catalog. A complete instrument description can be found in Scarf and Gurnett [1977]." CONFIDENCE_LEVEL_NOTE = " This data set includes all available spectrum analyzer data within the interval of time covered. The data obtained within planetary magnetospheres has been cleaned as well as possible for periodic noise spikes due to a stepper motor operating on the LECP and a modulated grid within the plasma instrument. This periodic noise spike elimination has not, in general, been performed for the data taken outside of planetary magnetosphere (in the solar wind). Other possible sources of noise which may be present include random intense spikes of noise below 1 kiloHertz due to the operation of attitude control thrusters. Randomly occurring spikes or time periods of intense spikes over the entire frequency range are indicative of telemetry errors. To make this data set as useful as possible, we have tried to eliminate the most obvious telemetry errors by not including any noise spike of more than 75 dn in the peaks or averages except during the encounter intervals when only the periodic spikes have been eliminated as indicated above. 75 dn corresponds to an electric field of approximately 0.0001 V/m, but this varies somewhat from channel to channel. The choice of this amplitude as a criterion results from extensive study of the data. Only rarely are amplitudes so large encountered during cruise, and possible example of affected phenomena would be Langmuir waves upstream of Jupiter. This criterion leaves numerous noise spikes which are likely thruster firing interference or data hits, but to eliminate bursts of much lower amplitude would likely delelete some valid data points. We STRONGLY urge CAUTION in using these average data sets! A good practice for any serious use would be to start from the original data, find the phenomenon of interest, and then apply the above or other despiking alorithms with careful tests to see that the phenomenon of interest is not adversely affected. The original data are included in the the data set called VG1-SS-PWS-2-RDR-SA-V1.0. The 17.8-Hz channel is sometimes contaminated by interference from the PRA instrument, depending on that instrument's mode. This interference is at a relatively constant level." END_OBJECT = DATA_SET_INFORMATION OBJECT = DATA_SET_TARGET TARGET_NAME = "SOLAR WIND" END_OBJECT = DATA_SET_TARGET OBJECT = DATA_SET_HOST INSTRUMENT_HOST_ID = VG1 INSTRUMENT_ID = PWS END_OBJECT = DATA_SET_HOST OBJECT = DATA_SET_REFERENCE_INFORMATION REFERENCE_KEY_ID = "GURNETT&SCARF1977" END_OBJECT = DATA_SET_REFERENCE_INFORMATION END_OBJECT = DATA_SET