/************************ Voyager Mission Template ****************************/ /* MODIFICATIONS: */ /* 920929 RMONARREZ */ /* Generated from database */ /* Template: Mission Template Rev: 19890121 */ /* Note: The following templates form part of a standard set */ /* for the submission of a mission to the PDS. */ /* Hierarchy: MISSION */ /* MSNINFO */ /* MSNPHSINFO */ /* MSNREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = MISSION MISSION_NAME = "VOYAGER" OBJECT = MSNINFO MISSION_START_DATE = 1972-07-01 MISSION_STOP_DATE = UNK MISSION_ALIAS_NAME = "MJS77" MISSION_DESC = " The Voyager mission was the product of a redesign of the Outer Planets grand tour conceived in the late 1960s. Direct measurement instruments on Voyager measured cosmic ray particles, low energy charged particles, magnetic fields, plasma particles and plasma waves. The remote sensing investigations were essentially astronomical in nature, measuring the lighter radio waves reflected or emitted by the planets and their satellites. A final Voyager investigation used the radio telemetry link between the spacecraft and controllers on Earth to probe the atmospheres of the planets and satellites and to determine the masses of planets and satellites as the spacecraft passed near them. The Voyager mission used two identical spacecraft. Each Voyager spacecraft followed a billion-kilometer path to Jupiter, where the gravitational pull of the giant planet was used to redirect the trajectory toward Saturn. Voyager 1 received a larger kick from the gravitational slingshot than Voyager 2, increasing its lead so that it arrived at Saturn in November 1980, about nine months before Voyager 2. During the Saturn flyby, Voyager 1s trajectory was deflected northward of the ecliptic plane, in which the solar system planets orbit. Voyager 2 used the Saturn flyby to redirect its path toward a Uranus encounter in 1986. (Refer to Morrison, 1982)" MISSION_OBJECTIVES_SUMMARY = " Voyager's objective was the exploration of the two giant planets, Jupiter and Saturn, and their magnetospheres and satellites. Major emphasis was placed on studying the satellites, many of which are planet-sized worlds, in as much detail as possible. The study of Titan, the only satellite in the solar system known to have an extensive atmosphere, was nearly as high a priority as studies of Saturn itself.(Refer to Morrison, 1982)" OBJECT = MSNPHSINFO SPACECRAFT_ID = VG2 TARGET_NAME = NEPTUNE MISSION_PHASE_TYPE = ENCOUNTER SPACECRAFT_OPERATIONS_TYPE = FLYBY MISSION_PHASE_START_TIME = 1989-06-05 MISSION_PHASE_STOP_TIME = 1989-10-02 MISSION_PHASE_DESC = " This mission phase covers all Neptune encounter science activities and includes both the observatory and close encounter periods." END_OBJECT = MSNPHSINFO OBJECT = MSNPHSINFO SPACECRAFT_ID = VG2 TARGET_NAME = URANUS MISSION_PHASE_TYPE = ENCOUNTER SPACECRAFT_OPERATIONS_TYPE = FLYBY MISSION_PHASE_START_TIME = 1985-11-04 MISSION_PHASE_STOP_TIME = 1986-02-25 MISSION_PHASE_DESC = " This mission phase covers all Uranus encounter science activities and includes both the observatory and close encounter periods." END_OBJECT = MSNPHSINFO END_OBJECT = MSNINFO OBJECT = MSNREFINFO REFERENCE_KEY_ID = "MORRISON1982" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MISSION DESCRIPTION" JOURNAL_NAME = "NASA PUBLICATION" PUBLICATION_DATE = 1982 REFERENCE_DESC = " Morrison, D., Voyages to Saturn, NASA SP-451, Washington, 1982." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DAVID MORRISON" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = MSNREFINFO END_OBJECT = MISSION /********************** Voyager Spacecraft Template **************************/ /* MODIFICATIONS: */ /* 920929 RMONARREZ */ /* Generated from database */ /* Template: Spacecraft Template Rev: 19890121 */ /* Note: The following templates form part of a standard */ /* set for the submission of a spacecraft to the PDS. */ /* Hierarchy: SPACECRAFT */ /* SCINFO */ /* PLATFORM */ /* SCREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SPACECRAFT SPACECRAFT_ID = "VG2" OBJECT = SCINFO LAUNCH_DATE = 1977-08-20 INSTRUMENT_HOST_NAME = "VOYAGER 2" INSTRUMENT_HOST_TYPE = "SPACECRAFT" SPACECRAFT_DESC = " The two identical Voyager spacecraft, each with a mass of 815 kilograms, are among the most autonomous, sophisticated robots ever sent to explore other worlds. Each is a self-contained system, carrying its own power, propulsion, communications systems, and science instruments. Communication between the spacecraft and Earth is carried out via a high-gain radio antenna 3.7 meters in diameter that is always oriented toward the Earth. The radio transmitters (there are two complete systems to provide backup in case of failure) have only 23 watts of transmitting power, about the power of a refrigerator light bulb. Yet with the aid of the sensitive receivers of the NASA Deep Space Network of tracking stations, this 23-watt radio can transmit data over a distance of 1 billion kilometers at the enormous rate of 115200 bits per second, almost a hundred times faster than Pioneer. At the greater distance to Saturn, a lower data rate of 44800 bits per second was adopted. In addition, the Voyager spacecraft carried a digital tape recorder with a storage capacity of 500 million bits. The power for each Voyager spacecraft is supplied by three radioisotope thermoelectric generators (RTGs) that produce about 400 watts of electrical power. Each spacecraft is controlled by a set of interconnected electronic brains called the attitude and articulation control subsystem (AACS), the flight data subsystem (FDS) and the computer command subsystem (CCS). Rather than being instructed directly by ground controllers (as were the pioneers), the Voyager control systems accept precoded sets of several thousand instructions that can provide autonomous operation for days or weeks at a time. These systems also include elaborate error detection and correction routines so the spacecraft can locate and correct problems before ground controllers are aware of them. The AACS, FDS, and CCS can be reprogrammed in flight if necessary, allowing great flexibility in responding to changing conditions or science objectives." END_OBJECT = SCINFO OBJECT = PLATFORM PLATFORM_OR_MOUNTING_NAME = "MAGNETOMETER BOOM" PLATFORM_OR_MOUNTING_DESC = " A 13-meter-long boom that was unfurled and extended automatically after launch." END_OBJECT = PLATFORM OBJECT = PLATFORM PLATFORM_OR_MOUNTING_NAME = "SCAN PLATFORM" PLATFORM_OR_MOUNTING_DESC = " The part of the Voyager spacecraft that carries the imaging, IRIS, ultraviolet, and photopolarimeter instruments. It can be pointed to any part of the sky by rotating around two axes (azimuth and elevation)" END_OBJECT = PLATFORM OBJECT = PLATFORM PLATFORM_OR_MOUNTING_NAME = "SCIENCE BOOM" PLATFORM_OR_MOUNTING_DESC = " The Voyager science instrument boom carries the plasma detector, cosmic ray detector and the low energy charged particle detector." END_OBJECT = PLATFORM OBJECT = PLATFORM PLATFORM_OR_MOUNTING_NAME = "SPACECRAFT BUS" PLATFORM_OR_MOUNTING_DESC = " The basic structure of the spacecraft is called the 'bus', which carries the various engineering subsystems and scientific instruments. It is like a large ten-sided box. The centerline of the bus is called the z-axis (and thus the High Gain Antenna) points to Earth. The spacecraft is designed to roll about this axis by firing small thrusters which are attached to the bus. The thrusters are fueled by a liquid called hydrazine. Each of the ten sides of the bus contains a compartment (a bay) that houses various electronic assemblies. Bay 1, for example, contains the radio transmitters. The bays are numbered from 1 to 10 (numbered clockwise as see from Earth). Two additional turn axes, at right angles to the roll axis and to each other, are needed to give the spacecraft full maneuverability. These are the x-axis (pitch) and the y-axis (yaw). The booms supporting the nuclear power sources and the scan platform lie along the y-axis." END_OBJECT = PLATFORM OBJECT = SCREFINFO REFERENCE_KEY_ID = "MORRISON1982" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MISSION DESCRIPTION" JOURNAL_NAME = "NASA PUBLICATION" PUBLICATION_DATE = 1982 REFERENCE_DESC = " Morrison, D., Voyages to Saturn, NASA SP-451, Washington, 1982." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DAVID MORRISON" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = SCREFINFO END_OBJECT = SPACECRAFT /************************ CRS Instrument Template *****************************/ /* MODIFICATION */ /* 920806 JPLPDS::RMONARREZ */ /* received by mail */ /* 92-08 EFRIED */ /* 920916 EFRIED */ /* last changes made */ /* Template: Spacecraft Instrument Template Rev: 19890121 */ /* Note: The following templates form part of a standard */ /* set for the submission of a spacecraft instrument */ /* to the PDS. */ /* Hierarchy: SCINSTRUMENT */ /* INSTINFO */ /* INSTDETECT */ /* INSTELEC */ /* INSTFILTER */ /* INSTOPTICS */ /* SCINSTOFFSET */ /* INSTSECTION */ /* INSTSECTINFO */ /* INSTSECTFOVS */ /* INSTSECTPARM */ /* INSTSECTDET */ /* INSTSECTELEC */ /* INSTSECTFILT */ /* INSTSECTOPTC */ /* INSTMODEINFO */ /* INSTMODESECT */ /* INSTREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCINSTRUMENT SPACECRAFT_ID = VG2 INSTRUMENT_ID = CRS OBJECT = INSTINFO INSTRUMENT_NAME = "COSMIC RAY SYSTEM" INSTRUMENT_TYPE = "CHARGED PARTICLE ANALYZER" PI_PDS_USER_ID = ESTONE NAIF_DATA_SET_ID = "N/A" BUILD_DATE = 1976 INSTRUMENT_MASS = 7 INSTRUMENT_HEIGHT = 0.177 INSTRUMENT_LENGTH = 0.286 INSTRUMENT_WIDTH = 0.203 INSTRUMENT_MANUFACTURER_NAME = SPACETAC INSTRUMENT_SERIAL_NUMBER = FU2 INSTRUMENT_DESC = " The Voyager cosmic ray experiment (CRS) measures charged particles in charge, mass and energy intervals summarized as follows: (i) Nuclei charge and energy spectra: Z = 1-30, energy range 1-500 MeV for H to 2.5-500 MeVuc for Fe. (ii)Isotopes: Z = 1-8 (delta M = 1), energy range 2-75 MeVuc. (iii) Electrons: 3-110 MeV (iv) Anisotropies: All components ranging from H (1-150) to Fe (2.7-500 MeVuc) as well as 3-110 MeV electrons. CRS has three detector systems containing a total of seven particle telescopes consisting entirely of solid-state charged-particle detectors. The detector systems are: the High Energy Telescope System (HETS), consisting of two double ended telescopes each containing eight detectors; the Low Energy Telescope System (LETS), consisting of four telescopes with four detectors each; and the Electron Telescope (TET), with eight detectors. The combination of these telescope systems achieve the measurements described above through multi-parameter analysis of individual particle events. The analyzed events occur at a rate of a few per second, and consist of pulse height information from three detectors or combinations of detectors. More detailed information can be found in Stone et al., Space Science Reviews, 1977, and Stilwell et al., IEEE Transactions on Nuclear Science, 1979. In addition to the event analysis, each detector, and various combinations of detectors in coincidence/anti-coincidence, have counting-rate data for all events occurring in that detector (or combination) satisfying certain electronic requirements (the pulses should be above a certain energy threshold and sufficiently spaced in time for discrimination). The counting-rate data generally have an associated geometry factor and energy interval (or lower energy threshold), which can be used to calculate fluxes of the relevant particle species in that energy interval. However, these are often ill-defined because of the varying thickness of passive shielding material which must be penetrated by particles reaching individual detectors. It is therefore essential to consider the sensitivity to particles of different species and of different energy intervals when interpreting the counting-rate data. Also, during times of high particle flux, it is sometimes necessary to correct the counting rates for non-linear detector response due to deadtime, for pulse pile-up and for discriminator baseline shifts." SCIENTIFIC_OBJECTIVES_SUMMARY = " To provide measurements of the cosmic ray flux and energy spectra during the cruise phase of the Voyager mission, and of the trapped, energetic particles during planetary encounters. The planetary data are used to study the dynamics of the radiation belts in each magnetosphere, including the source, loss, transport and energization mechanisms, elemental composition and satellite/ring interactions." INSTRUMENT_CALIBRATION_DESC = " Laboratory calibrations of the individual detectors and the complete telescopes have been made with particle accelerators and radioactive sources. A calibration file for the electron telescope is included in PDS (see the DATA_SET_OR_INST_PARM_DESC). The calibrations of the electron telescope, which need to be considered in the data analysis, are described in internal reports at CalTech. Copies of these documents can be obtained from the experimental representatives." OPERATIONAL_CONSID_DESC = " The instrument operates continuously sampling data over uniform accumulation intervals. The accumulation intervals vary for the different rate numbers, of which there are 135 consisting of the individual detector and multiple detector counting rates being used in a particular instrument mode. They are always multiples of six seconds and are sampled in a sequence which repeats every 96 seconds, with some rates being sampled continuously over each 96 second period, and some (including all of the single detector rates) only with a single six second sample each 96 seconds. The mode, which determines the various combinations of detectors that are included in the multiple detector measurements, is commandable by the spacecraft and during planetary encounters is usually set to a mode which provides good data return for high flux environments." END_OBJECT = INSTINFO OBJECT = INSTDETECT DETECTOR_ID = CRS DETECTOR_TYPE = "SOLID STATE" DETECTOR_ASPECT_RATIO = "N/A" MINIMUM_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" NOMINAL_OPERATING_TEMPERATURE = 273 DETECTOR_DESC = " The Cosmic Ray System (CRS) instrument contains 40 solid-state silicon detectors that are used individually and in combinations (using coincidence and anti-coincidence criteria) to detect and characterize charged particles. The detector effective thicknesses range from 35 microns to 6 mm to cover a broad range of particle energy and mass characteristics." SENSITIVITY_DESC = " In the case of nuclear particles, detectors count the particles that have energy deposits which exceed the detectors individual threshold with an efficiency that approaches 1. Therefore the sensitivity is strictly a function of the geometry factors of the detectors and their energy and species band widths (these are documented elsewhere in this catalog). The geometry factors have units of area times steradians (cm**2 sr). In the case of electrons, the detector efficiencies are less than 1, leading to energy and direction dependent effective geometry factors which are determined by laboratory calibration. Tables of these geometry factors are included in this catalog, and need to be unfolded from the electron counting rates to determine the absolute flux levels." END_OBJECT = INSTDETECT OBJECT = INSTELEC ELECTRONICS_ID = CRS ELECTRONICS_DESC = " Timed accumulations of particle counts satisfying various analog pulse-height discrimination levels and simultaneous analog pulse-height discriminations for multiple detectors. Pulse-height analog-to-digital conversions from multiple, simultaneous detectors for direct telemetry. For details see Stilwell et al., IEEE Transactions on Nuclear Science, 1979." END_OBJECT = INSTELEC OBJECT = INSTFILTER FILTER_NUMBER = "N/A" FILTER_NAME = "N/A" FILTER_TYPE = "N/A" MINIMUM_WAVELENGTH = "N/A" CENTER_FILTER_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" MEASUREMENT_WAVE_CALBRT_DESC = "N/A" END_OBJECT = INSTFILTER OBJECT = INSTOPTICS TELESCOPE_ID = "N/A" TELESCOPE_FOCAL_LENGTH = "N/A" TELESCOPE_DIAMETER = "N/A" TELESCOPE_F_NUMBER = "N/A" TELESCOPE_RESOLUTION = "N/A" TELESCOPE_TRANSMITTANCE = "N/A" TELESCOPE_T_NUMBER = "N/A" TELESCOPE_T_NUMBER_ERROR = "N/A" TELESCOPE_SERIAL_NUMBER = "N/A" OPTICS_DESC = "N/A" END_OBJECT = INSTOPTICS OBJECT = SCINSTOFFSET PLATFORM_OR_MOUNTING_NAME = "SCIENCE BOOM" CONE_OFFSET_ANGLE = "N/A" CROSS_CONE_OFFSET_ANGLE = "N/A" TWIST_OFFSET_ANGLE = "N/A" INSTRUMENT_MOUNTING_DESC = " The Cosmic Ray System (CRS) instrument is mounted about half way along the science boom on the side of the high-gain antenna, so as to provide an unobstructed nominal field of view for each of the particle telescopes. The nominal unit vectors of each of the telescope bore sights relative to the spacecraft fixed coordinate system are as follows: LETA .9063078, 0.0, .4226183 LETB .2862054, .7455905, -.6018150 LETC -.9063078, 0.0, -.4226183 LETD .3150813, -.6665596, -.6755902 HET1 -.7263100, .4716712, .5000000 HET2(Voyager1) -.6617401, -.7096294, .2419219 HET2(Voyager2) -.9372337, .2511310, .2419219" END_OBJECT = SCINSTOFFSET OBJECT = INSTSECTION SECTION_ID = CRS OBJECT = INSTSECTINFO SCAN_MODE_ID = "N/A" DATA_RATE = "N/A" SAMPLE_BITS = 12 TOTAL_FOVS = "N/A" OBJECT = INSTSECTFOVS FOV_SHAPE_NAME = "N/A" HORIZONTAL_PIXEL_FOV = "N/A" VERTICAL_PIXEL_FOV = "N/A" HORIZONTAL_FOV = "N/A" VERTICAL_FOV = "N/A" FOVS = "N/A" END_OBJECT = INSTSECTFOVS END_OBJECT = INSTSECTINFO OBJECT = INSTSECTPARM INSTRUMENT_PARAMETER_NAME = "D1 RATE" MINIMUM_INSTRUMENT_PARAMETER = "N/A" MAXIMUM_INSTRUMENT_PARAMETER = "N/A" NOISE_LEVEL = "N/A" INSTRUMENT_PARAMETER_UNIT = "COUNTS/SECOND" SAMPLING_PARAMETER_NAME = TIME MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 96.0 SAMPLING_PARAMETER_RESOLUTION = 6.0 SAMPLING_PARAMETER_UNIT = SECOND END_OBJECT = INSTSECTPARM OBJECT = INSTSECTPARM INSTRUMENT_PARAMETER_NAME = "D2 RATE" MINIMUM_INSTRUMENT_PARAMETER = "N/A" MAXIMUM_INSTRUMENT_PARAMETER = "N/A" NOISE_LEVEL = "N/A" INSTRUMENT_PARAMETER_UNIT = "COUNTS/SECOND" SAMPLING_PARAMETER_NAME = TIME MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 96.0 SAMPLING_PARAMETER_RESOLUTION = 6.0 SAMPLING_PARAMETER_UNIT = SECOND END_OBJECT = INSTSECTPARM OBJECT = INSTSECTPARM INSTRUMENT_PARAMETER_NAME = "D1 RATE" MINIMUM_INSTRUMENT_PARAMETER = "N/A" MAXIMUM_INSTRUMENT_PARAMETER = "N/A" NOISE_LEVEL = "N/A" INSTRUMENT_PARAMETER_UNIT = "COUNTS/SECOND" SAMPLING_PARAMETER_NAME = TIME MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 6.0 SAMPLING_PARAMETER_RESOLUTION = 6.0 SAMPLING_PARAMETER_UNIT = SECOND END_OBJECT = INSTSECTPARM OBJECT = INSTSECTDET DETECTOR_ID = CRS END_OBJECT = INSTSECTDET OBJECT = INSTSECTELEC ELECTRONICS_ID = CRS END_OBJECT = INSTSECTELEC OBJECT = INSTSECTFILT FILTER_NUMBER = "N/A" END_OBJECT = INSTSECTFILT OBJECT = INSTSECTOPTC TELESCOPE_ID = "N/A" END_OBJECT = INSTSECTOPTC END_OBJECT = INSTSECTION OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = ENCOUNTER GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = REALTIME INSTRUMENT_POWER_CONSUMPTION = 5.0 INSTRUMENT_MODE_DESC = " During the planetary encounters the instrument is placed in a modes designed to optimize the data return in high particle flux environments. These involve adjustments to the multiple detector confidence requirements and do not effect the single detector rates. Detailed knowledge of the instrument modes is not required to understand the data provided in this catalog." OBJECT = INSTMODESECT SECTION_ID = CRS END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO /* */ /* Repeat for "Playback Data" */ /* */ OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = ENCOUNTER GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "RECORDED DATA PLAYBACK" INSTRUMENT_POWER_CONSUMPTION = 5.0 INSTRUMENT_MODE_DESC = " During the planetary encounters the instrument is placed in a modes designed to optimize the data return in high particle flux environments. These involve adjustments to the multiple detector confidence requirements and do not effect the single detector rates. Detailed knowledge of the instrument modes is not required to understand the data provided in this catalog." OBJECT = INSTMODESECT SECTION_ID = CRS END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO /* */ /* End repeated info */ /* */ OBJECT = INSTREFINFO REFERENCE_KEY_ID = "STONEETAL1977" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "CRS DOCUMENTATION" JOURNAL_NAME = "SPACE SCIENCE REVIEWS" PUBLICATION_DATE = 1977-12-01 REFERENCE_DESC = " Scientific goals and operating characteristics of the CRS instrument" OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "E.C. STONE" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "STILWELLETAL1979" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "CRS DOCUMENTATION" JOURNAL_NAME = "IEEE TRANSACTIONS ON NUCLEAR SCIENCE" PUBLICATION_DATE = 1979 REFERENCE_DESC = " CRS operating characteristics, especially of electronics" OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "D.E. STILWELL" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO END_OBJECT = SCINSTRUMENT /********************* LECP INSTRUMENT **************************************/ /* MODIFICATIONS */ /* 920805 SJOY from JPLPDS::RMONARREZ 920527 */ /* received by mail */ /* 920814 EFRIED */ /* Capitalization of descriptions was changed from all UPPERCASE */ /* to normal format(UC -> LC). */ /* Inserted values for INST_MODE_DESC, REF_DESC, and */ /* AUTHOR_FULL_NAME. (All UC -> LC) */ /* Unknown value for SCAN_MODE_ID. */ /* 920916 EFRIED */ /* last changes made */ /* Template: Spacecraft Instrument Template - Rev: 19890121*/ /* Note: The following templates form part of a standard */ /* set for the submission of a spacecraft instrument */ /* to the PDS. */ /* */ /* Hierarchy: SCINSTRUMENT */ /* INSTINFO */ /* INSTDETECT */ /* INSTELEC */ /* INSTFILTER */ /* INSTOPTICS */ /* SCINSTOFFSET */ /* INSTSECTION */ /* INSTSECTINFO */ /* INSTSECTFOVS */ /* INSTSECTPARM */ /* INSTSECTDET */ /* INSTSECTELEC */ /* INSTSECTFILT */ /* INSTSECTOPTC */ /* INSTMODESECT */ /* INSTREFINFO */ /* REFERENCE */ /* REFAUTHORS */ /* */ OBJECT = SCINSTRUMENT SPACECRAFT_ID = "VG2" INSTRUMENT_ID = "LECP" OBJECT = INSTINFO INSTRUMENT_NAME = "LOW ENERGY CHARGED PARTICLE" INSTRUMENT_TYPE = "CHARGED PARTICLE ANALYZER" PI_PDS_USER_ID = "KRIMIGIS" NAIF_DATA_SET_ID = "N/A" BUILD_DATE = 1977-08-20 INSTRUMENT_MASS = 6.652000 INSTRUMENT_HEIGHT = UNK INSTRUMENT_LENGTH = UNK INSTRUMENT_WIDTH = UNK INSTRUMENT_MANUFACTURER_NAME = "THE JOHNS HOPKINS UNIVERSITY APPLIED PHYSICS LABORATORY" INSTRUMENT_SERIAL_NUMBER = "01" INSTRUMENT_DESC = " The low energy charged particle experiment employs a set of many solid state detectors arranged to characterize, with various levels of energy, directional, and compositional discriminations, the in-situ charged particle environment of the spacecraft, both within interplanetary and planetary magnetospheric regions. Electrons can be characterized, with various electron rate energy channels, between 22 keV and greater than 10 meV (mode dependent). Ions, without mass species discriminations, can be characterized with various ion rate energy channels between 28 keV and greater than 152 keV (mode dependent). Rate data is telemetered as simple counts per accumulation time period. The different channels correspond to different onboard energy discrimination windows (for ions the discrimination values are mass species dependent, leading to some ambiguity). Above about 200 keV/nucleon, the ions can be discriminated as to their mass species composition by the use of multiple parameter measurements. These measurements consist of the energies that individual particles deposit in more than one detector. This information is telemetered both as ion rate data, obtained by on-board species identification circuitry (with various channels representing various energy-species combinations), and as particle multiple parameters data, consisting of pulse-height-analysis values from each of the affected particle detectors for each analyzed particle. (A maximum of about 2 to 5 particles per second can be analyzed in this fashion due to telemetry limitations. A priority scheme avoids saturation by one species group. there are three such groups defined: atomic number z = 1,2 each group in a rotating fashion.) Angular information is obtained through mechanical rotation of the detectors. The main detectors look within a single scan plane that is rotated 360 degrees, stopping at 8 different look sectors (one of the sectors is blocked to obtain a background measurement: sector 8). The lower energy detectors have full width viewcones of about 45 degrees. The scan plane is oriented such that a line that passes exactly between sectors 8 and 1, and also exactly between sectors 4 and 5, is exactly parallel to the roll axis of the spacecraft (which nominally points at earth). When the roll orientation of the spacecraft is such that the star sensor is locked on canopus, the scan plane is tilted about 30 degrees out of the ecliptic plane, with sector 3 tilting towards north ecliptic (and also in the direction that is retrograde with respect to the planetary orbits). Sectors 1 and 8 point in the general direction of earth. The scan rate is variable between 48 seconds to 48 minutes per 360 degree scan. There are some electron detectors (whose properties are not as well established as the others) that view out of the scan plane described here (see Krimigis et al. 1977, Space Science Reviews, 21, p.329). Some of the data is subject to substantial contamination depending on the region under consideration. Before the data from this instrument can be used, it is vital that the contamination descriptions be examined ('CONTAMINATION_ DESC') for each contamination type ('CONTAMINATION_ID') and that the contaminations levels be determined ('DATA_QUALITY_ID' AND 'DATA_QUALITY_DESC'). While sector 8 is the background sector for most (and generally the most used) data channels, sector 4 is the background sector for some channels. Of those channels documented in this catalog, sector 4 is the background sector for channels: ESA0, ESB0, AB10, AB12, AB13, PSA1, PSA2, PSA3, PSB1, PSB2, AND PSB3." SCIENTIFIC_OBJECTIVES_SUMMARY = " Characterize the energy spectra, angular distributions, species composition, spatial structures, and temporal variations of the hot plasmas, energetic particles, and particulate radiation that exist in the vicinity of the outer planets (Jupiter, Saturn, Uranus, and Neptune) and within the interplanetary environment. To study the mechanisms by which such particles are energized and transported throughout such systems. To study in particular the energization and transport processes associated with hot plasmas and particulate radiation in the vicinity of planetary bow shocks, magnetopauses, magnetotail plasma sheets, inner radiation zones, the auroral zones, etc., and to study the interaction of such media with planetary satellites and the planetary atmospheres and ionospheres." INSTRUMENT_CALIBRATION_DESC = " The instrument was calibrated on the ground by placing it into beam chambers (e.g. Van DeGraf machines) and firing calibrated beams of known composition at it. Also, a radioactive source is positioned behind the 'sunshield' positioned at sector 8 for in-flight calibration of some detector- electronic gains. Also, the instrument has a calibration mode whereby pulses of known strength are sent into the pre-amplifier chains following the detectors. Information about calibration can be found in: Krimigis et al., Space Science Reviews, Vol. 21, p 329, 1977 et al., Journal Of Geophysical Research, Vol. 86, p 8227, 1981 Vol. 86, p 8343, 1981 Geophysical Research, Vol. 86, p 8301, 1981." OPERATIONAL_CONSID_DESC = " Instrument operates continuously sampling data over uniform accumulation intervals. The accumulation intervals are different for the different channels of information (almost 100 channels). The scan head of the LECP Instrument usually scans back-and-forth continuously (forward by 315 degrees and then back by 315 degrees). The scanning head pauses at 8 different scan sectors for periods ranging between 6 seconds and 48 seconds (for the encounter time periods) and takes about 0.5 seconds to scan between the sectors. Specially scanning modes for Voyager 2 at Uranus and Neptune have been developed whereby 1 or 2 quick scans are performed followed by 6 to 12 minutes of no scanning. Also, for Voyager 2 at Jupiter there was an extended period of no scanning. The roll orientation of the spacecraft is of crucial importance as to the type of data returned since that orientation determines the orientation of the scan plane of the LECP Instrument. That orientation also has safety consequences since a poor orientation could expose the LECP detectors to ring particulate damage." END_OBJECT = INSTINFO OBJECT = INSTDETECT DETECTOR_ID = "LECP" DETECTOR_TYPE = "SOLID STATE" DETECTOR_ASPECT_RATIO = 0.000000 MINIMUM_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" NOMINAL_OPERATING_TEMPERATURE = 273.000000 DETECTOR_DESC = " The LECP Instrument consists of a variety (about 28) of 'Solid State Detectors' that are used individually and in combinations (using coincidence and anti-coincidence criterion) to detect and characterize nuclear particles. The detector thicknesses range from 2 to 2450 microns to cover a very broad range of particle energy and mass characteristic." SENSITIVITY_DESC = " Detectors count particles that have appropriate discriminated characteristics with an efficiency that approaches 1. Therefore the sensitivity is strickly a function of the geometric factors of the detectors (geometric factors associated with different data channels are documented elsewhere in this catalog) and the energy and species band-widths of the data channels (also documented elsewhere). The geometric factors have units of area X Steradians (CM^2 X STR)." END_OBJECT = INSTDETECT OBJECT = INSTELEC ELECTRONICS_ID = "LECP" ELECTRONICS_DESC = " Timed accumulations of particle counts satisfying various analog pulse-height discrimination levels. Timed accumulations of particle counts satisfying simultaneous analog pulse-height discriminations for multiple detectors. Pulse-height analog-to-digital conversions from multiple, simultaneous detectors for direct telemetry." END_OBJECT = INSTELEC OBJECT = INSTFILTER FILTER_NUMBER = "N/A" FILTER_NAME = "N/A" FILTER_TYPE = "N/A" MINIMUM_WAVELENGTH = "N/A" CENTER_FILTER_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" MEASUREMENT_WAVE_CALBRT_DESC = "N/A" END_OBJECT = INSTFILTER OBJECT = INSTOPTICS TELESCOPE_ID = "N/A" TELESCOPE_FOCAL_LENGTH = "N/A" TELESCOPE_DIAMETER = "N/A" TELESCOPE_F_NUMBER = "N/A" TELESCOPE_RESOLUTION = "N/A" TELESCOPE_TRANSMITTANCE = "N/A" TELESCOPE_T_NUMBER = "N/A" TELESCOPE_T_NUMBER_ERROR = "N/A" TELESCOPE_SERIAL_NUMBER = "N/A" OPTICS_DESC = "N/A" END_OBJECT = INSTOPTICS OBJECT = SCINSTOFFSET PLATFORM_OR_MOUNTING_NAME = "SCIENCE BOOM" CONE_OFFSET_ANGLE = "N/A" CROSS_CONE_OFFSET_ANGLE = "N/A" TWIST_OFFSET_ANGLE = "N/A" INSTRUMENT_MOUNTING_DESC = " LECP Instrument is mounted on the science boom about half way between the boom's spacecraft anchor point and imaging scan platform. The mounting is such that the 360 degree scan plane of the LECP scanning head (not to be confused with the scanning of the imaging instruments) is coplanar with the spacecraft's roll axis. Also, on the canopus star lock the LECP scan plane is about 30 degrees rotated away from the ecliptic plane. A line passing between sectors 1 and 8, and between sectors 4 and 5, is parallel to the spacecraft roll axis. Sectors 1 and 8 point in the general direction or earth, and with the canopus lock, sector 3 points generally in the retrograde direction (referring to the direction with respect to the directions of motion of the orbiting planets) and about 30 degrees north of the ecliptic." END_OBJECT = SCINSTOFFSET OBJECT = INSTSECTION SECTION_ID = "LECP" OBJECT = INSTSECTINFO SCAN_MODE_ID = "UNK" DATA_RATE = 600.000000 SAMPLE_BITS = 10 TOTAL_FOVS = 8 OBJECT = INSTSECTFOVS FOV_SHAPE_NAME = "N/A" HORIZONTAL_PIXEL_FOV = "N/A" VERTICAL_PIXEL_FOV = "N/A" HORIZONTAL_FOV = "N/A" VERTICAL_FOV = "N/A" FOVS = 8 END_OBJECT = INSTSECTFOVS END_OBJECT = INSTSECTINFO OBJECT = INSTSECTPARM INSTRUMENT_PARAMETER_NAME = "ELECTRON RATE" MINIMUM_INSTRUMENT_PARAMETER = 0.000000 MAXIMUM_INSTRUMENT_PARAMETER = 0.000000 NOISE_LEVEL = 0.000000 INSTRUMENT_PARAMETER_UNIT = "COUNTS/SECOND" SAMPLING_PARAMETER_NAME = "ENERGY PER NUCLEON" MINIMUM_SAMPLING_PARAMETER = 0.022000 MAXIMUM_SAMPLING_PARAMETER = 20.000000 SAMPLING_PARAMETER_INTERVAL = 0.000000 SAMPLING_PARAMETER_RESOLUTION = 0.000000 SAMPLING_PARAMETER_UNIT = "MEV PER NUCLEON" END_OBJECT = INSTSECTPARM OBJECT = INSTSECTPARM INSTRUMENT_PARAMETER_NAME = "ELECTRON RATE" MINIMUM_INSTRUMENT_PARAMETER = 0.000000 MAXIMUM_INSTRUMENT_PARAMETER = 0.000000 NOISE_LEVEL = 0.000000 INSTRUMENT_PARAMETER_UNIT = "COUNTS/SECOND" SAMPLING_PARAMETER_NAME = "TIME" MINIMUM_SAMPLING_PARAMETER = 0.000000 MAXIMUM_SAMPLING_PARAMETER = 0.000000 SAMPLING_PARAMETER_INTERVAL = 0.000000 SAMPLING_PARAMETER_RESOLUTION = 0.000000 SAMPLING_PARAMETER_UNIT = "SECOND" END_OBJECT = INSTSECTPARM OBJECT = INSTSECTPARM INSTRUMENT_PARAMETER_NAME = "ION RATE" MINIMUM_INSTRUMENT_PARAMETER = 0.000000 MAXIMUM_INSTRUMENT_PARAMETER = 0.000000 NOISE_LEVEL = 0.000000 INSTRUMENT_PARAMETER_UNIT = "COUNTS/SECOND" SAMPLING_PARAMETER_NAME = "ATOMIC NUMBER" MINIMUM_SAMPLING_PARAMETER = 1.000000 MAXIMUM_SAMPLING_PARAMETER = 26.000000 SAMPLING_PARAMETER_INTERVAL = 0.000000 SAMPLING_PARAMETER_RESOLUTION = 0.000000 SAMPLING_PARAMETER_UNIT = "ATOMIC NUMBER" END_OBJECT = INSTSECTPARM OBJECT = INSTSECTPARM INSTRUMENT_PARAMETER_NAME = "ION RATE" MINIMUM_INSTRUMENT_PARAMETER = 0.000000 MAXIMUM_INSTRUMENT_PARAMETER = 0.000000 NOISE_LEVEL = 0.000000 INSTRUMENT_PARAMETER_UNIT = "COUNTS/SECOND" SAMPLING_PARAMETER_NAME = "ENERGY PER NUCLEON" MINIMUM_SAMPLING_PARAMETER = 0.028000 MAXIMUM_SAMPLING_PARAMETER = 152.000000 SAMPLING_PARAMETER_INTERVAL = 0.000000 SAMPLING_PARAMETER_RESOLUTION = 0.000000 SAMPLING_PARAMETER_UNIT = "MEV PER NUCLEON" END_OBJECT = INSTSECTPARM OBJECT = INSTSECTPARM INSTRUMENT_PARAMETER_NAME = "ION RATE" MINIMUM_INSTRUMENT_PARAMETER = 0.000000 MAXIMUM_INSTRUMENT_PARAMETER = 0.000000 NOISE_LEVEL = 0.000000 INSTRUMENT_PARAMETER_UNIT = "COUNTS/SECOND" SAMPLING_PARAMETER_NAME = "TIME" MINIMUM_SAMPLING_PARAMETER = 0.000000 MAXIMUM_SAMPLING_PARAMETER = 0.000000 SAMPLING_PARAMETER_INTERVAL = 0.000000 SAMPLING_PARAMETER_RESOLUTION = 0.000000 SAMPLING_PARAMETER_UNIT = "SECOND" END_OBJECT = INSTSECTPARM OBJECT = INSTSECTPARM INSTRUMENT_PARAMETER_NAME = "PARTICLE MULTIPLE PARAMETERS" MINIMUM_INSTRUMENT_PARAMETER = 0.000000 MAXIMUM_INSTRUMENT_PARAMETER = 0.000000 NOISE_LEVEL = 0.000000 INSTRUMENT_PARAMETER_UNIT = "MEV X MEV" SAMPLING_PARAMETER_NAME = "ATOMIC NUMBER" MINIMUM_SAMPLING_PARAMETER = 1.000000 MAXIMUM_SAMPLING_PARAMETER = 26.000000 SAMPLING_PARAMETER_INTERVAL = 0.000000 SAMPLING_PARAMETER_RESOLUTION = 0.000000 SAMPLING_PARAMETER_UNIT = "ATOMIC NUMBER" END_OBJECT = INSTSECTPARM OBJECT = INSTSECTDET DETECTOR_ID = "LECP" END_OBJECT = INSTSECTDET OBJECT = INSTSECTELEC ELECTRONICS_ID = "LECP" END_OBJECT = INSTSECTELEC OBJECT = INSTSECTFILT FILTER_NUMBER = "N/A" END_OBJECT = INSTSECTFILT OBJECT = INSTSECTOPTC TELESCOPE_ID = "N/A" END_OBJECT = INSTSECTOPTC END_OBJECT = INSTSECTION OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "FAR ENCOUNTER" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "UNK" INSTRUMENT_POWER_CONSUMPTION = 4.725000 INSTRUMENT_MODE_DESC = " Used in the vicinity of planetary encounters. High intensity detectors turned off (A, B, DELTA, DELTA PRIME). (Affected channels are documented in detailed level catalog.) Bit Rate allocated 1/3 for Particle Multiple Parameters (PMP) data, also called Pulse Height Analysis data, and 2/3 for Rate data (counts/second). Full composition discrimination capabilities enabled (in both Rate and PMP forms). Angular scanning is typically 6.4 minutes per 360 degree scan but is often changed. Scanning cyclics driven by the spacecraft computer are included. Experiment Bit Rate is 600 bits per second. Electrons measured up to 0.5 MEV. minimum sample time is 0.4 sec." OBJECT = INSTMODESECT SECTION_ID = "LECP" END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "FAR ENCOUNTER STOW" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "UNK" INSTRUMENT_POWER_CONSUMPTION = 4.725000 INSTRUMENT_MODE_DESC = " This mode includes the Full Far Encounter Mode configuration with the exception that the angular scanning is halted so that the detectors are fixed looking into a non-standard direction. This direction is such that the detectors peek around a sun screen (which covers the sector 8 positon of the scan plane) having the effect of protecting the low energy ion and electron detectors by reducing their geometric factors. For the one application of this mode the geometric factor was reduced by a factor of 26 for the low energy ions (Alpha detector) and by an as yet uncalibrated factor for the electrons (Beta and Gamma detectors)." OBJECT = INSTMODESECT SECTION_ID = "LECP" END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "NEAR ENCOUNTER" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "UNK" INSTRUMENT_POWER_CONSUMPTION = 4.525000 INSTRUMENT_MODE_DESC = " Sometimes used at the closest-in positions during a planetary encounter. The high intensity detectors are turned on (A, B, DELTA, DELTA PRIME). (Affected channels are documented in the detailed level catalog.) Particle Multiple Parameter (PMP) composition discrimination capabilities are turned off (including the rate channels derived from the multiple parameter information). All data appears in rate (counts/second) form. Angular scanning is typically 6.4 minutes per 360 degrees scan but is often changed. Scanning cyclics driven by the spacecraft computer are included. Experiment Bit Rate is 600 bits per second. Electrons are measured up to greater than 10 MEV. Minimum sample time is 0.4 sec." OBJECT = INSTMODESECT SECTION_ID = "LECP" END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "URANUS SCAN CYCLIC" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "UNK" INSTRUMENT_POWER_CONSUMPTION = 4.725000 INSTRUMENT_MODE_DESC = " Data accumulated as with the Far Encounter Mode. Angular scanning controlled by spacecraft. Two quick full angular scans are obtained using 6 second scanning and lasting for 96 seconds total. In between these scan periods the sensors are held fixed looking in sector 7. The scan periods occur every 12 minutes." OBJECT = INSTMODESECT SECTION_ID = "LECP" END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "KRIMIGISETAL1977" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "LECP DOCUMENTATION" JOURNAL_NAME = "SPACE SCIENCE REVIEWS" PUBLICATION_DATE = 1977 REFERENCE_DESC = " Krimigis, S. M., T. P. Armstrong, W.I. Axford, C. O. Bostrom, C. Y. Fan, G. Gloeckler, and L. J. Lanzerotti, The Low Energy Charged Particle (LECP) Experiment On The Voyager Spacecraft, Space Science Reviews, 21, 329 1977." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. S. M. KRIMIGIS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "KRIMIGISETAL1981" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "LECP JUPITER DOCUMENTATION" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1981 REFERENCE_DESC = " Krimigis, S. M., J. F. Carbury, E. P. Keath, C. O. Bostrom, W. I. Axford, G. Gloeckler, L. J. Lanzerotti, and T. P. Armstrong, Characteristics Of Hot Plasma In The Jovian Magnetosphere: Results From The Voyager Spacecraft, Journal Of Geophysical Research, 86, 8227, 1981." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. S. M. KRIMIGIS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO END_OBJECT = SCINSTRUMENT /*************************** MAG Instrument **********************************/ /* MODIFICATIONS */ /* 920813 -- EFRIED */ /* Inserted values for INSTOPTICS, INSTRUMENT_MODE_DESC, */ /* REFERENCE_DESC, and AUTHOR_FULL_NAME */ /* 920916 -- EFRIED */ /* last changes made */ /* Template: Spacecraft Instrument Template - Rev: 19890121 */ /* Note: The following templates form part of a standard */ /* set for the submission of a spacecraft instrument */ /* to the PDS. */ /* Hierarchy: SCINSTRUMENT */ /* INSTINFO */ /* INSTDETECT */ /* INSTELEC */ /* INSTFILTER */ /* INSTOPTICS */ /* SCINSTOFFSET */ /* INSTSECTION */ /* INSTSECTINFO */ /* INSTSECTFOVS */ /* INSTSECTPARM */ /* INSTSECTDET */ /* INSTSECTELEC */ /* INSTSECTFILT */ /* INSTSECTOPTC */ /* INSTMODEINFO */ /* INSTMODESECT */ /* INSTREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCINSTRUMENT SPACECRAFT_ID = "VG2" INSTRUMENT_ID = "MAG" OBJECT = INSTINFO INSTRUMENT_NAME = "TRIAXIAL FLUXGATE MAGNETOMETER" INSTRUMENT_TYPE = "MAGNETOMETER" PI_PDS_USER_ID = "NNESS" NAIF_DATA_SET_ID = "N/A" BUILD_DATE = 1977-08-20 INSTRUMENT_MASS = 5.600000 INSTRUMENT_HEIGHT = "UNK" INSTRUMENT_LENGTH = 13.000000 INSTRUMENT_WIDTH = "UNK" INSTRUMENT_MANUFACTURER_NAME = "UNK" INSTRUMENT_SERIAL_NUMBER = "UNK" INSTRUMENT_DESC = " The magnetic field experiment carried out on the Voyager 2 mission consists of dual low field (LFM) and high field magnetometer (HFM) systems. The dual systems provide greater reliability and, in the case of the LFM's, permit the separation of the spacecraft magnetic fields from the ambient fields. Additional reliability is achieved through electronics redundancy. The wide dynamic ranges of +/- 0.002 G for the LFM's and +/- 20G for the HFM's, low quantization uncertainty (+/- 12.4, 488 nanotesla respectively), low sensor RMS noise level (0.006 nanotesla), and the use of data compaction schemes to optimize the experiment information rate all combine to permit the study of a broad spectrum of phenomena during the mission." SCIENTIFIC_OBJECTIVES_SUMMARY = " The investigations of the magnetic fields and magnetospheres of the major planetary systems in the outer Solar System and their interactions with the solar wind are primary objectives of the space exploration program to be conducted during the Voyager 2 mission. In addition, the investigation of the interplanetary magnetic field phenomena during the flights is of fundamental importance both to the understanding of the magnetospheric observations and to a number of outstanding questions in basic plasma physics and in the general dynamics of the solar wind. If the Heliospheric boundary is penetrated, accurate measurement of the interstellar magnetic field is also an important objective." INSTRUMENT_CALIBRATION_DESC = " The 13 meter Astromast booms have proved in extensive pre-flight testing to be highly rigid with respect to bending motions but soft to torsional or twisting motion. Deployment repeatability tests have shown as much as +/- 7 degrees uncertainty in the knowledge of the boom twist angle (about the boom axis) at the magnetometer sensor positions, compared with +/- 0.5 uncertainty in bend angles (rotation about axes orthogonal to the boom axis). In order to minimize sensor alignment uncertainties, a method to estimate an angular correction matrix was developed that eliminates most of the twist uncertainty and some of the bend uncertainty. A special calibration coil has been wound around the periphery of the spacecrafts high gain antenna to generate, upon command, a known magnetic field at both LFM magnetometer sensors. The difference between measurements taken when the coil is turned on and off is the coil field, independent of all external fields. Using a 20 turn coil of 1/2 amp yields nominal field intensities 0f 33.4 and 6.1 nanotesla at the inboard and outboard sensors, respectively. All magnetometer data are calibrated. Three types of in-flight calibrations are performed: 1) sensitivity calibrations, 2) zero-level calibrations, based on rolls of the spacecraft, and 3) boom-alignment calibrations based on the activation of on-board coils and resulting data (especially important when dual magnetometers are used and in strong fields for any magnetometer). Sensitivity calibrations (for 8 ranges) are done approximately once every two months (early in the mission they were done more frequently). The magnetometer team generally use one or two axis rolls (cruise maneuvers, CRSMR's) of the spacecraft for zero level calibrations as often as they are provided which is variable this is about three times per year for the so-called mini-CRSMR's, which are two axis rolls. Full CRSMR's and z-axis (only) roll-maneuvers have not occurred within the last few years (full CRSMR's and mini's differ only in the number of rolls in each). The magnetometer team usually succeeds in arguing for a series of rolls near each planetary encounter. Boom-alignment calibrations were done once after launch and around the time of the Jupiter encounter. Others have been executed, but it has been determined that the inter-sensor misalignment is small and constant. For more information, consult Behannon et al, Space Science Reviews, 1977 volume 21 pages 235-257." OPERATIONAL_CONSID_DESC = " There are no special operational considerations for the magnetometer described in Behannon et al, Space Science Reviews, 21 (1977). All magnetometer data are calibrated. Three types of in-flight calibrations are performed: 1) sensitivity calibrations, 2) zero-level calibrations, based on rolls of the spacecraft, and 3) boom-alignment calibrations based on the activation of on-board coils and resulting data (especially important when dual magnetometers are used and in strong fields for any magnetometer). Sensitivity calibrations (for 8 ranges) are done approximately once every two months (early in the mission they were done more frequently). The magnetometer team generally use one or two axis rolls (cruise maneuvers, CRSMR's) of the spacecraft for zero level calibrations as often as they are provided which is variable this is about three times per year for the so-called mini-CRSMR's, which are two axis rolls. Full CRSMR's and z-axis (only) roll-maneuvers have not occurred within the last few years (full CRSMR's and mini's differ only in the number of rolls in each). The magnetometer team usually succeeds in arguing for a series of rolls near each planetary encounter. Boom-alignment calibrations were done once after launch and around the time of the Jupiter encounter. Others have been executed, but it has been determined that the inter-sensor misalignment is small and constant." END_OBJECT = INSTINFO OBJECT = INSTDETECT DETECTOR_ID = "HFM1" DETECTOR_TYPE = "RING CORE" DETECTOR_ASPECT_RATIO = 0.000000 MINIMUM_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" NOMINAL_OPERATING_TEMPERATURE = 273.000000 DETECTOR_DESC = " Both high and low field magnetometer sensors utilize a ring core geometry and thus have lower drive power requirements and better zero level stability than other types of fluxgates and are smaller in size (Acuna, 1974). The cores consist of an advanced molybdenum alloy, especially developed in cooperation with the Naval Surface Weapons Center, White Oak, Maryland, which exhibits extremely low noise and high stability characteristics. The use of this alloy and the ring core sensor geometry thus allows the realization of compact, low power, ultrastable fluxgate sensors with a noise performance that is improved almost an order of magnitude over the best previously flown fluxgate sensors. The HFM's use specially processed miniature ring cores (1cm diameter) which minimize the power required to measure large fields. This description is taken directly from Behannon et al, Space Science Reviews (1977). The HFM1 detector is designated as the detector which measures the i component of the vector (i, j, k)." SENSITIVITY_DESC ="N/A" END_OBJECT = INSTDETECT OBJECT = INSTDETECT DETECTOR_ID = "HFM2" DETECTOR_TYPE = "RING CORE" DETECTOR_ASPECT_RATIO = 0.000000 MINIMUM_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" NOMINAL_OPERATING_TEMPERATURE = 273.000000 DETECTOR_DESC = " Both high and low field magnetometer sensors utilize a ring core geometry and thus have lower drive power requirements and better zero level stability than other types of fluxgates and are smaller in size (Acuna, 1974). The cores consist of an advanced molybdenum alloy, especially developed in cooperation with the Naval Surface Weapons Center, White Oak, Maryland, which exhibits extremely low noise and high stability characteristics. The use of this alloy and the ring core sensor geometry thus allows the realization of compact, low power, ultrastable fluxgate sensors with a noise performance that is improved almost an order of magnitude over the best previously flown fluxgate sensors. The HFM's use specially processed miniature ring cores (1cm diameter) which minimize the power required to measure large fields. This description is taken directly from Behannon et al, Space Science Reviews (1977). The HFM2 detector is designated as the detector which measures the j component of the vector (i,j,k)." SENSITIVITY_DESC = "N/A" END_OBJECT = INSTDETECT OBJECT = INSTDETECT DETECTOR_ID = "HFM3" DETECTOR_TYPE = "RING CORE" DETECTOR_ASPECT_RATIO = 0.000000 MINIMUM_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" NOMINAL_OPERATING_TEMPERATURE = 273.000000 DETECTOR_DESC = " Both high and low field magnetometer sensors utilize a ring core geometry and thus have lower drive power requirements and better zero level stability than other types of fluxgates and are smaller in size (Acuna, 1974). The cores consist of an advanced molybdenum alloy, especially developed in cooperation with the Naval Surface Weapons Center, White Oak, Maryland, which exhibits extremely low noise and high stability characteristics. The use of this alloy and the ring core sensor geometry thus allows the realization of compact, low power, ultrastable fluxgate sensors with a noise performance that is improved almost an order of magnitude over the best previously flown fluxgate sensors. The HFM's use specially processed miniature ring cores (1cm diameter) which minimize the power required to measure large fields. This description is taken directly from Behannon et al, Space Science Reviews (1977). The HFM3 detector is designated as the detector which measures the k component of the vector (i,j,k)." SENSITIVITY_DESC = "N/A" END_OBJECT = INSTDETECT OBJECT = INSTDETECT DETECTOR_ID = "LFM1" DETECTOR_TYPE = "RING CORE" DETECTOR_ASPECT_RATIO = 0.000000 MINIMUM_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" NOMINAL_OPERATING_TEMPERATURE = 273.000000 DETECTOR_DESC = " Both high and low field magnetometer sensors utilize a ring core geometry and thus have lower drive power requirements and better zero level stability than other types of fluxgates and are smaller in size (Acuna, 1974). The cores consist of an advanced molybdenum alloy, especially developed in cooperation with the Naval Surface Weapons Center, White Oak, Maryland, which exhibits extremely low noise and high stability characteristics. The use of this alloy and the ring core sensor geometry thus allows the realization of compact, low power, ultrastable fluxgate sensors with a noise performance that is improved almost an order of magnitude over the best previously flown fluxgate sensors. The HFM's use specially processed miniature ring cores (1cm diameter) which minimize the power required to measure large fields. This description is taken directly from Behannon et al, Space Science Reviews (1977). The LFM1 detector is designated as the detector which measures the i component of the vector (i,j,k)." SENSITIVITY_DESC = "N/A" END_OBJECT = INSTDETECT OBJECT = INSTDETECT DETECTOR_ID = "LFM2" DETECTOR_TYPE = "RING CORE" DETECTOR_ASPECT_RATIO = 0.000000 MINIMUM_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" NOMINAL_OPERATING_TEMPERATURE = 273.000000 DETECTOR_DESC = " Both high and low field magnetometer sensors utilize a ring core geometry and thus have lower drive power requirements and better zero level stability than other types of fluxgates and are smaller in size (Acuna, 1974). The cores consist of an advanced molybdenum alloy, especially developed in cooperation with the Naval Surface Weapons Center, White Oak, Maryland, which exhibits extremely low noise and high stability characteristics. The use of this alloy and the ring core sensor geometry thus allows the realization of compact, low power, ultrastable fluxgate sensors with a noise performance that is improved almost an order of magnitude over the best previously flown fluxgate sensors. The HFM's use specially processed miniature ring cores (1cm diameter) which minimize the power required to measure large fields. This description is taken directly from Behannon et al, Space Science Reviews (1977). The LFM2 detector is designated as the detector which measures the j component of the vector (i,j,k)." SENSITIVITY_DESC = "N/A" END_OBJECT = INSTDETECT OBJECT = INSTDETECT DETECTOR_ID = "LFM3" DETECTOR_TYPE = "RING CORE" DETECTOR_ASPECT_RATIO = 0.000000 MINIMUM_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" NOMINAL_OPERATING_TEMPERATURE = 273.000000 DETECTOR_DESC = " Both high and low field magnetometer sensors utilize a ring core geometry and thus have lower drive power requirements and better zero level stability than other types of fluxgates and are smaller in size (Acuna, 1974). The cores consist of an advanced molybdenum alloy, especially developed in cooperation with the Naval Surface Weapons Center, White Oak, Maryland, which exhibits extremely low noise and high stability characteristics. The use of this alloy and the ring core sensor geometry thus allows the realization of compact, low power, ultrastable fluxgate sensors with a noise performance that is improved almost an order of magnitude over the best previously flown fluxgate sensors. The HFM's use specially processed miniature ring cores (1cm diameter) which minimize the power required to measure large fields. This description is taken directly from Behannon et al, Space Science Reviews (1977). The LFM3 detector is designated as the detector which measures the k component of the vector (i,j,k)." SENSITIVITY_DESC = "N/A" END_OBJECT = INSTDETECT OBJECT = INSTELEC ELECTRONICS_ID = "P" ELECTRONICS_DESC = " P - primary system. The experiment electronics instrumentation consists of the flux-gate magnetometer electronics and associated controls, and the calibration and data processing electronics. Complete redundancy is provided for the analog to digital converters, data and status readout buffers, command decoders and power converters. Thus not only can the two magnetometers of a system be interchanged, but considerable cross-strapping within the electronics permits interchange of critical internal functions as well. This significantly reduces the impact of single-component failure on the ability of the experiment to continue successful operation during the mission duration of > 4 years. This description is directly transposed from Behannon et al, Space Science Reviews, 21 (1977) page 249." END_OBJECT = INSTELEC OBJECT = INSTELEC ELECTRONICS_ID = "S" ELECTRONICS_DESC = " S - secondary system. The experiment electronics instrumentation consists of the flux-gate magnetometer electronics and associated controls, and the calibration and data processing electronics. Complete redundancy is provided for the analog to digital converters, data and status readout buffers, command decoders and power converters. Thus not only can the two magnetometers of a system be interchanged, but considerable cross-strapping within the electronics permits interchange of critical internal functions as well. This significantly reduces the impact of single-component failure on the ability of the experiment to continue successful operation during the mission duration of > 4 years. This description is directly transposed from Behannon et al, Space Science Reviews, 21 (1977) page 249." END_OBJECT = INSTELEC OBJECT = INSTFILTER FILTER_NUMBER = "N/A" FILTER_NAME = "N/A" FILTER_TYPE = "N/A" MINIMUM_WAVELENGTH = "N/A" CENTER_FILTER_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" MEASUREMENT_WAVE_CALBRT_DESC = "N/A" END_OBJECT = INSTFILTER OBJECT = INSTOPTICS TELESCOPE_ID = "N/A" TELESCOPE_FOCAL_LENGTH = "N/A" TELESCOPE_DIAMETER = "N/A" TELESCOPE_F_NUMBER = "N/A" TELESCOPE_RESOLUTION = "N/A" TELESCOPE_TRANSMITTANCE = "N/A" TELESCOPE_T_NUMBER = "N/A" TELESCOPE_T_NUMBER_ERROR = "N/A" TELESCOPE_SERIAL_NUMBER = "N/A" OPTICS_DESC = "N/A" END_OBJECT = INSTOPTICS OBJECT = SCINSTOFFSET PLATFORM_OR_MOUNTING_NAME = "MAGNETOMETER BOOM" CONE_OFFSET_ANGLE = "N/A" CROSS_CONE_OFFSET_ANGLE = "N/A" TWIST_OFFSET_ANGLE = "N/A" INSTRUMENT_MOUNTING_DESC = " The LFM is located near the tip of the boom and the HFM is located near the spacecraft body. See Behannon et al, 1977 for a picture of the actual magnetometer mounting positions and a complete description." END_OBJECT = SCINSTOFFSET OBJECT = INSTSECTION SECTION_ID = "HFM" OBJECT = INSTSECTINFO SCAN_MODE_ID = "N/A" DATA_RATE = "UNK" SAMPLE_BITS = 12 TOTAL_FOVS = 1 OBJECT = INSTSECTFOVS FOV_SHAPE_NAME = "N/A" HORIZONTAL_PIXEL_FOV = "N/A" VERTICAL_PIXEL_FOV = "N/A" HORIZONTAL_FOV = "N/A" VERTICAL_FOV = "N/A" FOVS = 1 END_OBJECT = INSTSECTFOVS END_OBJECT = INSTSECTINFO OBJECT = INSTSECTPARM INSTRUMENT_PARAMETER_NAME = "MAGNETIC FIELD COMPONENT" MINIMUM_INSTRUMENT_PARAMETER = -2000000.000000 MAXIMUM_INSTRUMENT_PARAMETER = 2000000.000000 NOISE_LEVEL = 0.006000 INSTRUMENT_PARAMETER_UNIT = "NANOTESLA" SAMPLING_PARAMETER_NAME = "TIME" MINIMUM_SAMPLING_PARAMETER = 0.600000 MAXIMUM_SAMPLING_PARAMETER = 0.600000 SAMPLING_PARAMETER_INTERVAL = 0.600000 SAMPLING_PARAMETER_RESOLUTION = 0.600000 SAMPLING_PARAMETER_UNIT = "SECOND" END_OBJECT = INSTSECTPARM OBJECT = INSTSECTDET DETECTOR_ID = "HFM1" END_OBJECT = INSTSECTDET OBJECT = INSTSECTDET DETECTOR_ID = "HFM2" END_OBJECT = INSTSECTDET OBJECT = INSTSECTDET DETECTOR_ID = "HFM3" END_OBJECT = INSTSECTDET OBJECT = INSTSECTELEC ELECTRONICS_ID = "P" END_OBJECT = INSTSECTELEC OBJECT = INSTSECTELEC ELECTRONICS_ID = "S" END_OBJECT = INSTSECTELEC OBJECT = INSTSECTFILT FILTER_NUMBER = "HFM1" END_OBJECT = INSTSECTFILT OBJECT = INSTSECTOPTC TELESCOPE_ID = "N/A" END_OBJECT = INSTSECTOPTC END_OBJECT = INSTSECTION OBJECT = INSTSECTION SECTION_ID = "LFM" OBJECT = INSTSECTINFO SCAN_MODE_ID = "N/A" DATA_RATE = "UNK" SAMPLE_BITS = 12 TOTAL_FOVS = 1 OBJECT = INSTSECTFOVS FOV_SHAPE_NAME = "N/A" HORIZONTAL_PIXEL_FOV = "N/A" VERTICAL_PIXEL_FOV = "N/A" HORIZONTAL_FOV = "N/A" VERTICAL_FOV = "N/A" FOVS = 1 END_OBJECT = INSTSECTFOVS END_OBJECT = INSTSECTINFO OBJECT = INSTSECTPARM INSTRUMENT_PARAMETER_NAME = "MAGNETIC FIELD COMPONENT" MINIMUM_INSTRUMENT_PARAMETER = -50000.000000 MAXIMUM_INSTRUMENT_PARAMETER = 50000.000000 NOISE_LEVEL = 0.006000 INSTRUMENT_PARAMETER_UNIT = "NANOTESLA" SAMPLING_PARAMETER_NAME = "TIME" MINIMUM_SAMPLING_PARAMETER = 0.060000 MAXIMUM_SAMPLING_PARAMETER = 0.060000 SAMPLING_PARAMETER_INTERVAL = 0.060000 SAMPLING_PARAMETER_RESOLUTION = 0.060000 SAMPLING_PARAMETER_UNIT = "SECOND" END_OBJECT = INSTSECTPARM OBJECT = INSTSECTDET DETECTOR_ID = "LFM1" END_OBJECT = INSTSECTDET OBJECT = INSTSECTDET DETECTOR_ID = "LFM2" END_OBJECT = INSTSECTDET OBJECT = INSTSECTDET DETECTOR_ID = "LFM3" END_OBJECT = INSTSECTDET OBJECT = INSTSECTELEC ELECTRONICS_ID = "P" END_OBJECT = INSTSECTELEC OBJECT = INSTSECTELEC ELECTRONICS_ID = "S" END_OBJECT = INSTSECTELEC OBJECT = INSTSECTFILT FILTER_NUMBER = "LFM1" END_OBJECT = INSTSECTFILT OBJECT = INSTSECTOPTC TELESCOPE_ID = "N/A" END_OBJECT = INSTSECTOPTC END_OBJECT = INSTSECTION OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "CRUISE" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "REALTIME" INSTRUMENT_POWER_CONSUMPTION = 2.200000 INSTRUMENT_MODE_DESC = " In the CRUISE mode, only the LFM subsystem is operating. The basic sample rate in this mode is 50/3 vectors/second." OBJECT = INSTMODESECT SECTION_ID = "LFM" END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "ENCOUNTER" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "REALTIME" INSTRUMENT_POWER_CONSUMPTION = 2.200000 INSTRUMENT_MODE_DESC = " In the ENCOUNTER mode, both LFM and HFM subsystems are operating. The basic sample rate in this mode is 50/3 vectors/second for the LFM system and 5/3 vectors/second for the HFM system." OBJECT = INSTMODESECT SECTION_ID = "HFM" END_OBJECT = INSTMODESECT OBJECT = INSTMODESECT SECTION_ID = "LFM" END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "ACUNAETAL1983" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "Z3 ZONAL HARMONIC MODEL SATURN'S MAGNETIC FIELD ANALYSIS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1983 REFERENCE_DESC = " Acuna, M. H., J. E. P. Connerney, and N. F. Ness, The Z3 Zonal Harmonic Model of Saturn's Magnetic Field: Analysis and Implications, J. Geophys. Res., 88, 8771, 1983." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "J.E.P. CONNERNEY" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "BEHANNONETAL1977" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD EXPERIMENT FOR VOYAGER 1 AND 2" JOURNAL_NAME = "SPACE SCIENCE REVIEWS" PUBLICATION_DATE = 1977 REFERENCE_DESC = " Behannon K. W., M. H. Acuna, L. F. Burlaga, R. P. Lepping, N. F. Ness, and F. M. Neubauer, Magnetic Field Experiment for Voyagers 1 and 2, Space Science Reviews, 21, 235, 1977." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "F.M. NEUBAUER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.F. BURLAGA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R.P. LEPPING" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "BEHANNONETAL1981" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "JOVIAN MAGNETOTAIL AND CURRENT SHEET" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1981 REFERENCE_DESC = " Behannon, K. W., L. F. Burlaga, and N. F. Ness, The Jovian Magnetotail and its Current Sheet, J. Geophys. Res., 86, 8385, 1981." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.F. BURLAGA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "BEHANNONETAL1983" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "STRUCTURE DYNAMICS SATURN'S OUTER MAGNETOSPHERE BOUNDARY" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1983 REFERENCE_DESC = " Behannon, K. W., R. P. Lepping, and N. F. Ness, Structure and Dynamics of Saturn's Outer Magnetosphere and Boundary Regions, J. Geophys. Res., 88, 8791, 1983." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R.P. LEPPING" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "BEHANNONETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETOTAIL URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Behannon, K. W., et al, The Magnetotail of Uranus, J. Geophys. Res., 92, 366, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "CONNERNEYETAL1981" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MODELING JOVIAN CURRENT SHEET AND INNER MAGNETOSPHERE" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1981 REFERENCE_DESC = " Connerney, J. E. P., M. H. Acuna, and N. F. Ness, Modeling of the Jovian Current Sheet and Inner Magnetosphere, J. Geophys Res., 86, 8370, 1981." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "J.E.P. CONNERNEY" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "CONNERNEYETAL1983" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "CURRENTS IN SATURN'S MAGNETOSPHERE" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1983 REFERENCE_DESC = " Connerney, J. E. P., M. H. Acuna, and N. F. Ness, Currents in Saturn's Magnetosphere, J. Geophys. Res., 88, 8779, 1983." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "J.E.P. CONNERNEY" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "CONNERNEYETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Connerney, J. E. P., M. H. Acuna, and N. F. Ness, The Magnetic Field of Uranus, J. Geophys. Res., 92, 336, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "J.E.P. CONNERNEY" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "DESCH&KAISER1981" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "VOYAGER MEASUREMENT ROTATION PERIOD SATURN MAGNETIC FIELD" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH LETTERS" PUBLICATION_DATE = 1981 REFERENCE_DESC = " Desch, M.D., and M.L. Kaiser, Voyager Measurement of the Rotation Period of Saturn's Magnetic Field, J. Geophys. Res. Letters, 8, 253, 1981." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.D. DESCH" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.L. KAISER" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "DESSLER1983" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "PHYSICS OF JOVIAN MAGNETOSPHERE COORDINATE SYSTEMS" JOURNAL_NAME = "PHYSICS OF THE JOVIAN MAGNETOSPHERE" PUBLICATION_DATE = 1983 REFERENCE_DESC = " Dessler, A. J. ed., Physics of the Jovian Magnetosphere, Cambridge University Press, London, Appendix B - Coordinate Systems, Dessler, A. J., 1983." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "A.J. DESSLER" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "LEPPINGETAL1981" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD AND PLASMA FLOW IN JUPITER MAGNETOSHEATH" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1981 REFERENCE_DESC = " Lepping R. P., et al, Observations of the Magnetic Field and Plasma Flow in the Jupiter Magnetosheath, J. Geophys. Res., 86, 8145 1981." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R.P. LEPPING" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "LEPPINGETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "SURFACE WAVES URANUS MAGNETOPAUSE" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Lepping, R. P., L. F. Burlaga, and L. W. Klein, Surface Waves on Uranus' Magnetopause, J. Geophys, Res., 92, 353, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.F. BURLAGA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.W. KLIEN" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R.P. LEPPING" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "NESSETAL1979A" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD STUDIES AT JUPITER BY VOYAGER 2" JOURNAL_NAME = "SCIENCE" PUBLICATION_DATE = 1979 REFERENCE_DESC = " Ness, N. F., et al, Magnetic Field Studies at Jupiter by Voyager 2: Preliminary Results, Science, 206, 966, 1979." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "NESSETAL1983" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD STUDIES VOYAGER 2 SATURN PRELIMINARY" JOURNAL_NAME = "SCIENCE" PUBLICATION_DATE = 1983 REFERENCE_DESC = " Ness, N. F., et al, Magnetic Fields at Uranus, Science, 233, 85, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "NESSETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD STUDIES URANUS" JOURNAL_NAME = "SCIENCE" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Ness, N. F., et al, Magnetic Fields at Uranus, Science, 233, 85, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "VOIGTETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD CURRENT STRUCTURES MAGNETOSPHERE URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Voigt, G. H., K. W. Behannon, and N. F. Ness, Magnetic Field and Current Structures in the Magnetosphere of Uranus, J. Geophys. Res., 92, 346, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "G.H. VOIGT" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO END_OBJECT = SCINSTRUMENT /**************** PLS Instrument Template*************************************/ /* Modifications */ /* 920811 -- EFRIED */ /* Minor adjustments and changed capitalized descriptions */ /* to normal form(UC -> LC). */ /* 920813 -- EFRIED */ /* Inserted values for INSTOPTICS, INSTRUMENT_MODE_DESC(UC -> LC),*/ /* REFERENCE_DESC(UC -> LC), and AUTHOR_FULL_NAME. */ /* 920916 -- EFRIED */ /* last changes made */ /* Template: Spacecraft Instrument Template - Rev: 19890121 */ /* Note: The following templates form part of a standard */ /* set for the submission of a spacecraft instrument */ /* to the PDS. */ /* Hierarchy: SCINSTRUMENT */ /* INSTINFO */ /* INSTDETECT */ /* INSTELEC */ /* INSTFILTER */ /* INSTOPTICS */ /* SCINSTOFFSET */ /* INSTSECTION */ /* INSTSECTINFO */ /* INSTSECTFOVS */ /* INSTSECTPARM */ /* INSTSECTDET */ /* INSTSECTELEC */ /* INSTSECTFILT */ /* INSTSECTOPTC */ /* INSTMODEINFO */ /* INSTMODESECT */ /* INSTREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCINSTRUMENT SPACECRAFT_ID = 'VG2' INSTRUMENT_ID = 'PLS' OBJECT = INSTINFO INSTRUMENT_NAME = "PLASMA SCIENCE EXPERIMENT" INSTRUMENT_TYPE = "PLASMA INSTRUMENT" PI_PDS_USER_ID = 'JBELCHER' NAIF_DATA_SET_ID = 'N/A' BUILD_DATE = 1973 INSTRUMENT_MASS = 9.900000 INSTRUMENT_HEIGHT = 'UNK' INSTRUMENT_LENGTH = 'UNK' INSTRUMENT_WIDTH = 'UNK' INSTRUMENT_MANUFACTURER_NAME = "MASSACHUSETTS INSTITUTE OF TECHNOLOGY" INSTRUMENT_SERIAL_NUMBER = 'SN001' INSTRUMENT_DESC = " The Voyager Plasma Science experiment consists of four modulated grid Faraday Cups, three (A,B,C) of which are positioned about the Telemetry Antenna Axis and generally point toward the Earth with the fourth (D) at a right angle to this direction. Ion currents are sampled simultaneously in all four cups, electrons in the D-cup only. The instrument has an energy/charge range of 10-5950 V. Data is taken in four ways, high and low resolution ion modes and high and low energy electron modes, with energy resolution varying between 3.6 and 29%. The integration time for each energy channel can be varied are used at Jupiter and Saturn and 0.93 and 0.21 second integration times are used at Uranus and Neptune. Supersonic flow can be observed only when one of the detectors points into the flow orientation allows determination of the plasma density, temperature, and velocity." SCIENTIFIC_OBJECTIVES_SUMMARY = " The objective of the Plasma Instrument is to characterize plasma conditions throughout the Voyager trajectory, in the solar wind and during the planetary encounters." INSTRUMENT_CALIBRATION_DESC = " The instrument was calibrated at MIT using ion and electron beams and compared to output from other Faraday Cups in the same beam. Current levels are also calibrated in-flight by injecting known currents into the detectors with the modulators on and off. Much theoretical modeling has been done on the response of the detectors to arbitrary plasma conditions. Contact the PI for more information." OPERATIONAL_CONSID_DESC = " Each detector has an effective field of view which is a cone of half angle 45 degrees falls off quickly at higher angles. Thus, for the instrument to measure ion parameters in a Supersonic or Transonic plasma some of the detectors must look into the plasma flow. Secondary ions and electrons produced within the detectors can also effect the measurements, especially if large fluxes of hot ions or electrons are present and these effects are not well modeled. The instrument does not measure composition, only energy/charge, so a model of plasma composition must be adopted to fit the ion data choice of models can be unambiguous for large Mach number flow (M>3) but is non-unique for lower Mach numbers. After the Jupiter encounter the highest channels of the A, B, and C detectors often contain spurious signal and currents in the upper half of the energy range should be examined carefully before use." END_OBJECT = INSTINFO OBJECT = INSTDETECT DETECTOR_ID = 'A' DETECTOR_TYPE = "FARADAY CUP" DETECTOR_ASPECT_RATIO = 0.000000 MINIMUM_WAVELENGTH = 'N/A' MAXIMUM_WAVELENGTH = 'N/A' NOMINAL_OPERATING_TEMPERATURE = 278.000000 DETECTOR_DESC = " This detector is a Faraday Cup which is part of a cluster of three detectors (A, B, C) arranged in a cone whose central axis is parallel to the direction of the telemetry antenna. The look direction of the cup is offset 20 degrees from the central axis. It consists of three modulator grids, six shield grids and a suppressor grid in front of the collector. It measures ion currents in the range 10-5950 V." SENSITIVITY_DESC = " Depending on the integration time the detector measures current from a minimum of 3.E-14 to 2.E-13 AMPS up to a maximum of 6.E-8 AMPS." END_OBJECT = INSTDETECT OBJECT = INSTDETECT DETECTOR_ID = 'B' DETECTOR_TYPE = "FARADAY CUP" DETECTOR_ASPECT_RATIO = 0.000000 MINIMUM_WAVELENGTH = 'N/A' MAXIMUM_WAVELENGTH = 'N/A' NOMINAL_OPERATING_TEMPERATURE = 278.000000 DETECTOR_DESC = " This detector is a Faraday Cup which is part of a cluster of three detectors (A, B, C) arranged in a cone whose central axis is parallel to the direction of the telemetry antenna. The look direction of the cup is offset 20 degrees from the central axis. It consists of three modulator grids, six shield grids and a suppressor grid in front of the collector. It measures ion currents in the range 10-5950 V." SENSITIVITY_DESC = " Depending on the integration time the detector measures current from a minimum of 3.E-14 to 2.E-13 AMPS up to a maximum of 6.E-8 AMPS." END_OBJECT = INSTDETECT OBJECT = INSTDETECT DETECTOR_ID = 'C' DETECTOR_TYPE = "FARADAY CUP" DETECTOR_ASPECT_RATIO = 0.000000 MINIMUM_WAVELENGTH = 'N/A' MAXIMUM_WAVELENGTH = 'N/A' NOMINAL_OPERATING_TEMPERATURE = 278.000000 DETECTOR_DESC = " This detector is a Faraday Cup which is part of a cluster of three detectors (A, B, C) arranged in a cone whose central axis is parallel to the direction of the Telemetry antenna. The look direction of the cup is offset 20 degrees from the central axis. It consists of three modulator grids, six shield grids and a suppressor grid in front of the collector. It measures ion currents in the range 10-5950 V." SENSITIVITY_DESC = " Depending on the integration time the detector measures current from a minimum of 3.E-14 to 2.E-13 AMPS up to a maximum of 6.E-8 AMPS." END_OBJECT = INSTDETECT OBJECT = INSTDETECT DETECTOR_ID = 'D' DETECTOR_TYPE = "FARADAY CUP" DETECTOR_ASPECT_RATIO = 0.000000 MINIMUM_WAVELENGTH = 'N/A' MAXIMUM_WAVELENGTH = 'N/A' NOMINAL_OPERATING_TEMPERATURE = 278.000000 DETECTOR_DESC = " This detector is a Faraday Cup which has a look direction approximately perpendicular to the direction of the telemetry antenna. It consists of three modulator grids, six shield grids and a suppressor grid in front of a collector. It measures both electron and ion currents in the range 10-5950 V." SENSITIVITY_DESC = " Depending on the integration time the detector measures current from a minimum of 3.E-14 to 2.E-13 AMPS up to a maximum of 6.E-8 AMPS." END_OBJECT = INSTDETECT OBJECT = INSTELEC ELECTRONICS_ID = 'PLS' ELECTRONICS_DESC = " Currents from the four detectors are amplified, filtered, and integrated using four different measurement chains. a single 8-bit logarithmic A-D converter samples the four outputs of the measurement chains and transfers the data to the spacecraft. The high voltage modulator supplies a DC pedestal and a superimposed 400 Hz square wave modulation voltage. For positive ions the modulator grids of all four detectors are driven in parallel. A more complete description and block diagram of the instrument electronics is available in bridge et al., Space Sci. rev., 21, 25, 1977." END_OBJECT = INSTELEC OBJECT = INSTFILTER FILTER_NUMBER = 'N/A' FILTER_NAME = 'N/A' FILTER_TYPE = 'N/A' MINIMUM_WAVELENGTH = 'N/A' CENTER_FILTER_WAVELENGTH = 'N/A' MAXIMUM_WAVELENGTH = 'N/A' MEASUREMENT_WAVE_CALBRT_DESC = 'N/A' END_OBJECT = INSTFILTER OBJECT = INSTOPTICS TELESCOPE_ID = 'N/A' TELESCOPE_FOCAL_LENGTH = 'N/A' TELESCOPE_DIAMETER = 'N/A' TELESCOPE_F_NUMBER = 'N/A' TELESCOPE_RESOLUTION = 'N/A' TELESCOPE_TRANSMITTANCE = 'N/A' TELESCOPE_T_NUMBER = 'N/A' TELESCOPE_T_NUMBER_ERROR = 'N/A' TELESCOPE_SERIAL_NUMBER = 'N/A' OPTICS_DESC = 'N/A' END_OBJECT = INSTOPTICS OBJECT = SCINSTOFFSET PLATFORM_OR_MOUNTING_NAME = "SCAN PLATFORM" CONE_OFFSET_ANGLE = 'N/A' CROSS_CONE_OFFSET_ANGLE = 'N/A' TWIST_OFFSET_ANGLE = 'N/A' INSTRUMENT_MOUNTING_DESC = " The PLS instrument is located on the Science Boom. The center of the main detector cluster (A, B, C) points parallel to the spacecraft Telemetry antenna and detector D is at right angles to this direction." END_OBJECT = SCINSTOFFSET OBJECT = INSTSECTION SECTION_ID = 'PLS' OBJECT = INSTSECTINFO SCAN_MODE_ID = 'N/A' DATA_RATE = 'N/A' SAMPLE_BITS = 'N/A' TOTAL_FOVS = 'N/A' OBJECT = INSTSECTFOVS FOV_SHAPE_NAME = 'N/A' HORIZONTAL_PIXEL_FOV = 'N/A' VERTICAL_PIXEL_FOV = 'N/A' HORIZONTAL_FOV = 'N/A' VERTICAL_FOV = 'N/A' FOVS = 'N/A' END_OBJECT = INSTSECTFOVS END_OBJECT = INSTSECTINFO OBJECT = INSTSECTPARM INSTRUMENT_PARAMETER_NAME = "ELECTRON CURRENT" MINIMUM_INSTRUMENT_PARAMETER = 0.000000 MAXIMUM_INSTRUMENT_PARAMETER = 0.000000 NOISE_LEVEL = 'N/A' INSTRUMENT_PARAMETER_UNIT = 'AMPS' SAMPLING_PARAMETER_NAME = 'TIME' MINIMUM_SAMPLING_PARAMETER = 0.030000 MAXIMUM_SAMPLING_PARAMETER = 0.930000 SAMPLING_PARAMETER_INTERVAL = 'N/A' SAMPLING_PARAMETER_RESOLUTION = 'N/A' SAMPLING_PARAMETER_UNIT = 'SECOND' END_OBJECT = INSTSECTPARM OBJECT = INSTSECTPARM INSTRUMENT_PARAMETER_NAME = "ION CURRENT" MINIMUM_INSTRUMENT_PARAMETER = 0.000000 MAXIMUM_INSTRUMENT_PARAMETER = 0.000000 NOISE_LEVEL = 'N/A' INSTRUMENT_PARAMETER_UNIT = 'AMPS' SAMPLING_PARAMETER_NAME = 'TIME' MINIMUM_SAMPLING_PARAMETER = 0.030000 MAXIMUM_SAMPLING_PARAMETER = 0.930000 SAMPLING_PARAMETER_INTERVAL = 'N/A' SAMPLING_PARAMETER_RESOLUTION = 'N/A' SAMPLING_PARAMETER_UNIT = 'SECOND' END_OBJECT = INSTSECTPARM OBJECT = INSTSECTDET DETECTOR_ID = 'A' END_OBJECT = INSTSECTDET OBJECT = INSTSECTDET DETECTOR_ID = 'B' END_OBJECT = INSTSECTDET OBJECT = INSTSECTDET DETECTOR_ID = 'C' END_OBJECT = INSTSECTDET OBJECT = INSTSECTDET DETECTOR_ID = 'D' END_OBJECT = INSTSECTDET OBJECT = INSTSECTELEC ELECTRONICS_ID = 'PLS' END_OBJECT = INSTSECTELEC OBJECT = INSTSECTFILT FILTER_NUMBER = 'A' END_OBJECT = INSTSECTFILT OBJECT = INSTSECTOPTC TELESCOPE_ID = 'N/A' END_OBJECT = INSTSECTOPTC END_OBJECT = INSTSECTION OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "E1-LONG" GAIN_MODE_ID = 'N/A' DATA_PATH_TYPE = 'N/A' INSTRUMENT_POWER_CONSUMPTION = 8.100000 INSTRUMENT_MODE_DESC = " Low energy electron mode which measures the range 10-140 V with 16 contiguous channels. The integration time for each channel is 0.93 sec." OBJECT = INSTMODESECT SECTION_ID = 'PLS' END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "E1-SHORT" GAIN_MODE_ID = 'N/A' DATA_PATH_TYPE = 'N/A' INSTRUMENT_POWER_CONSUMPTION = 8.100000 INSTRUMENT_MODE_DESC = " Low energy electron mode which measures the range 10-140 V with 16 contiguous channels. The integration time for each channel is 0.21 sec." OBJECT = INSTMODESECT SECTION_ID = 'PLS' END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "E2-LONG" GAIN_MODE_ID = 'N/A' DATA_PATH_TYPE = 'N/A' INSTRUMENT_POWER_CONSUMPTION = 8.100000 INSTRUMENT_MODE_DESC = " High energy electron mode which measures the range 10-5950 V with 16 contiguous channels. The integration time for each channel is 0.93 sec." OBJECT = INSTMODESECT SECTION_ID = 'PLS' END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "E2-SHORT" GAIN_MODE_ID = 'N/A' DATA_PATH_TYPE = 'N/A' INSTRUMENT_POWER_CONSUMPTION = 8.100000 INSTRUMENT_MODE_DESC = " High energy electron mode which measures the range 10-5950 V with 16 contiguous channels. The integration time for each channel is 0.21 sec." OBJECT = INSTMODESECT SECTION_ID = 'PLS' END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "L-LONG" GAIN_MODE_ID = 'N/A' DATA_PATH_TYPE = 'N/A' INSTRUMENT_POWER_CONSUMPTION = 8.100000 INSTRUMENT_MODE_DESC = " Low resolution ion mode which measures the range 10-5950 V with 16 contiguous channels. The integration time for each channel is 0.93 sec." OBJECT = INSTMODESECT SECTION_ID = 'PLS' END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "L-SHORT" GAIN_MODE_ID = 'N/A' DATA_PATH_TYPE = 'N/A' INSTRUMENT_POWER_CONSUMPTION = 8.100000 INSTRUMENT_MODE_DESC = " Low resolution ion mode which measures the range 10-5950 V with 16 contiguous channels. The integration time for each channel is 0.21 sec." OBJECT = INSTMODESECT SECTION_ID = 'PLS' END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "M-LONG" GAIN_MODE_ID = 'N/A' DATA_PATH_TYPE = 'N/A' INSTRUMENT_POWER_CONSUMPTION = 8.100000 INSTRUMENT_MODE_DESC = " High resolution ion mode which measures the range 10-5950 V with 128 contiguous channels. The integration time for each channel is 0.93 sec." OBJECT = INSTMODESECT SECTION_ID = 'PLS' END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "M-SHORT" GAIN_MODE_ID = 'N/A' DATA_PATH_TYPE = 'N/A' INSTRUMENT_POWER_CONSUMPTION = 8.100000 INSTRUMENT_MODE_DESC = " High resolution ion mode which measures the range 10-5950 V with 128 contiguous channels. The integration time for each channel is 0.21 sec." OBJECT = INSTMODESECT SECTION_ID = 'PLS' END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = 'BRIDGEETAL1977' OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "PLS INSTRUMENT DESCRIPTION" JOURNAL_NAME = "SPACE SCI. REV." PUBLICATION_DATE = 1977 REFERENCE_DESC = " Bridge, H. S., J. W. Belcher, R. J. Butler, A. J. Lazarus, A. M. Mavretic, J. D. Sullivan, G. L. Siscoe, and V. M. Vasyliunas, The Plasma Experiment on the 1977 Voyager Mission, Space Sci. Rev., 21, 259-287, 1977." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "H. S. BRIDGE" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "J. W. BELCHER" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO END_OBJECT = SCINSTRUMENT /****************** Planetary Radio Astronomy Instrument Template *************/ /* MODIFICATIONS */ /* 920831 -- JPLPDS::RMONARREZ */ /* received by mail */ /* 920916 -- EFRIED */ /* last changes made */ /* Template: Spacecraft Instrument Template Rev: 19890121 */ /* Note: The following templates form part of a standard */ /* set for the submission of a spacecraft instrument */ /* to the PDS. */ /* Hierarchy: SCINSTRUMENT */ /* INSTINFO */ /* INSTDETECT */ /* INSTELEC */ /* INSTFILTER */ /* INSTOPTICS */ /* SCINSTOFFSET */ /* INSTSECTION */ /* INSTSECTINFO */ /* INSTSECTFOVS */ /* INSTSECTPARM */ /* INSTSECTDET */ /* INSTSECTELEC */ /* INSTSECTFILT */ /* INSTSECTOPTC */ /* INSTMODEINFO */ /* INSTMODESECT */ /* INSTREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCINSTRUMENT SPACECRAFT_ID = "VG2" INSTRUMENT_ID = "PRA" OBJECT = INSTINFO INSTRUMENT_NAME = "PLANETARY RADIO ASTRONOMY RECEIVER" INSTRUMENT_TYPE = "RADIO SPECTROMETER" PI_PDS_USER_ID = "N/A" NAIF_DATA_SET_ID = "N/A" BUILD_DATE = "UNK" INSTRUMENT_MASS = 7.7 INSTRUMENT_HEIGHT = "UNK" INSTRUMENT_LENGTH = "UNK" INSTRUMENT_WIDTH = "UNK" INSTRUMENT_MANUFACTURER_NAME = "MARK MARIETTA" INSTRUMENT_SERIAL_NUMBER = "UNK" INSTRUMENT_DESC = " The Voyager Planetary Radio Astronomy (PRA) receiver comprises a 200-channel radio receiver which covers the range from 1.2 kHz to 40 MHz. The receiver is capable of operation in 14 distinct useful modes. The instrument returns 16-bit status words, which generally replace the first two eight-bit data numbers within a single scan of 200 data numbers. The channels are numbered so that the lowest frequency channel (1.2 kHz center frequency - cf) is channel number 200. Channels in the range 1 to 130 are referred to as 'high band', and the remaining channels as 'low band'. In low band, the channel spacing is 19.2 kHz. In high band, the lowest channel (cf) is at 1.3 MHz, and the channel spacing is 307.2 kHz. The instrument is sensitive to, and can distinguish between, the opposing states of circular polarization of an incoming wave. THE PRA STATUS WORD The PRA status word is a 16-bit quantity. The bits are interpreted as follows (in the format S(n), where n is the nth bit of the status word; bits are numbered zero through fifteen, with the Most Significant Bit (MSB) as bit zero): S(0) - phase calibrator on S(1) through S(4) - PRA mode (see below) S(5) - A/D from lower channel S(6) - RHC from upper channel S(7) - PLL closed S(8) - PLL unlocked S(9) - channel toggling disabled *** see below S(10) - calibrate power on S(11) - calibrate bypass open *** see below S(12) - lower preamp selected S(13) - 45 dB attenuator in S(14) - 30 dB attenuator in S(15) - 15 dB attenuator in *** the meanings of S(9) and S(11) were changed around 1980. For status words returned after this time, bits S(9) and S(11) represent a 2-bit POR counter. These bits are overwritten by the spacecraft FDS, and the counter is incremented every time that the FDS detects a PRA POR. The FDS assumes that a POR has occurred whenever it sees a PRA status word with all three attenuator bits set, since this is the power-up condition of the PRA. Graphically, this is: | 0 | 1 | 2 | 3 | 4 | 5 | 6 | 7 | ---------------------------- ----------------------------- |PHASE | FIXED |POLHI| POL |HARAD | A/D | RHC | LOOP | | CAL | FREQ | OR |SWITCH| OR | FROM |UPPER | CLOSED| | ON | MODE |LEVEL| OFF | HF |LOWER | | | ---------------------------- ----------------------------- | 8 | 9 | 10 | 11 | 12 | 13 | 14 | 15 | ---------------------------- ----------------------------- | LOOP | CHAN | CAL | CAL |LOWER | 45DB | 30DB | 15DB | | UN- | TOGGLE|POWER|BYPASS|PREAMP| IN | IN | IN | |LOCKED|DISABLE| ON | OPEN |SELECT| | | | ---------------------------- ----------------------------- Bits S(1) through S(4) return the mode in which the PRA instrument is running. These are as follows: 0000 - POLLO 0001 - HARAD 0010 - POLLO1 0011 - HARAD1 0100 - LEVEL 0101 - LEVEL1 0110 - LEVEL2 0111 - LEVEL3 1000 - FIXLOL 1001 - FIXLOH 1010 - VLOBRL 1011 - VLOBRH 1100 - XXXXXL 1101 - XXXXXH 1110 - POLHIL 1111 - POLHIH ******************************* *********************************** The remainder of this text describes the meanings of the various modes in the order presented above. ******************************* *********************************** ***************** POLLO ***************** Data produced every 30 msec; 25 msec of integration; bandwidth is 200 kHz in high band, 1 kHz in low band. Channel spacing is 307.2 kHz in high band and 19.2 kHz in low band. The lowest high band channel is at 1.3 MHz (cf), and the lowest low band channel is at 1.2 kHz (cf). Data come from either the upper instrument channel or the lower instrument channel only. That is, THERE IS NO CHANNEL TOGGLING, regardless of the setting of the configuration command. Polarization of data word number 'n' is reversed each time that a MODE command is received (usually every six seconds). STATUS X000 000X XXXX XXXX Odd numbered data words 003-129 contain LH, UC data; Odd numbered data words 131-199 contain RH, UC data; Even numbered data words 004-130 contain RH, UC data; Even numbered data words 132-200 contain LH, UC data. STATUS X000 001X XXXX XXXX Odd numbered data words 003-129 contain RH, UC data; Odd numbered data words 131-199 contain LH, UC data; Even numbered data words 004-130 contain LH, UC data; Even numbered data words 132-200 contain RH, UC data. STATUS X000 010X XXXX XXXX Odd numbered data words 003-129 contain RH, LC data; Odd numbered data words 131-199 contain LH, LC data; Even numbered data words 004-130 contain LH, LC data; Even numbered data words 132-200 contain RH, LC data. STATUS X000 011X XXXX XXXX Odd numbered data words 003-129 contain LH, LC data; Odd numbered data words 131-199 contain RH, LC data; Even numbered data words 004-130 contain RH, LC data; Even numbered data words 132-200 contain LH, LC data. ***************** POLLO1 ***************** Data produced every 30 msec; 25 msec of integration; bandwidth is 200 kHz in high band, 1 kHz in low band. Channel spacing is 307.2 kHz in high band and 19.2 kHz in low band. The lowest high band channel is at 1.3 MHz (cf), and the lowest low band channel is at 1.2 kHz (cf). Data come from either the upper instrument channel or the lower instrument channel only. That is, THERE IS NO CHANNEL TOGGLING, regardless of the setting of the configuration command. Polarization does not alternate between adjacent channels. STATUS X001 000X XXXX XXXX Data words 003-130 contain LH, UC data; Data words 131-200 contain RH, UC data. STATUS X001 001X XXXX XXXX Data words 003-130 contain RH, UC data; Data words 131-200 contain LH, UC data. STATUS X001 010X XXXX XXXX Data words 003-130 contain RH, LC data; Data words 131-200 contain LH, UC data. STATUS X001 011X XXXX XXXX Data words 003-130 contain LH, LC data; Data words 131-200 contain RH, UC data. ***************** HARAD ***************** Data produced every 30 msec; 25 msec of integration; bandwidth is 200 Khz in high band, 800 Hz in low band. Channel spacing is 307.2 Khz in high band and 19.2 kHz in low band. The lowest high band channel is at 1.3 MHz (cf), and the lowest low band channel is at 2.4 kHz (cf). Data come from either the upper instrument channel or the lower instrument channel only. That is, THERE IS NO CHANNEL TOGGLING, regardless of the setting of the configuration command. Polarization of data word number 'n' is reversed each time that a MODE command is received (usually every six seconds). STATUS X000 100X XXXX XXXX Odd numbered data words 003-129 contain LH, UC data; Odd numbered data words 131-199 contain RH, UC data; Even numbered data words 004-130 contain RH, UC data; Even numbered data words 132-200 contain LH, UC data. STATUS X000 101X XXXX XXXX Odd numbered data words 003-129 contain RH, UC data; Odd numbered data words 131-199 contain LH, UC data; Even numbered data words 004-130 contain LH, UC data; Even numbered data words 132-200 contain RH, UC data. STATUS X000 110X XXXX XXXX Odd numbered data words 003-129 contain RH, LC data; Odd numbered data words 131-199 contain LH, LC data; Even numbered data words 004-130 contain LH, LC data; Even numbered data words 132-200 contain RH, LC data. STATUS X000 111X XXXX XXXX Odd numbered data words 003-129 contain LH, LC data; Odd numbered data words 131-199 contain RH, LC data; Even numbered data words 004-130 contain RH, LC data; Even numbered data words 132-200 contain LH, LC data. ******************* HARAD1 ******************* Data produced every 30 msec; 25 msec of integration; bandwidth is 200 kHz in high band, 1 kHz in low band. Channel spacing is 307.2 kHz in high band and 19.2 kHz in low band. The lowest high band channel is at 1.3 MHz (cf), and the lowest low band channel is at 2.4 kHz (cf). Data come from either the upper instrument channel or the lower instrument channel only. That is, THERE IS NO CHANNEL TOGGLING, regardless of the setting of the configuration command. Polarization does not alternate between adjacent channels. STATUS X001 100X XXXX XXXX Data words 003-130 contain LH, UC data; Data words 131-200 contain RH, UC data. STATUS X001 101X XXXX XXXX Data words 003-130 contain RH, UC data; Data words 131-200 contain LH, UC data. ** THE FOLLOWING TWO DESCRIPTIONS ARE UNDOCUMENTED, but follow logically from the behavior of the instrument in the other modes. Treat them with caution, however. STATUS X001 110X XXXX XXXX Data words 003-130 contain RH, LC data; Data words 131-200 contain LH, UC data. STATUS X001 111X XXXX XXXX Data words 003-130 contain LH, LC data; Data words 131-200 contain RH, UC data. ***************** LEVEL ***************** Data produced every 30 msec; 25 msec of integration. Channel spacing is 307.2 kHz in high band and 19.2 kHz in low band. The lowest high band channel is at 1.3 MHz (cf), and the lowest low band channel is at 1.2 kHz (cf). Bandwidth is 200 kHz in high band, 1 kHz in low band. Polarization alternates every data word. STATUS X010 00XX X0XX XXXX Take the channel number modulo 4 Data words 003-130: Channel modulo 4 0 1 2 3 Data RH, UC RH, LC LH, LC LH, UC Data words 131-200: Channel modulo 4 0 1 2 3 Data LH, UC LH, LC RH, LC RH, UC STATUS X010 00XX X1XX XXXX Odd numbered data words 003-129 contain LH, UC data; Odd numbered data words 131-199 contain RH, UC data; Even numbered data words 004-130 contain RH, UC data; Even numbered data words 132-200 contain LH, UC data. STATUS X010 01XX X0XX XXXX Take the channel number modulo 4 Data words 003-130: Channel modulo 4 0 1 2 3 Data LH, LC LH, UC RH, UC RH, LC Data words 131-200: Channel modulo 4 0 1 2 3 Data RH, LC RH, UC LH, UC LH, LC STATUS X010 01XX X1XX XXXX Odd numbered data words 003-129 contain RH, LC data; Odd numbered data words 131-199 contain LH, LC data; Even numbered data words 004-130 contain LH, LC data; Even numbered data words 132-200 contain RH, LC data. ***************** LEVEL1 ***************** Data produced every 30 msec; 25 msec of integration. Channel spacing is 307.2 kHz in high band and 19.2 kHz in low band. The lowest high band channel is at 1.3 MHz (cf), and the lowest low band channel is at 1.2 kHz (cf). Bandwidth is 200 kHz in high band, 800 Hz in low band. Polarization alternates every data word. STATUS X010 10XX X0XX XXXX Take the channel number modulo 4 Data words 003-130: Channel modulo 4 0 1 2 3 Data RH, UC RH, LC LH, LC LH, UC Data words 131-200: Channel modulo 4 0 1 2 3 Data LH, UC LH, LC RH, LC RH, UC STATUS X010 00XX X1XX XXXX Odd numbered data words 003-129 contain LH, UC data; Odd numbered data words 131-199 contain RH, UC data; Even numbered data words 004-130 contain RH, UC data; Even numbered data words 132-200 contain LH, UC data. STATUS X010 11XX X0XX XXXX Take the channel number modulo 4 Data words 003-130: Channel modulo 4 0 1 2 3 Data LH, LC LH, UC RH, UC RH, LC Data words 131-200: Channel modulo 4 0 1 2 3 Data RH, LC RH, UC LH, UC LH, LC STATUS X010 11XX X1XX XXXX Odd numbered data words 003-129 contain RH, LC data; Odd numbered data words 131-199 contain LH, LC data; Even numbered data words 004-130 contain LH, LC data; Even numbered data words 132-200 contain RH, LC data. ***************** LEVEL2 ***************** Data produced every 30 msec; 25 msec of integration. Channel spacing is 307.2 kHz in high band and 19.2 kHz in low band. The lowest high band channel is at 1.3 MHz (cf), and the lowest low band channel is at 1.2 kHz (cf). Bandwidth is 200 kHz in high band, 1 kHz in low band. Polarization does not alternate. STATUS X011 00XX X0XX XXXX Take the channel number modulo 4 Data words 003-130: Channel modulo 4 0 1 2 3 Data LH, UC RH, LC RH, LC LH, UC Data words 131-200: Channel modulo 4 0 1 2 3 Data RH, UC LH, LC LH, LC RH, UC STATUS X011 00XX X1XX XXXX Data words 003-130 contain LH, UC data; Data words 131-200 contain RH, UC data; STATUS X011 01XX X0XX XXXX Take the channel number modulo 4 Data words 003-130: Channel modulo 4 0 1 2 3 Data RH, LC LH, UC LH, UC RH, LC Data words 131-200: Channel modulo 4 0 1 2 3 Data LH, LC RH, UC RH, UC LH, LC STATUS X011 01XX X1XX XXXX Data words 003-130 contain RH, LC data; Data words 131-200 contain LH, LC data; ***************** LEVEL3 ***************** Data produced every 30 msec; 25 msec of integration. Channel spacing is 307.2 kHz in high band and 19.2 kHz in low band. The lowest high band channel is at 1.3 MHz (cf), and the lowest low band channel is at 1.2 kHz (cf). Bandwidth is 200 kHz in high band, 800 Hz in low band. Polarization does not alternate. STATUS X011 10XX X0XX XXXX Take the channel number modulo 4 Data words 003-130: Channel modulo 4 0 1 2 3 Data LH, UC RH, LC RH, LC LH, UC Data words 131-200: Channel modulo 4 0 1 2 3 Data RH, UC LH, LC LH, LC RH, UC STATUS X011 10XX X1XX XXXX Data words 003-130 contain LH, UC data; Data words 131-200 contain RH, UC data; STATUS X011 11XX X0XX XXXX Take the channel number modulo 4 Data words 003-130: Channel modulo 4 0 1 2 3 Data RH, LC LH, UC LH, UC RH, LC Data words 131-200: Channel modulo 4 0 1 2 3 Data LH, LC RH, UC RH, UC LH, LC STATUS X011 11XX X1XX XXXX Data words 003-130 contain RH, LC data; Data words 131-200 contain LH, LC data; ***************** FIXLOL ***************** Data produced every 30 msec; 25 msec of integration. Frequency is fixed. Bandwidth is 1 kHz. STATUS X100 00XX X0XX XXXX Take the channel number modulo 4 Channel modulo 4 0 1 2 3 Data LH, UC LH, LC RH, LC RH, UC STATUS X100 00XX X1XX XXXX Odd numbered data words contain RH, UC data Even numbered data words contain LH, UC data STATUS X100 01XX X0XX XXXX Take the channel number modulo 4 Channel modulo 4 0 1 2 3 Data RH, LC RH, UC LH, UC LH, LC STATUS X100 01XX X1XX XXXX Odd numbered data words contain LH, LC data Even numbered data words contain RH, LC data ***************** FIXLOH ***************** Data produced every 30 msec; 25 msec of integration. Frequency is fixed. Bandwidth is 200 kHz. STATUS X100 10XX X0XX XXXX Take the channel number modulo 4 Channel modulo 4 0 1 2 3 Data RH, UC RH, LC LH, LC LH, UC STATUS X100 10XX X1XX XXXX Odd numbered data words contain LH, UC data Even numbered data words contain RH, UC data STATUS X100 11XX X0XX XXXX Take the channel number modulo 4 Channel modulo 4 0 1 2 3 Data LH, LC LH, UC RH, UC RH, LC STATUS X100 11XX X1XX XXXX Odd numbered data words contain RH, LC data Even numbered data words contain LH, LC data ***************** VLOBRL ***************** Data produced every 30 msec; 25 msec of integration. Frequency is fixed. Bandwidth is 1 kHz. STATUS X101 00XX X0XX XXXX Odd numbered data words contain LH, LC data Even numbered data words contain RH, UC data STATUS X101 00XX X1XX XXXX All data words contain RH, UC data STATUS X101 01XX X0XX XXXX Odd numbered data words contain RH, UC data Even numbered data words contain LH, LC data STATUS X101 01XX X1XX XXXX All data words contain LH, LC data ***************** VLOBRH ***************** Data produced every 30 msec; 25 msec of integration. Frequency is fixed. Bandwidth is 200 kHz. STATUS X101 10XX X0XX XXXX Odd numbered data words contain RH, LC data Even numbered data words contain LH, UC data STATUS X101 10XX X1XX XXXX All data words contain LH, UC data STATUS X101 11XX X0XX XXXX Odd numbered data words contain LH, UC data Even numbered data words contain RH, LC data STATUS X101 11XX X1XX XXXX All data words contain RH, LC data ***************** XXXXXL ***************** STATUS X110 1XXX XXXX XXXX No meaningful data are returned because the polarization alternates every 69.4 microseconds, but the RC time constant is 100 microseconds. ***************** XXXXXH ***************** STATUS X110 0XXX XXXX XXXX No meaningful data are returned because the polarization alternates every 69.4 microseconds, but the RC time constant is 100 microseconds. ***************** n/ POLHIL ***************** Data produced every 69.4 microseconds, but sample-and-hold operates once every 138.8 microseconds on both data channels simultaneously (i.e. channels 2n-1 and 2n contain simultaneously sampled data). Integration time is 100 microseconds with an RC circuit (i.e. exponential). Frequency is fixed. Bandwidth is 1 kHz. STATUS X111 00XX X0XX XXXX Odd numbered data words contain LH, LC data Even numbered data words contain RH, UC data STATUS X111 00XX X1XX XXXX All data words contain RH, UC data STATUS X111 01XX X0XX XXXX Odd numbered data words contain RH, UC data Even numbered data words contain LH, LC data STATUS X111 01XX X1XX XXXX All data words contain LH, LC data ***************** POLHIH ***************** Data produced every 69.4 microseconds, but sample-and-hold operates once every 138.8 microseconds on both data channels simultaneously (i.e. channels 2n-1 and 2n contain simultaneously sampled data). Integration time is 100 microseconds with an RC circuit (i.e. exponential). Frequency is fixed. Bandwidth is 200 kHz. STATUS X111 10XX X0XX XXXX Odd numbered data words contain RH, LC data Even numbered data words contain LH, UC data STATUS X111 10XX X1XX XXXX All data words contain LH, UC data STATUS X111 11XX X0XX XXXX Odd numbered data words contain LH, UC data Even numbered data words contain RH, LC data STATUS X111 11XX X1XX XXXX All data words contain RH, LC data ***************** CONFIGURATION COMMAND ***************** The PRA configuration command is contained in the EDR header. It is a 16-bit word whose last four bits are always '0011'. The remaining bits are: C(0) - calibrator power on C(1) - phase calibrate on C(2) - calibrator bypass open C(3) - A/D from upper C(4) - channel toggle disable C(5) - loop closed C(6) - 45dB attenuator out C(7) - unused C(8) - calibrate inject C(9) - upper preamp select C(10) - 30dB attenuator out C(11) - 15dB attenuator out C(12) - 0 C(13) - 0 C(14) - 1 C(15) - 1 | 0 | 1 | 2 | 3 | 4 | 5 | 6 | 7 | ------------------------------ ---------------------------- | CAL | PHASE | CAL | A/D | CHAN | LOOP | 45DB| | | POWER| CAL | BYPASS| FROM | TOGGLE|CLOSED| OUT |UNUSED| | ON | ON | OPEN | UPPER|DISABLE| | | | ------------------------------ ---------------------------- | 8 | 9 | 10 | 11 | 12 | 13 | 14 | 15 | ------------------------------ ---------------------------- | CAL | UPPER | 30DB | 15DB| | | | | |INJECT| PREAMP| OUT | OUT | 0 | 0 | 1 | 1 | | | SELECT| | | | | | | ------------------------------ ----------------------------- Note that many (but not all!) of these bits are the logical inverse of bits in the status word. MODE WORD M(0) - fixed frequency mode M(1) - POLHI or LEVEL M(2) - polarization switch off M(3) - HARAD or HF M(4) to M(11) - frequency bits M(12) - 0 M(13) - 0 M(14) - 1 M(15) - 1 | 0 | 1 | 2 | 3 | 4 | 5 | 6 | 7 | -------------------------------- ------------------------- | FIXED | POLHI | POL | HARAD | | | | | | FREQ | OR | SWITCH| OR | F | R | E | Q | | MODE | LEVEL | OFF | HF | | | | | -------------------------------- ------------------------- | 8 | 9 | 10 | 11 | 12 | 13 | 14 | 15 | -------------------------------- ------------------------- | | | | | | | | | | B | I | T | S | 0 | 0 | 1 | 1 | | | | | | | | | | -------------------------------- -------------------------" /* /* /* SCIENTIFIC_OBJECTIVES_SUMMARY = " The Planetary Radio Astronomy (PRA) experiments' primary objective is to locate and explain kilometric, hectometric, and decametric radio emissions from the planets, to measure plasma resonances near the giant planets, and to detect lightning on the giant planets. They have also been successful at observing solar radio emissions from the perspective of the outer solar system. The Voyager Planetary Radio Astronomy experiment is designed to investigate naturally-occurring radio emissions from the outer planets and Sun. Radio emissions from Jupiter have been known from Earth-based measurements since 1955; PRA represents the first attempt to survey those emissions, and to perform near-encounter searches for radio emissions from the other gas planets. Radio emissions can be used to determine the rate of rotation of the inner core of a planet; to determine the existence of a magnetic field and search for magnetic anomalies. Radio emissions are often the only remote diagnostic for interactions occurring in the portions of magnetospheres through which a spacecraft does not pass. This is particularly true for the inner magnetosphere, which usually goes unsampled. PRA is also sensitive to impacts on the spacecraft by micron-sized dust particles. Particularly in its high data rate modes, the information obtained therefrom produces insights into the processes which occur under such situations." /* /* /* INSTRUMENT_CALIBRATION_DESC = " The Planetary Radio Astronomy (PRA) receivers were calibrated under environmentally- controlled conditions and over the entire frequency and dynamic range of the instruments. This calibration consisted in application of a known narrow-band signal across the inputs and recording the receiver outputs. This falls far short of an overall, front-to-back calibration of the instruments, including their antennas performing on the actual spacecraft in deep space under conditions of perfect vacuum. This full calibration was not possible for many reasons. To fill this gap, we have implemented software programs that electromagnetically model the spacecraft with, in practice, 168 conducting elements; in principle, with more powerful computers, this limitation could be made even less restrictive. The ideal for which we strive is a conversion of the receivers' data numbers to absolute flux density values for signals of known direction of arrival and polarization. The laboratory calibrations provide us with power levels for each data number (DN) and each frequency in terms of known inputs across the antenna terminals of each of the experiment's two monopoles. calibrations were carried out over a range of receiver temperatures, but in practice the stability of the receiver as a function of temperature and the stability of the temperature of the receiver as a function of mission phase and the status of the overall spacecraft have been such as to allow us to use a single calibration curve for each DN and for each frequency. The minimum value for the wave flux density is frequency dependent varying from 5.E-20 W M**-2 Hz**-1 at frequencies below 1.5MHz to 5.E-19 to frequencies above 1.5MHz. The maximum wave flux density is typically 50 dB above the minimum values. The instrument noise level also is frequency dependent. It is about 1.E-19 W M**-2 Hz**-1 below 1.5MHz. The noise at 10 MHz is still about 1E-19 W M**-2 Hz**-1, increases to about 1.E-17 W M**-2 Hz**-1 at 25 MHz and then decreases to an intermediate value at 40 MHz. The low-band operation of the receivers, from 1.2kHz to 1326.0 kHz, and the high-band operation of the receiver, from 1228.8 kHz to 40.5504 MHz, differ. In low-band the receiver operates with a sharply tuned filter only 1 kHz broad at the 3 dB points and in high-band, with a 200 kHz filter. The gain of the receivers is designed in such a way that the output increases discontinuously by 23 dB as they tune downward through the transition frequency. This causes the receiver output to remain constant if its input is broadband noise sensibly constant across the transition point. If unpolarized radiation falls orthogonally on each monopole, the total unpolarized flux density for signals below about 5 MHz can be roughly estimated to be S = So (10**(m/1000)), where m is the channel reading in millibels an So is So = 1.5E-21 (W/Hz m**2). With courage, one may even use these formulas at higher frequencies. But, for more accurate values at low frequencies, or for significant flux density values at higher frequencies, it is necessary to use the spacecraft EM modeling techniques mentioned above. Since the resulting flux density values depend on polarization of the emission there is no practical way to provide the general user with simple algorithms to convert millibels to flux density." OPERATIONAL_CONSID_DESC = "Not applicable." END_OBJECT = INSTINFO /* */ /* Instrument Detectors */ /* */ OBJECT = INSTDETECT DETECTOR_ID = "PRA ANTENNA" DETECTOR_TYPE = "MONOPOLE PR ANTENNA" DETECTOR_ASPECT_RATIO = "N/A" MINIMUM_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" NOMINAL_OPERATING_TEMPERATURE= 298 DETECTOR_DESC = "The Planetary Radio Astronomy (PRA) Antennas are 10 meter BeCu hollow tubes 0.5 inches in diameter mounted orthogonal to one another." SENSITIVITY_DESC = "Not applicable." END_OBJECT = INSTDETECT OBJECT = INSTELEC ELECTRONICS_ID = "PRA" ELECTRONICS_DESC = "The PRA consists of two superhetordyne receivers, one for the range from 1326.0 to 1.2 kHz and a second for the range 40.55 to 1.5 MHz." END_OBJECT = INSTELEC OBJECT = INSTFILTER FILTER_NUMBER = "N/A" FILTER_NAME = "N/A" FILTER_TYPE = "N/A" MINIMUM_WAVELENGTH = "N/A" CENTER_FILTER_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" MEASUREMENT_WAVE_CALBRT_DESC = "Not applicable." END_OBJECT = INSTFILTER OBJECT = INSTOPTICS TELESCOPE_ID = "N/A" TELESCOPE_FOCAL_LENGTH = "N/A" TELESCOPE_DIAMETER = "N/A" TELESCOPE_F_NUMBER = "N/A" TELESCOPE_RESOLUTION = "N/A" TELESCOPE_TRANSMITTANCE = "N/A" TELESCOPE_T_NUMBER = "N/A" TELESCOPE_T_NUMBER_ERROR = "N/A" TELESCOPE_SERIAL_NUMBER = "N/A" OPTICS_DESC = "Not applicable." END_OBJECT = INSTOPTICS OBJECT = SCINSTOFFSET PLATFORM_OR_MOUNTING_NAME = "SPACECRAFT BUS" CONE_OFFSET_ANGLE = "N/A" CROSS_CONE_OFFSET_ANGLE = "N/A" TWIST_OFFSET_ANGLE = "N/A" INSTRUMENT_MOUNTING_DESC = "Not applicable." END_OBJECT = SCINSTOFFSET OBJECT = INSTSECTION SECTION_ID = "PRA" OBJECT = INSTSECTINFO SCAN_MODE_ID = "N/A" DATA_RATE = 266.667 SAMPLE_BITS = 8 TOTAL_FOVS = 1 OBJECT = INSTSECTFOVS FOV_SHAPE_NAME = "N/A" HORIZONTAL_PIXEL_FOV = "N/A" VERTICAL_PIXEL_FOV = "N/A" HORIZONTAL_FOV = 360 VERTICAL_FOV = 180 FOVS = 1 END_OBJECT = INSTSECTFOVS END_OBJECT = INSTSECTINFO OBJECT = INSTSECTPARM INSTRUMENT_PARAMETER_NAME = "WAVE FLUX DENSITY" MINIMUM_INSTRUMENT_PARAMETER = 1400 MAXIMUM_INSTRUMENT_PARAMETER = 17000 NOISE_LEVEL = 2400 INSTRUMENT_PARAMETER_UNIT = "WATT/METER**2/HERTZ" SAMPLING_PARAMETER_NAME = "FREQUENCY" MINIMUM_SAMPLING_PARAMETER = 7.0E2 MAXIMUM_SAMPLING_PARAMETER = 4.1336E7 SAMPLING_PARAMETER_INTERVAL = "N/A" SAMPLING_PARAMETER_RESOLUTION = "N/A" SAMPLING_PARAMETER_UNIT = "HERTZ" END_OBJECT = INSTSECTPARM OBJECT = INSTSECTDET DETECTOR_ID = "PRA ANTENNA" END_OBJECT = INSTSECTDET OBJECT = INSTSECTELEC ELECTRONICS_ID = "PRA" END_OBJECT = INSTSECTELEC OBJECT = INSTSECTFILT FILTER_NUMBER = "N/A" END_OBJECT = INSTSECTFILT OBJECT = INSTSECTOPTC TELESCOPE_ID = "N/A" END_OBJECT = INSTSECTOPTC END_OBJECT = INSTSECTION OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "POLLO" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "N/A" INSTRUMENT_POWER_CONSUMPTION = 6.7 INSTRUMENT_MODE_DESC = " POLLO Data produced every 30 msec; 25 msec of integration; bandwidth is 200 kHz in high band, 1 kHz in low band. Channel spacing is 307.2 kHz in high band and 19.2 kHz in low band. The lowest high band channel is at 1.3 MHz (cf), and the lowest low band channel is at 1.2 kHz (cf). Data come from either the upper instrument channel or the lower instrument channel only. That is, THERE IS NO CHANNEL TOGGLING, regardless of the setting of the configuration command. Polarization of data word number 'n' is reversed each time that a MODE command is received (usually every six seconds). STATUS X000 000X XXXX XXXX Odd numbered data words 003-129 contain LH, UC data; Odd numbered data words 131-199 contain RH, UC data; Even numbered data words 004-130 contain RH, UC data; Even numbered data words 132-200 contain LH, UC data. STATUS X000 001X XXXX XXXX Odd numbered data words 003-129 contain RH, UC data; Odd numbered data words 131-199 contain LH, UC data; Even numbered data words 004-130 contain LH, UC data; Even numbered data words 132-200 contain RH, UC data. STATUS X000 010X XXXX XXXX Odd numbered data words 003-129 contain RH, LC data; Odd numbered data words 131-199 contain LH, LC data; Even numbered data words 004-130 contain LH, LC data; Even numbered data words 132-200 contain RH, LC data. STATUS X000 011X XXXX XXXX Odd numbered data words 003-129 contain LH, LC data; Odd numbered data words 131-199 contain RH, LC data; Even numbered data words 004-130 contain RH, LC data; Even numbered data words 132-200 contain LH, LC data. " OBJECT = INSTMODESECT SECTION_ID = UNK END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO /* */ /* MODE - POLLO1 */ /* */ OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "POLLO1" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "N/A" INSTRUMENT_POWER_CONSUMPTION = 6.7 INSTRUMENT_MODE_DESC = " POLLO1 Data produced every 30 msec; 25 msec of integration; bandwidth is 200 kHz in high band, 1 kHz in low band. Channel spacing is 307.2 kHz in high band and 19.2 kHz in low band. The lowest high band channel is at 1.3 MHz (cf), and the lowest low band channel is at 1.2 kHz (cf). Data come from either the upper instrument channel or the lower instrument channel only. That is, THERE IS NO CHANNEL TOGGLING, regardless of the setting of the configuration command. Polarization does not alternate between adjacent channels. STATUS X001 000X XXXX XXXX Data words 003-130 contain LH, UC data; Data words 131-200 contain RH, UC data. STATUS X001 001X XXXX XXXX Data words 003-130 contain RH, UC data; Data words 131-200 contain LH, UC data. STATUS X001 010X XXXX XXXX Data words 003-130 contain RH, LC data; Data words 131-200 contain LH, UC data. STATUS X001 011X XXXX XXXX Data words 003-130 contain LH, LC data; Data words 131-200 contain RH, UC data." OBJECT = INSTMODESECT SECTION_ID = UNK END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO /* */ /* MODE - HARAD */ /* */ OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "HARAD" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "N/A" INSTRUMENT_POWER_CONSUMPTION = 6.7 INSTRUMENT_MODE_DESC = " HARAD Data produced every 30 msec; 25 msec of integration; bandwidth is 200 kHz in high band, 800 Hz in low band. Channel spacing is 307.2 kHz in high band and 19.2 kHz in low band. The lowest high band channel is at 1.3 MHz (cf), and the lowest low band channel is at 2.4 kHz (cf). Data come from either the upper instrument channel or the lower instrument channel only. That is, THERE IS NO CHANNEL TOGGLING, regardless of the setting of the configuration command. Polarization of data word number 'n' is reversed each time that a MODE command is received (usually every six seconds). STATUS X000 100X XXXX XXXX Odd numbered data words 003-129 contain LH, UC data; Odd numbered data words 131-199 contain RH, UC data; Even numbered data words 004-130 contain RH, UC data; Even numbered data words 132-200 contain LH, UC data. STATUS X000 101X XXXX XXXX Odd numbered data words 003-129 contain RH, UC data; Odd numbered data words 131-199 contain LH, UC data; Even numbered data words 004-130 contain LH, UC data; Even numbered data words 132-200 contain RH, UC data. STATUS X000 110X XXXX XXXX Odd numbered data words 003-129 contain RH, LC data; Odd numbered data words 131-199 contain LH, LC data; Even numbered data words 004-130 contain LH, LC data; Even numbered data words 132-200 contain RH, LC data. STATUS X000 111X XXXX XXXX Odd numbered data words 003-129 contain LH, LC data; Odd numbered data words 131-199 contain RH, LC data; Even numbered data words 004-130 contain RH, LC data; Even numbered data words 132-200 contain LH, LC data." OBJECT = INSTMODESECT SECTION_ID = UNK END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO /* */ /* MODE - HARAD1 */ /* */ OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "HARAD1" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "N/A" INSTRUMENT_POWER_CONSUMPTION = 6.7 INSTRUMENT_MODE_DESC = " HARAD1 Data produced every 30 msec; 25 msec of integration; bandwidth is 200 kHz in high band, 1 kHz in low band. Channel spacing is 307.2 kHz in high band and 19.2 kHz in low band. The lowest high band channel is at 1.3 MHz (cf), and the lowest low band channel is at 2.4 kHz (cf). Data come from either the upper instrument channel or the lower instrument channel only. That is, THERE IS NO CHANNEL TOGGLING, regardless of the setting of the configuration command. Polarization does not alternate between adjacent channels. STATUS X001 100X XXXX XXXX Data words 003-130 contain LH, UC data; Data words 131-200 contain RH, UC data. STATUS X001 101X XXXX XXXX Data words 003-130 contain RH, UC data; Data words 131-200 contain LH, UC data. ** THE FOLLOWING TWO DESCRIPTIONS ARE UNDOCUMENTED, but follow logically from the behavior of the instrument in the other modes. Treat them with caution, however. STATUS X001 110X XXXX XXXX Data words 003-130 contain RH, LC data; Data words 131-200 contain LH, UC data. STATUS X001 111X XXXX XXXX Data words 003-130 contain LH, LC data; Data words 131-200 contain RH, UC data." OBJECT = INSTMODESECT SECTION_ID = UNK END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO /* */ /* MODE - LEVEL */ /* */ OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "LEVEL" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "N/A" INSTRUMENT_POWER_CONSUMPTION = 6.7 INSTRUMENT_MODE_DESC = " LEVEL Data produced every 30 msec; 25 msec of integration. Channel spacing is 307.2 kHz in high band and 19.2 kHz in low band. The lowest high band channel is at 1.3 MHz (cf), and the lowest low band channel is at 1.2 kHz (cf). Bandwidth is 200 kHz in high band, 1 kHz in low band. Polarization alternates every data word. STATUS X010 00XX X0XX XXXX Take the channel number modulo 4 Data words 003-130: Channel modulo 4 0 1 2 3 Data RH, UC RH, LC LH, LC LH, UC Data words 131-200: Channel modulo 4 0 1 2 3 Data LH, UC LH, LC RH, LC RH, UC STATUS X010 00XX X1XX XXXX Odd numbered data words 003-129 contain LH, UC data; Odd numbered data words 131-199 contain RH, UC data; Even numbered data words 004-130 contain RH, UC data; Even numbered data words 132-200 contain LH, UC data. STATUS X010 01XX X0XX XXXX Take the channel number modulo 4 Data words 003-130: Channel modulo 4 0 1 2 3 Data LH, LC LH, UC RH, UC RH, LC Data words 131-200: Channel modulo 4 0 1 2 3 Data RH, LC RH, UC LH, UC LH, LC STATUS X010 01XX X1XX XXXX Odd numbered data words 003-129 contain RH, LC data; Odd numbered data words 131-199 contain LH, LC data; Even numbered data words 004-130 contain LH, LC data; Even numbered data words 132-200 contain RH, LC data." OBJECT = INSTMODESECT SECTION_ID = UNK END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO /* */ /* MODE - LEVEL1 */ /* */ OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "LEVEL1" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "N/A" INSTRUMENT_POWER_CONSUMPTION = 6.7 INSTRUMENT_MODE_DESC = " LEVEL1 Data produced every 30 msec; 25 msec of integration. Channel spacing is 307.2 kHz in high band and 19.2 kHz in low band. The lowest high band channel is at 1.3 MHz (cf), and the lowest low band channel is at 1.2 kHz (cf). Bandwidth is 200 kHz in high band, 800 Hz in low band. Polarization alternates every data word. STATUS X010 10XX X0XX XXXX Take the channel number modulo 4 Data words 003-130: Channel modulo 4 0 1 2 3 Data RH, UC RH, LC LH, LC LH, UC Data words 131-200: Channel modulo 4 0 1 2 3 Data LH, UC LH, LC RH, LC RH, UC STATUS X010 00XX X1XX XXXX Odd numbered data words 003-129 contain LH, UC data; Odd numbered data words 131-199 contain RH, UC data; Even numbered data words 004-130 contain RH, UC data; Even numbered data words 132-200 contain LH, UC data. STATUS X010 11XX X0XX XXXX Take the channel number modulo 4 Data words 003-130: Channel modulo 4 0 1 2 3 Data LH, LC LH, UC RH, UC RH, LC Data words 131-200: Channel modulo 4 0 1 2 3 Data RH, LC RH, UC LH, UC LH, LC STATUS X010 11XX X1XX XXXX Odd numbered data words 003-129 contain RH, LC data; Odd numbered data words 131-199 contain LH, LC data; Even numbered data words 004-130 contain LH, LC data; Even numbered data words 132-200 contain RH, LC data." OBJECT = INSTMODESECT SECTION_ID = UNK END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO /* */ /* MODE - LEVEL2 */ /* */ OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "LEVEL2" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "N/A" INSTRUMENT_POWER_CONSUMPTION = 6.7 INSTRUMENT_MODE_DESC = " LEVEL2 Data produced every 30 msec; 25 msec of integration. Channel spacing is 307.2 kHz in high band and 19.2 kHz in low band. The lowest high band channel is at 1.3 MHz (cf), and the lowest low band channel is at 1.2 kHz (cf). Bandwidth is 200 kHz in high band, 1 kHz in low band. Polarization does not alternate. STATUS X011 00XX X0XX XXXX Take the channel number modulo 4 Data words 003-130: Channel modulo 4 0 1 2 3 Data LH, UC RH, LC RH, LC LH, UC Data words 131-200: Channel modulo 4 0 1 2 3 Data RH, UC LH, LC LH, LC RH, UC STATUS X011 00XX X1XX XXXX Data words 003-130 contain LH, UC data; Data words 131-200 contain RH, UC data; STATUS X011 01XX X0XX XXXX Take the channel number modulo 4 Data words 003-130: Channel modulo 4 0 1 2 3 Data RH, LC LH, UC LH, UC RH, LC Data words 131-200: Channel modulo 4 0 1 2 3 Data LH, LC RH, UC RH, UC LH, LC STATUS X011 01XX X1XX XXXX Data words 003-130 contain RH, LC data; Data words 131-200 contain LH, LC data;" OBJECT = INSTMODESECT SECTION_ID = UNK END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO /* */ /* MODE - LEVEL3 */ /* */ OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "LEVEL3" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "N/A" INSTRUMENT_POWER_CONSUMPTION = 6.7 INSTRUMENT_MODE_DESC = " LEVEL3 Data produced every 30 msec; 25 msec of integration. Channel spacing is 307.2 kHz in high band and 19.2 kHz in low band. The lowest high band channel is at 1.3 MHz (cf), and the lowest low band channel is at 1.2 kHz (cf). Bandwidth is 200 kHz in high band, 800 Hz in low band. Polarization does not alternate. STATUS X011 10XX X0XX XXXX Take the channel number modulo 4 Data words 003-130: Channel modulo 4 0 1 2 3 Data LH, UC RH, LC RH, LC LH, UC Data words 131-200: Channel modulo 4 0 1 2 3 Data RH, UC LH, LC LH, LC RH, UC STATUS X011 10XX X1XX XXXX Data words 003-130 contain LH, UC data; Data words 131-200 contain RH, UC data; STATUS X011 11XX X0XX XXXX Take the channel number modulo 4 Data words 003-130: Channel modulo 4 0 1 2 3 Data RH, LC LH, UC LH, UC RH, LC Data words 131-200: Channel modulo 4 0 1 2 3 Data LH, LC RH, UC RH, UC LH, LC STATUS X011 11XX X1XX XXXX Data words 003-130 contain RH, LC data; Data words 131-200 contain LH, LC data;" OBJECT = INSTMODESECT SECTION_ID = UNK END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO /* */ /* MODE - FIXLOL */ /* */ OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "FIXLOL" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "N/A" INSTRUMENT_POWER_CONSUMPTION = 6.7 INSTRUMENT_MODE_DESC = " FIXLOL Data produced every 30 msec; 25 msec of integration. Frequency is fixed. Bandwidth is 1 kHz. STATUS X100 00XX X0XX XXXX Take the channel number modulo 4 Channel modulo 4 0 1 2 3 Data LH, UC LH, LC RH, LC RH, UC STATUS X100 00XX X1XX XXXX Odd numbered data words contain RH, UC data Even numbered data words contain LH, UC data STATUS X100 01XX X0XX XXXX Take the channel number modulo 4 Channel modulo 4 0 1 2 3 Data RH, LC RH, UC LH, UC LH, LC STATUS X100 01XX X1XX XXXX Odd numbered data words contain LH, LC data Even numbered data words contain RH, LC data" OBJECT = INSTMODESECT SECTION_ID = UNK END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO /* */ /* MODE - FIXLOH */ /* */ OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "FIXLOH" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "N/A" INSTRUMENT_POWER_CONSUMPTION = 6.7 INSTRUMENT_MODE_DESC = " FIXLOH Data produced every 30 msec; 25 msec of integration. Frequency is fixed. Bandwidth is 200 kHz. STATUS X100 10XX X0XX XXXX Take the channel number modulo 4 Channel modulo 4 0 1 2 3 Data RH, UC RH, LC LH, LC LH, UC STATUS X100 10XX X1XX XXXX Odd numbered data words contain LH, UC data Even numbered data words contain RH, UC data STATUS X100 11XX X0XX XXXX Take the channel number modulo 4 Channel modulo 4 0 1 2 3 Data LH, LC LH, UC RH, UC RH, LC STATUS X100 11XX X1XX XXXX Odd numbered data words contain RH, LC data Even numbered data words contain LH, LC data" OBJECT = INSTMODESECT SECTION_ID = UNK END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO /* */ /* MODE - VLOBRL */ /* */ OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "VLOBRL" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "N/A" INSTRUMENT_POWER_CONSUMPTION = 6.7 INSTRUMENT_MODE_DESC = " VLOBRL Data produced every 30 msec; 25 msec of integration. Frequency is fixed. Bandwidth is 1 kHz. n/ STATUS X101 00XX X0XX XXXX Odd numbered data words contain LH, LC data Even numbered data words contain RH, UC data STATUS X101 00XX X1XX XXXX All data words contain RH, UC data STATUS X101 01XX X0XX XXXX Odd numbered data words contain RH, UC data Even numbered data words contain LH, LC data STATUS X101 01XX X1XX XXXX All data words contain LH, LC data." OBJECT = INSTMODESECT SECTION_ID = UNK END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO /* */ /* MODE - VLOBRH */ /* */ OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "VLOBRH" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "N/A" INSTRUMENT_POWER_CONSUMPTION = 6.7 INSTRUMENT_MODE_DESC = " VLOBRH Data produced every 30 msec; 25 msec of integration. Frequency is fixed. Bandwidth is 200 kHz. STATUS X101 10XX X0XX XXXX Odd numbered data words contain RH, LC data Even numbered data words contain LH, UC data STATUS X101 10XX X1XX XXXX All data words contain LH, UC data STATUS X101 11XX X0XX XXXX Odd numbered data words contain LH, UC data Even numbered data words contain RH, LC data STATUS X101 11XX X1XX XXXX All data words contain RH, LC data." OBJECT = INSTMODESECT SECTION_ID = UNK END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO /* */ /* MODE - XXXXXL */ /* */ OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "XXXXXL" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "N/A" INSTRUMENT_POWER_CONSUMPTION = 6.7 INSTRUMENT_MODE_DESC = " XXXXXL STATUS X110 1XXX XXXX XXXX No meaningful data are returned because the polarization alternates every 69.4 microseconds, but the RC time constant is 100 microseconds." OBJECT = INSTMODESECT SECTION_ID = UNK END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO /* */ /* MODE - XXXXXH */ /* */ OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "XXXXXH" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "N/A" INSTRUMENT_POWER_CONSUMPTION = 6.7 INSTRUMENT_MODE_DESC = " XXXXXH STATUS X110 0XXX XXXX XXXX No meaningful data are returned because the polarization alternates every 69.4 microseconds, but the RC time constant is 100 microseconds." OBJECT = INSTMODESECT SECTION_ID = UNK END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO /* */ /* MODE - POLHIL */ /* */ OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "POLHIL" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "N/A" INSTRUMENT_POWER_CONSUMPTION = 6.7 INSTRUMENT_MODE_DESC = " POLHIL Data produced every 69.4 microseconds, but sample-and-hold operates once every 138.8 microseconds on both data channels simultaneously (i.e. channels 2n-1 and 2n contain simultaneously sampled data). Integration time is 100 microseconds with an RC circuit (i.e. exponential). Frequency is fixed. Bandwidth is 1 kHz. STATUS X111 00XX X0XX XXXX Odd numbered data words contain LH, LC data Even numbered data words contain RH, UC data STATUS X111 00XX X1XX XXXX All data words contain RH, UC data STATUS X111 01XX X0XX XXXX Odd numbered data words contain RH, UC data Even numbered data words contain LH, LC data STATUS X111 01XX X1XX XXXX All data words contain LH, LC data." OBJECT = INSTMODESECT SECTION_ID = UNK END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO /* */ /* MODE - POLHIH */ /* */ OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "POLHIH" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "N/A" INSTRUMENT_POWER_CONSUMPTION = 6.7 INSTRUMENT_MODE_DESC = " POLHIH Data produced every 69.4 microseconds, but sample-and-hold operates once every 138.8 microseconds on both data channels simultaneously (i.e. channels 2n-1 and 2n contain simultaneously sampled data). Integration time is 100 microseconds with an RC circuit (i.e. exponential). Frequency is fixed. Bandwidth is 200 kHz. STATUS X111 10XX X0XX XXXX Odd numbered data words contain RH, LC data Even numbered data words contain LH, UC data STATUS X111 10XX X1XX XXXX All data words contain LH, UC data STATUS X111 11XX X0XX XXXX Odd numbered data words contain LH, UC data Even numbered data words contain RH, LC data STATUS X111 11XX X1XX XXXX All data words contain RH, LC data." OBJECT = INSTMODESECT SECTION_ID = "PRA" END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = WARWICKETAL1977 OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "INSTRUMENT DESCRIPTION" JOURNAL_NAME = "SPACE SCIENCE REVIEWS" PUBLICATION_DATE = 1977-12-01 REFERENCE_DESC = " Warwick, J. W., J. B. Pearce, R. G. Peltzer and A. C. Riddle, 'Planetary Radio Astronomy Experiment for Voyager Missions', Space Sci Rev., 21, 3, 309, 1977." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. JAMES W. WARWICK" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. JEFFREY B. PEARCE" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "MR. ROBERT G. PELTZER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. ANTHONY C. RIDDLE" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO END_OBJECT = SCINSTRUMENT /******************** PWS Instrument Template *******************************/ /* MODIFICATIONS */ /* From: JPLPDS::RMONARREZ 6-AUG-1992 13:47:39.20 */ /* 92-08 EFRIED */ /* 920916 EFRIED */ /* last changes made */ /* Template: Spacecraft Instrument Template Rev: 19890121 */ /* Note: The following templates form part of a standard */ /* set for the submission of a spacecraft instrument */ /* to the PDS. */ /* Hierarchy: SCINSTRUMENT */ /* INSTINFO */ /* INSTDETECT */ /* INSTELEC */ /* INSTFILTER */ /* INSTOPTICS */ /* SCINSTOFFSET */ /* INSTSECTION */ /* INSTSECTINFO */ /* INSTSECTFOVS */ /* INSTSECTPARM */ /* INSTSECTDET */ /* INSTSECTELEC */ /* INSTSECTFILT */ /* INSTSECTOPTC */ /* INSTMODEINFO */ /* INSTMODESECT */ /* INSTREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCINSTRUMENT SPACECRAFT_ID = VG2 INSTRUMENT_ID = PWS OBJECT = INSTINFO INSTRUMENT_NAME = "PLASMA WAVE RECEIVER" INSTRUMENT_TYPE = "PLASMA WAVE SPECTROMETER" PI_PDS_USER_ID = DGURNETT NAIF_DATA_SET_ID = "N/A" BUILD_DATE = 1976-11-28 INSTRUMENT_MASS = 1.4 INSTRUMENT_HEIGHT = 0.048 INSTRUMENT_LENGTH = 0.318 INSTRUMENT_WIDTH = 0.185 INSTRUMENT_MANUFACTURER_NAME = "THE UNIVERSITY OF IOWA" INSTRUMENT_SERIAL_NUMBER = 3 INSTRUMENT_DESC = " The Plasma Wave Receiver (PWS) on Voyager consists of both a 16-channel spectrum analyzer covering the range of 10 Hertz to 56.2 kiloHertz and a wideband waveform receiver which returns the waveform of waves in the frequency range of 40 Hertz to 12 kiloHertz. The spectrum analyzer provides data on a continual basis with a maximum temporal resolution of one spectrum per 4 seconds. The waveform receiver returns 4-bit samples of the electric field measured at a rate of 28,800 samples per second. Because of the very high data rate, the waveform samples must be transmitted in the same manner as the Voyager imaging information. At Jupiter, some 10,000 48-second waveform frames were obtained. At Saturn, Uranus, and Neptune, the number of frames obtained was very small due to the lower telemetry rates available at the greater distances of those planets." SCIENTIFIC_OBJECTIVES_SUMMARY = " The primary science objective of the Voyager plasma wave investigation is to make the first surveys of the plasma wave and low frequency radio wave spectra in the magnetospheres of the outer planets: Jupiter, Saturn, Uranus, and Neptune. Plasma waves participate in a fundamental manner in the dynamics of planetary magnetospheres and in the interactions of that magnetosphere with the external solar wind and internal perturbations such as those induced by satellites interior to the magnetosphere. Plasma waves also provide diagnostic information about the plasma environment near the planets including such parameters as electron density and sometimes temperature. The instrument is also sensitive to low frequency radio emissions and, therefore, acts as a low frequency extension to the Planetary Radio Astronomy investigation. Radio waves are often the only means of remotely observing regions of plasma not accessible to the spacecraft and also lead to remote diagnostics of plasma conditions. The plasma wave receivers are also sensitive to the results of small dust particles impacting on various parts of the spacecraft at high velocities and, hence, provide a direct measure of the rate of impact, the density of the dust, and an estimate of the mass distribution of dust in the vicinity of the large planets, especially those with rings and otherwise dusty environments. Finally, the Plasma Wave Receiver will characterize the plasma wave and radio wave spectrum of the outer heliosphere and perhaps beyond, extending our understanding of solar wind plasma processes and wave-particle interactions to several tens of Astronomical Units." INSTRUMENT_CALIBRATION_DESC = " The Voyager plasma wave receiver spectrum analyzers were calibrated by first establishing a relationship between input voltage (of a sine wave at the filter center frequency) and output voltage and second by measuring the effective bandwidth of the filter. The bandwidth is measured by applying a random noise signal of known spectral density and by measuring the output voltage which, by the first part of the calibration, is related to the rms voltage of a sine wave. Dividing the equivalent sine wave voltage squared by the input spectral density gives a bandwidth. This procedure is repeated for each of the frequency channels. A special calibration problem exists for the upper 8 frequency channels (1 kiloHertz and above) due to a failure of a 'tree switch' in the Flight Data System. An in-flight recalibration was attempted by using a Solar type III radio burst observed by both Voyager 1 and 2. The recalibration has known deficiencies, but it has been impossible to date to improve on them. The deficiencies include 'flat-topped' emissions where the emission appears to grow in amplitude up to some plateau level and then stay artificially flat for long periods of time. The background level for each of the channels can vary in step-level fashion based on a number of engineering parameters which utilize the same failed circuitry. Other results of the tree-switch recalibration is that the instrument sensitivity is decreased by some amount which is not well known and the absolute calibration could be off as well. The calibration validity could be a function of frequency since some channels' (mostly the upper 3 channels, 17.8 kHz and above) calibration has been verified with the PRA, but others have not and seem internally inconsistent with the lower frequency, unaffected channels." OPERATIONAL_CONSID_DESC = " The primary operational considerations of the Plasma Wave Receiver (PWS) include maintaining the proper operating mode and obtaining waveform samples as often as the spacecraft tape recorder/downlink capabilities allow. The standard instrument mode is with Waveform Power On and Input Gain State Hi. For encounter periods, this corresponds to GS3GAINHI/WFMPWRON. Since there has never been a period when the signal levels were so high as to require the Low input gain state, and it is highly unlikely that such levels will ever be encountered, Low Input Gain State should never be selected. As long as there is power margin available, it is most straightforward to leave the Waveform Receiver Power on. The power consumption is less than 0.5 Watt for this section, hence, the power savings afforded by turning it off is not large. The most involved operational consideration is providing for the transmission of waveform data to the ground. At Jupiter, the majority of the waveform data could be sent directly to the ground via the 115200 bps downlink. This capability disappeared after Jupiter, however, because of the greater distance to the spacecraft, hence, lower telecon rates. Since operating the A/D converter at a rate less than 28800 Hertz would result in aliasing, it is necessary to record the data at the 115200 bps rate on the spacecraft tape recorder using the appropriate data mode and playback the recorded data at a lower rate, commensurate with the link capabilities. Again, a choice of the proper playback mode is required. Since the data modes available on the spacecraft are highly dependent on mission phase, these modes are not described here." END_OBJECT = INSTINFO OBJECT = INSTDETECT DETECTOR_ID = "PWS ANTENNA" DETECTOR_TYPE = "DIPOLE ANTENNA" DETECTOR_ASPECT_RATIO = "N/A" MINIMUM_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" NOMINAL_OPERATING_TEMPERATURE= 298 DETECTOR_DESC = " The Plasma Wave Receiver (PWS) uses a pair of 10 meter antenna elements as a balanced dipole antenna. The two elements are extended from the spacecraft at right angles to each other. (The elements are shared with the Planetary Radio Astronomy instrument, which uses them as a pair of monopoles so that measurements of the degree of right and left hand circular polarization can be made.) The PWS measures the voltage difference between the two elements which, when coupled with the effective length of the antenna system (7.07 m) yields an electric field strength in units of volt/meter. The antenna system has the usual dipole antenna pattern which yields nearly 4*pi steradians in its field of view, although there is a range of fields of view where the detector response drops dramatically as one expects from a dipole pattern." SENSITIVITY_DESC = " The Plasma Wave Receiver (PWS) antenna, used as a balanced dipole with an effective length of 7.07 meters gives a sensitivity to fluctuating (wave) electric fields down to the range of 5.E-6 volt/meter. Even though the antenna elements are extended orthogonally to each other, the antenna pattern is still a dipole since the elements are short with respect to the wavelengths of the waves. The presence of the various parts of the spacecraft in close proximity to the antenna can result in a distorted pattern, but this has not been studied in the frequency range of the PWS." END_OBJECT = INSTDETECT OBJECT = INSTELEC ELECTRONICS_ID = PWS ELECTRONICS_DESC = " The Plasma Wave Receiver (PWS) electronics system consists of three basic sections. The first is the power supply system which regulates and filters the 28 volt, 2400 Hertz spacecraft power supply and provides DC voltages to the remainder of the instrument electronics. The second section is the spectrum analyzer which consists of two banks of 8 narrowband filters, and two logarithmic detectors, each of which provides an analog voltage proportional to the log of the signal strength delivered to the detector from any of the eight filters it services. The analog outputs from these two compressors, as they are called, are sent to the Flight Data System of the spacecraft for conversion to an 8-bit digital value. The spacecraft steps the inputs to the two compressors periodically (once per 0.5 seconds in GS3 or encounter mode) so that signal strengths in each of the 16 channels is measured over a 4-second interval. The third section consists of a single broadband filter of 40 Hertz to 12 kiloHertz, an automatic gain controlled amplifier, and a 4-bit A/D converter. This section digitizes the electric field waveform at a 28800 Hertz rate. The output amplitude is controlled by the automatic gain control in order to keep the signals within the useful range provided by the 4-bit digitization." END_OBJECT = INSTELEC OBJECT = INSTFILTER FILTER_NUMBER = "N/A" FILTER_NAME = "N/A" FILTER_TYPE = "N/A" MINIMUM_WAVELENGTH = "N/A" CENTER_FILTER_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" MEASUREMENT_WAVE_CALBRT_DESC= "N/A" END_OBJECT = INSTFILTER OBJECT = INSTOPTICS TELESCOPE_ID = "N/A" TELESCOPE_FOCAL_LENGTH = "N/A" TELESCOPE_DIAMETER = "N/A" TELESCOPE_F_NUMBER = "N/A" TELESCOPE_RESOLUTION = "N/A" TELESCOPE_TRANSMITTANCE = "N/A" TELESCOPE_T_NUMBER = "N/A" TELESCOPE_T_NUMBER_ERROR = "N/A" TELESCOPE_SERIAL_NUMBER = "N/A" OPTICS_DESC = "N/A" END_OBJECT = INSTOPTICS OBJECT = SCINSTOFFSET PLATFORM_OR_MOUNTING_NAME = "SPACECRAFT BUS" CONE_OFFSET_ANGLE = "N/A" CROSS_CONE_OFFSET_ANGLE = "N/A" TWIST_OFFSET_ANGLE = "N/A" INSTRUMENT_MOUNTING_DESC = " The Plasma Wave Receiver (PWS) is mounted on top of the Planetary Radio Astronomy (PRA) experiment on top of spacecraft bus bays 8 and 9. The two orthogonal antenna elements are attached to the Planetary radio astronomy package." END_OBJECT = SCINSTOFFSET OBJECT = INSTSECTION SECTION_ID = SA OBJECT = INSTSECTINFO SCAN_MODE_ID = "N/A" DATA_RATE = 32 SAMPLE_BITS = 8 TOTAL_FOVS = 1 OBJECT = INSTSECTFOVS FOV_SHAPE_NAME = DIPOLE HORIZONTAL_PIXEL_FOV = "N/A" VERTICAL_PIXEL_FOV = "N/A" HORIZONTAL_FOV = 360 VERTICAL_FOV = 180 FOVS = 1 END_OBJECT = INSTSECTFOVS END_OBJECT = INSTSECTINFO OBJECT = INSTSECTPARM INSTRUMENT_PARAMETER_NAME = "WAVE ELECTRIC FIELD INTENSITY" MINIMUM_INSTRUMENT_PARAMETER = 0.000005 MAXIMUM_INSTRUMENT_PARAMETER = 0.5 NOISE_LEVEL = 0.000005 INSTRUMENT_PARAMETER_UNIT = "VOLT/METER" SAMPLING_PARAMETER_NAME = TIME MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 4.0 SAMPLING_PARAMETER_RESOLUTION = 4.0 SAMPLING_PARAMETER_UNIT = SECOND END_OBJECT = INSTSECTPARM OBJECT = INSTSECTDET DETECTOR_ID = "PWS ANTENNA" END_OBJECT = INSTSECTDET OBJECT = INSTSECTELEC ELECTRONICS_ID = PWS END_OBJECT = INSTSECTELEC OBJECT = INSTSECTFILT FILTER_NUMBER = "N/A" END_OBJECT = INSTSECTFILT OBJECT = INSTSECTOPTC TELESCOPE_ID = "N/A" END_OBJECT = INSTSECTOPTC END_OBJECT = INSTSECTION OBJECT = INSTSECTION SECTION_ID = WFRM OBJECT = INSTSECTINFO SCAN_MODE_ID = "N/A" DATA_RATE = 115200 SAMPLE_BITS = 4 TOTAL_FOVS = 1 OBJECT = INSTSECTFOVS FOV_SHAPE_NAME = DIPOLE HORIZONTAL_PIXEL_FOV = "N/A" VERTICAL_PIXEL_FOV = "N/A" HORIZONTAL_FOV = 360 VERTICAL_FOV = 180 FOVS = 1 END_OBJECT = INSTSECTFOVS END_OBJECT = INSTSECTINFO OBJECT = INSTSECTPARM INSTRUMENT_PARAMETER_NAME = "ELECTRIC FIELD COMPONENT" MINIMUM_INSTRUMENT_PARAMETER = 0.000005 MAXIMUM_INSTRUMENT_PARAMETER = 0.5 NOISE_LEVEL = 0.000005 INSTRUMENT_PARAMETER_UNIT = "VOLT/METER" SAMPLING_PARAMETER_NAME = TIME MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 0.0000347 SAMPLING_PARAMETER_RESOLUTION = 0.0000347 SAMPLING_PARAMETER_UNIT = SECOND END_OBJECT = INSTSECTPARM OBJECT = INSTSECTDET DETECTOR_ID = "PWS ANTENNA" END_OBJECT = INSTSECTDET OBJECT = INSTSECTELEC ELECTRONICS_ID = PWS END_OBJECT = INSTSECTELEC OBJECT = INSTSECTFILT FILTER_NUMBER = "N/A" END_OBJECT = INSTSECTFILT OBJECT = INSTSECTOPTC TELESCOPE_ID = "N/A" END_OBJECT = INSTSECTOPTC END_OBJECT = INSTSECTION OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "GS3GAINHI/WFMPWRON" GAIN_MODE_ID = "HIGH" DATA_PATH_TYPE = "REALTIME" INSTRUMENT_POWER_CONSUMPTION = 1.6 INSTRUMENT_MODE_DESC = " The Plasma Wave Receiver (PWS) instrument gain is high and the waveform receiver power is on. This is the normal encounter operating mode of the instrument and places it in its most sensitive input gain state with the waveform receiver section turned on. The fact that the waveform receiver power is on does not guarantee that waveform data is available. The spacecraft is in the GS-3 data mode which cycles the plasma wave spectrum analyzer so that a complete spectrum is obtained every 4 seconds." OBJECT = INSTMODESECT SECTION_ID = SA END_OBJECT = INSTMODESECT OBJECT = INSTMODESECT SECTION_ID = WFRM END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "GS3GAINHI/WFMPWRON" GAIN_MODE_ID = "HIGH" DATA_PATH_TYPE = "RECORDED DATA PLAYBACK" INSTRUMENT_POWER_CONSUMPTION = 1.6 INSTRUMENT_MODE_DESC = " The PWS instrument gain is high and the waveform receiver power is on. This is the normal encounter operating mode of the instrument and places it in its most sensitive input gain state with the waveform receiver section turned on. The fact that the waveform receiver power is on does not guarantee that waveform data is available. The spacecraft is in the GS-3 data mode which cycles the plasma wave spectrum analyzer so that a complete spectrum is obtained every 4 seconds." OBJECT = INSTMODESECT SECTION_ID = SA END_OBJECT = INSTMODESECT OBJECT = INSTMODESECT SECTION_ID = WFRM END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = SCARF&GURNETT1977 OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "INSTRUMENT DESCRIPTION" JOURNAL_NAME = "SPACE SCIENCE REVIEWS" PUBLICATION_DATE = 1977-12-01 REFERENCE_DESC = " Scarf, F. L., and D. A. Gurnett, A plasma wave investigation for the Voyager mission, Space Sci. Rev., 21, 289, 1977." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. FREDERICK L. SCARF" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. DONALD A. GURNETT" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO END_OBJECT = SCINSTRUMENT /******************* Uranus CRS 96 Second D1 Rate Data Set ********************/ /* MODIFICATIONS */ /* 920831 -- JPLPDS::RMONARREZ */ /* received by ftp */ /* 920914 -- EFRIED */ /* 920918 -- EFRIED */ /* updated Data Set templates according to new std. */ /* Data Set Template -> Spacecraft Data Set Template */ /* event_start_time, event_stop_time -> start_time, stop_time */ /* 920922 -- EFRIED */ /* Changed DATA_SET_ID and DATA_SET_NAME */ /* Included references for Science, J. of G. */ /* 920925 -- RMONARREZ */ /* Updated PROCESSING_LEVEL_ID to match DATA_SET_ID */ /* last changes made */ /* Template: Spacecraft Data Set Template - Rev: 19890121*/ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-CRS-4-SUMM-D1-96SEC-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA CRS RESAMPLED SUMMARY D1 RATE ELEC 96SEC V1.0" DATA_SET_COLLECTION_MEMBER_FLG = N START_TIME = 1986-01-24T10:00:00.000 STOP_TIME = 1986-01-25T00:00:00.000 NATIVE_START_TIME = "N/A" NATIVE_STOP_TIME = "N/A" DATA_OBJECT_TYPE = "TIME SERIES" DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = 4 PRODUCER_FULL_NAME = "RICHARD S. SELESNICK" PRODUCER_INSTITUTION_NAME = "CALIFORNIA INSTITUTE OF TECHNOLOGY" SOFTWARE_FLAG = "N" DETAILED_CATALOG_FLAG = "Y" PROCESSING_START_TIME = "UNK" PROCESSING_STOP_TIME = "UNK" DATA_SET_DESC = " This data set describes data of the counting rate from the D1 detector in the Cosmic Ray System (CRS) electron telescope (TET) on Voyager 2 during the Uranus encounter. The D1 detector nominally responds to electrons with kinetic energies above approximately 1 MeV (see detector description for details). Note that the instrument is saturated near the maximum of counting rate of approximately 50,000 counts / sec between approximately 1986-01-24T18:10:50Z and 1986-01-24T19:02:02Z. When they are near saturation, the counting rates should be corrected for deadtime according to the formula in the DATA_SET_OR_INST_PARM_DESC: {corrected rate} = {uncorrected rate/(1+deadtime*{uncorrected rate})." CONFIDENCE_LEVEL_NOTE = " Each data point represents a six-second accumulation, so that the statistical uncertainty is obtained according to Poisson statistics by taking the square root of one sixth of the counting rate. However, larger uncertainties are associated with the conversion from counting rate to flux (see the DATA_SET_OR_INST_PARM_DESC)" END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = "URANUS" END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = "TIME" SAMPLING_PARAMETER_RESOLUTION = 6.0 MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 96.0 MINIMUM_AVAILABLE_SAMPLING_INT = 96.0 SAMPLING_PARAMETER_UNIT = "SECOND" DATA_SET_PARAMETER_NAME = "D1 RATE" NOISE_LEVEL = 0.000 DATA_SET_PARAMETER_UNIT = "COUNTS/SECOND" END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = "VG2" INSTRUMENT_ID = "CRS" END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = "STONEETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "CRS URANUS REPORT" JOURNAL_NAME = "SCIENCE" PUBLICATION_DATE = 1986-07-04 REFERENCE_DESC = " Stone, E.C., J.F. Cooper, A.C. Cummings, F.B. McDonald, J.H. Trainor, N. Lal, R. McGuire, D.L. Chenette, Energetic Charged Particles in the Uranian Magnetosphere, Science, 233, 93-97, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "E. C. STONE" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "J. F. COOPER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "A. C. CUMMINGS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "F. B. MCDONALD" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "J. H. TRAINOR" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N. LAL" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R. MCGUIRE" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "D. L. CHENETTE" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "SELESNICK&STONE1991C" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "CRS URANUS ANALYSIS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1991-04-01 REFERENCE_DESC = " Selesnick, R. S., E. C. Stone, 'Energetic Electrons at Uranus: Bimodal Diffusion in a Satellite Limited Radiation Belt', Journal of Geophysical Research, 96 (No. A4), 5651-5665, 1991." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R. S. SELESNICK" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "E. C. STONE" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "COOPER&STONE1991" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "CRS URANUS ANALYSIS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1991-05-01 REFERENCE_DESC = " Cooper, J.F., E.C. Stone, Electron Signatures of Satellite Sweeping in the Magnetosphere of Uranus, Journal of Geophysical Research, 96 (No. A5), 7803-7821." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "J. F. COOPER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "E. C. STONE" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /*********************** Uranus CRS 96 Second D2 Rate Data Set ****************/ /* MODIFICATIONS */ /* 920831 -- JPLPDS::RMONARREZ */ /* received by ftp */ /* 920914 -- EFRIED */ /* 920918 -- EFRIED */ /* updated Data Set templates according to new std. */ /* Data Set Template -> Spacecraft Data Set Template */ /* event_start_time, event_stop_time -> start_time, stop_time */ /* 920922 -- EFRIED */ /* Changed DATA_SET_ID and DATA_SET_NAME */ /* Included full reference for Science and J. of G. */ /* 920925 -- RMONARREZ */ /* Updated PROCESSING_LEVEL_ID to match DATA_SET_ID */ /* last changes made */ /* Template: Spacecraft Data Set Template - Rev: 19890121*/ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-CRS-4-SUMM-D2-96SEC-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA CRS RESAMPLED SUMMARY D2 RATE ELEC 96SEC V1.0" DATA_SET_COLLECTION_MEMBER_FLG = N START_TIME = 1986-01-24T10:00:00.000 STOP_TIME = 1986-01-25T00:00:00.000 NATIVE_START_TIME = "N/A" NATIVE_STOP_TIME = "N/A" DATA_OBJECT_TYPE = "TIME SERIES" DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = 4 PRODUCER_FULL_NAME = "RICHARD S. SELESNICK" PRODUCER_INSTITUTION_NAME = "CALIFORNIA INSTITUTE OF TECHNOLOGY" SOFTWARE_FLAG = "N" DETAILED_CATALOG_FLAG = "Y" PROCESSING_START_TIME = "UNK" PROCESSING_STOP_TIME = "UNK" DATA_SET_DESC = " Counting rate from the D2 detector in the Cosmic Ray System (CRS) electron telescope (TET) on Voyager 2 during the Uranus encounter. The D2 detector nominally responds to electrons with kinetic energies above approximately 2.5 MeV (see detector description for details)." CONFIDENCE_LEVEL_NOTE = " Each data point represents a six-second accumulation, so that the statistical uncertainty is obtained according to Poisson statistics by taking the square root of one sixth of the counting rate. However, larger uncertainties are associated with the conversion from counting rate to flux (see the DATA_SET_OR_INST_PARM_DESC)" END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = "URANUS" END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = "TIME" SAMPLING_PARAMETER_RESOLUTION = 6.0 MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 96.0 MINIMUM_AVAILABLE_SAMPLING_INT = 96.0 SAMPLING_PARAMETER_UNIT = "SECOND" DATA_SET_PARAMETER_NAME = "D2 RATE" NOISE_LEVEL = 0.000 DATA_SET_PARAMETER_UNIT = "COUNTS/SECOND" END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = "VG2" INSTRUMENT_ID = "CRS" END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = "STONEETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "CRS URANUS REPORT" JOURNAL_NAME = "SCIENCE" PUBLICATION_DATE = 1986-07-04 REFERENCE_DESC = " Stone, E.C., J.F. Cooper, A.C. Cummings, F.B. McDonald, J.H. Trainor, N. Lal, R. McGuire, D. L. Chenette, Energetic Charged Particles in the Uranian Magnetosphere, 233, 93-97, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "E. C. STONE" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "J. F. COOPER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "A. C. CUMMINGS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "F. B. MCDONALD" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "J. H. TRAINOR" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N. LAL" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R. MCGUIRE" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "D. L. CHENETTE" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "SELESNICK&STONE1991" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "CRS URANUS ANALYSIS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1991-04-01 REFERENCE_DESC = " Selesnick. R.S., E.C. Stone, Energetic Electrons at Uranus: Bimodal Diffusion in a Satellite Limited Radiation Belt, Journal of Geophysical Research, 96 (No. A4), 5651-5665, 1991." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R. S. SELESNICK" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "E. C. STONE" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "COOPER&STONE1991" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "CRS URANUS ANALYSIS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1991-05-01 REFERENCE_DESC = " Cooper, J.F., E.C. Stone, Electron Signatures of Satellite Sweeping in the Magnetosphere of Uranus, Journal of Geophysical Research, 96 (No. A5), 7803-7821, 1991." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "J. F. COOPER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "E. C. STONE" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /*************** D1 DSPROC Template ******************************************/ /* MODIFICATIONS */ /* 920914 -- EFRIED */ /* 920922 -- EFRIED */ /* Revised PRODUCT_DATA_SET_ID */ /* Last changes made */ /* Template: Data Set Processing Template Rev: 19890121 */ /* */ /* Note: This template shall be repeated for each */ /* source dataset id used in production of the */ /* dataset id in the dataset template. */ /* */ /* Hierarchy: DSPROCESSING */ OBJECT = DSPROCESSING SOURCE_DATA_SET_ID = "N/A" SOFTWARE_NAME = "ENCYCLOPEDIA GENERATOR" PRODUCT_DATA_SET_ID = "VG2-U-CRS-4-SUMM-D1-96SEC-V1.0" END_OBJECT = DSPROCESSING /*************** D1 DSPROC Template *******************************************/ /* MODIFICATIONS */ /* 920914 -- EFRIED */ /* 920922 -- EFRIED */ /* Revised PRODUCT_DATA_SET_ID */ /* Last changes made */ /* Template: Data Set Processing Template Rev: 19890121 */ /* */ /* Note: This template shall be repeated for each */ /* source dataset id used in production of the */ /* dataset id in the dataset template. */ /* */ /* Hierarchy: DSPROCESSING */ OBJECT = DSPROCESSING SOURCE_DATA_SET_ID = "N/A" SOFTWARE_NAME = "VCRUSH" PRODUCT_DATA_SET_ID = "VG2-U-CRS-4-SUMM-D1-96SEC-V1.0" END_OBJECT = DSPROCESSING /***************** D2 DSPROC Template *****************************************/ /* MODIFICATIONS */ /* 920914 -- EFRIED */ /* 920922 -- EFRIED */ /* Revised PRODUCT_DATA_SET_ID */ /* Last changes made */ /* Template: Data Set Processing Template Rev: 19890121 */ /* */ /* Note: This template shall be repeated for each */ /* source dataset id used in production of the */ /* dataset id in the dataset template. */ /* */ /* Hierarchy: DSPROCESSING */ OBJECT = DSPROCESSING SOURCE_DATA_SET_ID = "N/A" SOFTWARE_NAME = "ENCYCLOPEDIA GENERATOR" PRODUCT_DATA_SET_ID = "VG2-U-CRS-4-SUMM-D2-96SEC-V1.0" END_OBJECT = DSPROCESSING /******************** D2 DSPROC Template **************************************/ /* MODIFICATIONS */ /* 920914 -- EFRIED */ /* 920922 -- EFRIED */ /* Revised PRODUCT_DATA_SET_ID */ /* Last changes made */ /* Template: Data Set Processing Template Rev: 19890121 */ /* */ /* Note: This template shall be repeated for each */ /* source dataset id used in production of the */ /* dataset id in the dataset template. */ /* */ /* Hierarchy: DSPROCESSING */ OBJECT = DSPROCESSING SOURCE_DATA_SET_ID = "N/A" SOFTWARE_NAME = "VCRUSH" PRODUCT_DATA_SET_ID = "VG2-U-CRS-4-SUMM-D2-96SEC-V1.0" END_OBJECT = DSPROCESSING /********************* D1 Rate Parameter Information **************************/ /* MODIFICATIONS: */ /* 920806 JPLPDS::RMONARREZ */ /* received by mail */ /* 92-08 EFRIED */ /* 920916 EFRIED */ /* last changes made */ /* Template: Parameter Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID = "VG1" DATA_SET_PARAMETER_NAME = "D1 RATE" INSTRUMENT_PARAMETER_NAME = "D1 RATE" IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER OBJECT = PARAMETER INSTRUMENT_HOST_ID = "VG2" DATA_SET_PARAMETER_NAME = "D1 RATE" INSTRUMENT_PARAMETER_NAME = "D1 RATE" IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /********************** D1 Rate Parameter Description *************************/ /* MODIFICATIONS: */ /* 920806 JPLPDS::RMONARREZ */ /* received by mail */ /* 92-08 EFRIED */ /* 920916 EFRIED */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM = "D1 RATE" DATA_SET_OR_INST_PARM_DESC = " The D1 rate is the counting rate from the D1 detector of the Cosmic Ray System (CRS) electron telecope (TET). When the rate is above background it is approximately proportional to the omnidirectional flux of electrons with kinetic energy greater than ~1 MeV. To obtain an accurate flux the D1 calibration tables should be used (see below). When the rate is near background, the background rate should be subtracted. The background rate is due to gamma rays generated in the spacecraft RTG and to penetrating cosmic rays. It varies slightly with time on the time scale of months, but is generally near 25 counts per second. When the rate is near saturation, corrections for discriminator deadtime should be made. The discriminator deadtime is approximately 20 micro-seconds (it varies slightly with the electron energy spectrum), so that the saturation level is approximately 50,000 counts per second. When the correction is near a factor of two or less a reliable corrected rate can be obtained from the formula {corrected rate} = {uncorrected rate}/(1+deadtime*{uncorrected rate}) When the deadtime correction is substantially larger than a factor of two, reliable corrections are not available. In this case, electron pileup and baseline shift may also be important, which may increase or decrease the expected rate. The data points are 6 second averages taken once every 96 seconds. The table below provides the D1 response function R(E,theta) which is a function of electron energy E in MeV (column at left) and angle theta in degrees from the TET axis (row at top). Each table entry is R in cm**2 for the corresponding E and theta. The D1 electron rate is related to the differential intensity j(E,alpha) in (cm**2 s sr MeV)**-1, where alpha is the electron pitch-angle, by integrating the product R*j over E and solid angle. Note that the angle between the TET axis and the local magnetic field direction is also required. The D1 RATE is then obtained by adding the background rate and applying the inverse of the deadtime correction described above. At energies above the maximum provided R can be approximated by the value at the highest provided energy. At angles above the maximum provided R can be approximated by zero. D1 response function: | 11. 15. 23. 32. 41. 51. 61. ______|________________________________________________ | 0.618 | 0.014 0.005 0.007 0.007 0.006 0.003 0.001 0.801 | 0.151 0.134 0.103 0.087 0.038 0.016 0.008 0.989 | 1.384 1.440 1.219 0.998 0.610 0.311 0.143 1.179 | 2.233 2.402 2.095 1.796 1.255 0.689 0.380 1.372 | 2.829 2.938 2.593 2.241 1.636 0.956 0.583 1.567 | 3.212 3.283 2.936 2.536 1.940 1.167 0.724 1.763 | 3.495 3.534 3.206 2.772 2.161 1.356 0.860 1.959 | 3.708 3.705 3.404 2.964 2.357 1.495 0.969 2.157 | 3.620 3.790 3.452 3.053 2.427 1.602 1.049 2.355 | 3.995 3.948 3.576 3.231 2.617 1.758 1.155 2.553 | 4.096 4.091 3.735 3.395 2.735 1.875 1.263 2.752 | 4.154 4.098 3.808 3.426 2.792 1.927 1.298 2.951 | 4.043 4.054 3.727 3.371 2.819 1.951 1.339 3.150 | 3.946 4.029 3.700 3.335 2.648 1.956 1.358 3.350 | 3.876 4.194 3.611 3.573 2.863 1.927 1.290 | 70. 80. 90. 100. ______|____________________________ | 0.618 | 0.002 0.001 0.000 0.000 0.801 | 0.010 0.007 0.004 0.001 0.989 | 0.163 0.095 0.047 0.018 1.179 | 0.386 0.217 0.113 0.056 1.372 | 0.526 0.301 0.163 0.087 1.567 | 0.617 0.366 0.201 0.117 1.763 | 0.679 0.413 0.241 0.146 1.959 | 0.730 0.461 0.270 0.179 2.157 | 0.760 0.484 0.296 0.207 2.355 | 0.809 0.518 0.329 0.242 2.553 | 0.836 0.551 0.363 0.292 2.752 | 0.856 0.564 0.392 0.319 2.951 | 0.845 0.548 0.401 0.348 3.150 | 0.837 0.559 0.400 0.374 3.350 | 0.792 0.486 0.440 0.375" END_OBJECT = DSINSTPARMD /******************* D2 Rate Parameter Information ****************************/ /* MODIFICATIONS: */ /* 920806 JPLPDS::RMONARREZ */ /* received by mail */ /* 92-08 EFRIED */ /* 920916 EFRIED */ /* last changes made */ /* Template: Parameter Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID = "VG1" DATA_SET_PARAMETER_NAME = "D2 RATE" INSTRUMENT_PARAMETER_NAME = "D2 RATE" IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER OBJECT = PARAMETER INSTRUMENT_HOST_ID = "VG2" DATA_SET_PARAMETER_NAME = "D2 RATE" INSTRUMENT_PARAMETER_NAME = "D2 RATE" IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /************************ D2 Rate Parameter Description ***********************/ /* MODIFICATIONS: */ /* 920806 JPLPDS::RMONARREZ */ /* received by mail */ /* 92-08 EFRIED */ /* 920916 EFRIED */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM = "D2 RATE" DATA_SET_OR_INST_PARM_DESC = " The D2 detector is located behind the D1 detector in the TET telescope, so that most of the electrons observed by D2 have to penetrate D1 first. The D2 rate therefore applies to higher energy electrons and the threshold energy is less distinct than for D1, but is near 2.5 MeV. The rate can be calculated from the electron differential flux in the same way as the D1 RATE (see D1 RATE description) with the following calibration table. D2 response function: | 11. 23. 41. 61. 80. 90. 100. ________|_________________________________________________ | 0.989 | 0.000 0.000 0.000 0.001 0.002 0.001 0.001 1.179 | 0.000 0.000 0.000 0.013 0.023 0.021 0.018 1.372 | 0.000 0.000 0.000 0.037 0.052 0.051 0.043 1.567 | 0.000 0.019 0.028 0.063 0.082 0.066 0.061 1.763 | 0.041 0.034 0.045 0.090 0.111 0.098 0.080 1.959 | 0.106 0.078 0.072 0.119 0.142 0.125 0.097 2.157 | 0.255 0.186 0.127 0.152 0.170 0.146 0.109 2.355 | 0.488 0.381 0.228 0.206 0.212 0.176 0.126 2.553 | 0.772 0.627 0.361 0.272 0.255 0.202 0.139 2.752 | 1.019 0.864 0.501 0.340 0.299 0.226 0.152 2.951 | 1.220 1.053 0.634 0.400 0.335 0.250 0.165 3.150 | 1.461 1.218 0.746 0.459 0.375 0.289 0.188 3.350 | 1.628 1.378 0.940 0.515 0.456 0.411 0.282" END_OBJECT = DSINSTPARMD /********************** Encyclopedia Generator Software Information ***********/ /* MODIFICATIONS: */ /* 920806 JPLPDS::RMONARREZ */ /* 92-08 EFRIED */ /* 920917 EFRIED */ /* last changes made */ /* Template: Software Information Template Rev: 19890121 */ /* */ /* Note: This template is completed for each node */ /* software application referenced in the PDS. */ /* */ /* Hierarchy: SOFTWARE */ OBJECT = SOFTWARE SOFTWARE_NAME = "ENCYCLOPEDIA GENERATOR" NODE_ID = "N/A" SOFTWARE_RELEASE_DATE = "N/A" SOFTWARE_TYPE = "N/A" COGNIZANT_FULL_NAME = "NAND LAL" SOFTWARE_ACCESSIBILITY_DESC = "N/A" SOFTWARE_DESC = " This program is run by Nand Lal at Goddard Space Flight Center. It reads the EDR tape, checks for error conditions, and reformats the data to generate a CRS encyclopedia tape, which is sent to CalTech for subsequent data analysis. Note: THIS SOFTWARE IS NOT FOR PUBLIC USE." END_OBJECT = SOFTWARE /******************** VCRUSH Software Information *****************************/ /* MODIFICATIONS: */ /* 920806 JPLPDS::RMONARREZ */ /* received by mail */ /* 92-08 EFRIED */ /* 920916 EFRIED */ /* last changes made */ /* Template: Software Information Template Rev: 19890121 */ /* */ /* Note: This template is completed for each node */ /* software application referenced in the PDS. */ /* */ /* Hierarchy: SOFTWARE */ OBJECT = SOFTWARE SOFTWARE_NAME = "VCRUSH" NODE_ID = "N/A" SOFTWARE_RELEASE_DATE = "N/A" SOFTWARE_TYPE = "N/A" COGNIZANT_FULL_NAME = "THOMAS L. GARRARD" SOFTWARE_ACCESSIBILITY_DESC = "N/A" SOFTWARE_DESC = " The VCRUSH program is run at CalTech to select data of interest from CRS encyclopedia tapes. In the case of counting rate data, no further analysis is done to produce the data in the PDS data sets. Note: THIS SOFTWARE IS NOT FOR PUBLIC USE." END_OBJECT = SOFTWARE /********************** Uranus LECP Calib. Browse 15 Minute Data ************/ /* MODIFICATIONS */ /* 920831 -- JPLPDS::RMONARREZ */ /* received by ftp */ /* 920914 -- EFRIED */ /* 920918 -- EFRIED */ /* updated Data Set templates according to new std. */ /* Data Set Template -> Spacecraft Data Set Template */ /* event_start_time, event_stop_time -> start_time, stop_time */ /* 920924 -- EFRIED */ /* Changed DATA_SET_ID and DATA_SET_NAME */ /* last changes made */ /* Template: Spacecraft Data Set Template - Rev: 19890121*/ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-LECP-4-SUMM-AVERAGE-15MIN-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA LECP RESAMPLED SUMMARY SCAN AVERAGED 15MIN V1.0" DATA_SET_COLLECTION_MEMBER_FLG = N START_TIME = 1986-01-24T00:00:00.000 STOP_TIME = 1986-01-30T00:00:00.000 NATIVE_START_TIME = UNK NATIVE_STOP_TIME = UNK DATA_OBJECT_TYPE = "TIME SERIES" DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = "4" PRODUCER_FULL_NAME = "BARRY H. MAUK" PRODUCER_INSTITUTION_NAME = "JOHNS HOPKINS UNIVERSITY APPLIED PHYSICS LABORATORY" SOFTWARE_FLAG = "Y" DETAILED_CATALOG_FLAG = "Y" PROCESSING_START_TIME = 1987-02-01 PROCESSING_STOP_TIME = "N/A" DATA_SET_DESC = " This browse data consists of resampled data from the Low Energy Charged Particle (LECP) experiment on Voyager 2 while the spacecraft was in the vicinity of Uranus. This instrument measures the intensities of in-situ charged particles (>26 keV electrons and >30 keV ions) with various levels of discrimination based on energy, mass species, and angular arrival direction. A subset of almost 100 LECP channels are included with this data set. The LECP data are globally calibrated to the extent possible (see below) and they are time averaged to about 15 minute time intervals with the exact beginning and ending times for those intervals matching the LECP instrumental cycle periods (the angular scanning periods). The LECP instrument has a rotating head for obtaining angular anisotropy measurements of the medium energy charged particles that it measures. The cycle time for the rotation if variable, but during encounters it is always faster than 15 minutes. For this browse data set only scan average data is given (no angular information). The data is in the form of 'rate' data which has not been converted to the usual physical units. The reason is that such a conversion would depend on uncertain determinations such as the mass species of the particles and the level of background. Both mass species and background are generally determined from context during the study of particular regions. To convert 'rate' to 'intensity' for a particular channel one performs the following tasks: 1) decide on the level of background contamination and subtract that off the given rate level. Background is to be determined from context and from making use of sector 8 rates (sector 8 has a 2 MM al shield covering it). 2) divide the background corrected rate by the channel geometric factor and by the energy bandpass of the channel. The geometric factor is found in entry 'CHANNEL_GEOMETRIC_FACTOR' as associated with each channel 'CHANNEL_ID'. To determine the energy bandpass, one must judge the mass species of the of the detected particles (for ions but not for electrons). The energy band passes are given in entries 'MINIMUM_INSTRUMENT_PARAMETER' and 'MAXIMUM_INSTRUMENT_PARAMETER' in table 'FPLECPENERGY', and are given in the form 'ENERGY/NUCLEON'. For channels that begin their names with the designations 'CH' these bandpasses can be used on mass species that are accepted into that channel (see entries 'MINIMUM_INSTRUMENT_PARAMETER' and 'MAXIMUM_INSTRUMENT_ PARAMETER' in table 'FPLECPCHANZ', which give the minimum and maximum 'Z' value accepted -- these entries are blank for electron channels). For other channels the given bandpass refers only to the lowest 'Z' value accepted. The bandpasses for other 'Z' values are not all known, but some are given in the literature (e.g. Krimigis et al., 1979). The final product of these instructions will be the particle intensity with the units: counts/(cm**2.str.sec.keV). Some channels are subject to serious contaminations, and many of these contaminations cannot be removed except with a region-by-region analysis, which has not been done for this data. Thus, to use this data it is absolutely vital that the contamination types ('CONTAMINATION_ID' , 'CONTAMINATION_DESC') and the levels of contamination ('DATA_QUALITY_ID' corresponding to the definitions 'DATA_QUALITY_DESC') be carefully examined for all regions of study. A dead time correction procedure has been applied in an attempt to correct the linear effects of detector overdrive (Pulse-Pileup). This procedure does not fix severely overdriven detectors. A procedure is available for correcting Voyager 2 LECP electron contamination of low energy ion channels, but its effectiveness has been evaluated only for the Uranus data set. THUs, corrections have been applied only to the Uranus data set." CONFIDENCE_LEVEL_NOTE = " At all times during this planetary encounter there exist data in this data set that can be rated with the highest confidence level. However, some of the channels of data are contaminated by various kinds and various levels of contaminations. It is therefore imperative, in using this data set, that the contamination tables within the catalog be examined. Also, not all kinds of contamination have been fully documented. when in doubt the data supplier must be contacted." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = "URANUS" END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = "TIME" SAMPLING_PARAMETER_RESOLUTION = 15.000000 MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 15.000000 MINIMUM_AVAILABLE_SAMPLING_INT = "N/A" SAMPLING_PARAMETER_UNIT = "MINUTE" DATA_SET_PARAMETER_NAME = "ELECTRON RATE" NOISE_LEVEL = 0.000000 DATA_SET_PARAMETER_UNIT = "COUNTS/SECOND" END_OBJECT = DSPARMINFO OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = "TIME" SAMPLING_PARAMETER_RESOLUTION = 15.000000 MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 15.000000 MINIMUM_AVAILABLE_SAMPLING_INT = "N/A" SAMPLING_PARAMETER_UNIT = "MINUTE" DATA_SET_PARAMETER_NAME = "ION RATE" NOISE_LEVEL = 0.000000 DATA_SET_PARAMETER_UNIT = "COUNTS/SECOND" END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = "VG2" INSTRUMENT_ID = "LECP" END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = "KRIMIGISETAL1977" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "LECP DOCUMENTATION" JOURNAL_NAME = "SPACE SCIENCE REVIEWS" PUBLICATION_DATE = 1977 REFERENCE_DESC = " Krimigis, S.M., T.P. Armstrong, W.I. Axford, C.O. Bostrom, C.Y. Fan, G. Gloeckler, and L.J. Lanzerotti, Low Energy Charged Particle (LECP) Experiment On the Voyager Spacecraft, Space Science Reviews, 21, 329 1977." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. S. M. KRIMIGIS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "MAUKETAL1987" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "LECP URANUS DOCUMENTATION" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1987 REFERENCE_DESC = " Mauk, B.H., S.M. Krimigis, E.P. Keath, A.F. Cheng, T.P. Armstrong, L.J. Lanzerotti, G. Gloeckler, and D.C. Hamilton, The Hot Plasma and Radiation Environment of the Uranian Magnetosphere, Journal of Geophysical Research, 92, 15283, 1987." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. BARRY H. MAUK" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /********************** Uranus LECP Calib. 15 Minute Data *********************/ /* MODIFICATIONS */ /* 920831 -- JPLPDS::RMONARREZ */ /* received by ftp */ /* 920914 -- EFRIED */ /* 920918 -- EFRIED */ /* updated Data Set templates according to new std. */ /* Data Set Template -> Spacecraft Data Set Template */ /* event_start_time, event_stop_time -> start_time, stop_time */ /* 920924 -- EFRIED */ /* Revised DATA_SET_ID and DATA_SET_NAME */ /* last changes made */ /* Template: Spacecraft Data Set Template - Rev: 19890121*/ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-LECP-4-RDR-SECTOR-15MIN-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA LECP RESAMPLED RDR STEPPING SECTOR 15MIN V1.0" DATA_SET_COLLECTION_MEMBER_FLG = N START_TIME = 1986-01-24T00:00:00.000 STOP_TIME = 1986-01-30T00:00:00.000 NATIVE_START_TIME = UNK NATIVE_STOP_TIME = UNK DATA_OBJECT_TYPE = "TIME SERIES" DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = "4" PRODUCER_FULL_NAME = "BARRY H. MAUK" PRODUCER_INSTITUTION_NAME = "JOHNS HOPKINS UNIVERSITY APPLIED PHYSICS LABORATORY" SOFTWARE_FLAG = "Y" DETAILED_CATALOG_FLAG = "Y" PROCESSING_START_TIME = 1987-02-01 PROCESSING_STOP_TIME = "N/A" DATA_SET_DESC = " This data set consists of resampled data from the Low Energy Charged Particle (LECP) experiment on Voyager 2 while the spacecraft was in the vicinity of Uranus. This instrument measures the intensities of in-situ charged particles (>26 keV electrons and >30 keV ions) with various levels of discrimination based on energy, mass species, and angular arrival direction. A subset of almost 100 LECP channels are included with this data set. The LECP data are globally calibrated to the extent possible (see below) and they are time averaged to about 15 minute time intervals with the exact beginning and ending times for those intervals matching the LECP instrumental cycle periods (the angular scanning periods). The LECP instrument has a rotating head for obtaining angular anisotropy measurements of the medium energy charged particles that it measures. The cycle time for the rotation if variable, but during encounters it is always faster than 15 minutes. Thus, the full angular anisotropy information is preserved with this data. The data is in the form of 'Rate' data which has not been converted to the usual physical units. The reason is that such a conversion would depend on uncertain determinations such as the mass species of the particles and the level of background. Both mass species and background are generally determined from context during the study of particular regions. To convert 'Rate' to 'Intensity' for a particular channel one performs the following tasks: 1) Decide on the level of background contamination and subtract that off the given rate level. Background is to be determined from context and from making use of sector 8 rates (sector 8 has a 2 mm Al shield covering it). 2) Divide the background corrected rate by the channel geometric factor and by the energy bandpass of the channel. The geometric factor is found in entry 'CHANNEL_GEOMETRIC_FACTOR' as associated with each channel 'CHANNEL_ID'. To determine the energy bandpass, one must judge the mass species of the of the detected particles (for ions but not for electrons). The energy band passes are given in entries 'MINIMUM_INSTRUMENT_PARAMETER' and 'MAXIMUM_INSTRUMENT_PARAMETER' in table 'FPLECPENERGY', and are given in the form 'Energy/Nucleon'. For channels that begin their names with the designations 'CH' these bandpasses can be used on mass species that are accepted into that channel (see entries 'MINIMUM_INSTRUMENT_PARAMETER' and 'MAXIMUM_INSTRUMENT_ PARAMETER' in table 'FPLECPCHANZ', which give the minimum and maximum 'Z' value accepted -- these entries are blank for electron channels). For other channels the given bandpass refers only to the lowest 'Z' value accepted. The bandpasses for other 'Z' values are not all known, but some are given in the literature (e.g. Krimigis et al., 1979). The final product of these instructions will be the particle intensity with the units: counts/(cm**2.str.sec.keV). Some channels are subject to serious contaminations, and many of these contaminations cannot be removed except with a region-by-region analysis, which has not been done for this data. thus, to use this data it is absolutely vital that the contamination types ('CONTAMINATION_ID' , 'CONTAMINATION_DESC') and the levels of contamination ('DATA_QUALITY_ID' corresponding to the definitions 'DATA_QUALITY_DESC') be carefully examined for all regions of study. A dead time correction procedure has been applied in an attempt to correct the linear effects of detector overdrive (pulse-pileup). This procedure does not fix severely overdriven detectors. A procedure is available for correcting Voyager 2 LECP electron contamination of low energy ion channels, but its effectiveness has been evaluated only for the Uranus data set. Thus, corrections have been applied only to the Uranus data set. Also included with this data are one standard deviation statistical uncertainties for the directional data (sectors 1 through 8) expressed as a percent. Unknown values are generally coded as such, however in some instances the value will read 'ZERO' when its status is unknown." CONFIDENCE_LEVEL_NOTE = " At all times during this planetary encounter there exist data in this data set that can be rated with the highest confidence level. However, some of the channels of data are contaminated by various kinds and various levels of contaminations. It is therefore imperative, in using this data set, that the contamination tables within the catalog be examined. Also, not all kinds of contamination have been fully documented. When in doubt the data supplier must be contacted." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = "URANUS" END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = "TIME" SAMPLING_PARAMETER_RESOLUTION = 15.000000 MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 15.000000 MINIMUM_AVAILABLE_SAMPLING_INT = "N/A" SAMPLING_PARAMETER_UNIT = "MINUTE" DATA_SET_PARAMETER_NAME = "ELECTRON RATE" NOISE_LEVEL = 0.000000 DATA_SET_PARAMETER_UNIT = "COUNTS/SECOND" END_OBJECT = DSPARMINFO OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = "TIME" SAMPLING_PARAMETER_RESOLUTION = 15.000000 MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 15.000000 MINIMUM_AVAILABLE_SAMPLING_INT = "N/A" SAMPLING_PARAMETER_UNIT = "MINUTE" DATA_SET_PARAMETER_NAME = "ION RATE" NOISE_LEVEL = 0.000000 DATA_SET_PARAMETER_UNIT = "COUNTS/SECOND" END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = "VG2" INSTRUMENT_ID = "LECP" END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = "KRIMIGISETAL1977" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "LECP DOCUMENTATION" JOURNAL_NAME = "SPACE SCIENCE REVIEWS" PUBLICATION_DATE = 1977 REFERENCE_DESC = " Krimigis, S.M., T.P. Armstrong, W.I. Axford, C.O. Bostrom, C.Y. Fan, G. Gloeckler, and L.J. Lanzerotti, The Low Energy Charged Particle (LECP) Experiment On the Voyager Spacecraft, Space Science Reviews, 21, 329 1977." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. S. M. KRIMIGIS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "MAUKETAL1987" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "LECP URANUS DOCUMENTATION" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1987 REFERENCE_DESC = " Mauk, B.H., S.M. Krimigis, E.P. Keath, A.F. Cheng, T.P. Armstrong, L.J. Lanzerotti, G. Gloeckler, D.C. Hamilton, The Hot Plasma and Radiation Environment of the Uranian Magnetosphere, Journal of Geophysical Research, 92, 15283, 1987." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. BARRY H. MAUK" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /*********** Uranus LECP Stepping Sector 12.8 Minute Data ********************/ /* MODIFICATIONS */ /* 920831 -- JPLPDS::RMONARREZ */ /* received by ftp */ /* 920914 -- EFRIED */ /* 920918 -- EFRIED */ /* updated Data Set templates according to new std. */ /* Data Set Template -> Spacecraft Data Set Template */ /* event_start_time, event_stop_time -> start_time, stop_time */ /* 920924 -- EFRIED */ /* Revised DATA_SET_ID and DATA_SET_NAME */ /* last changes made */ /* Template: Spacecraft Data Set Template - Rev: 19890121*/ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-LECP-4-RDR-STEP-12.8MIN-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA LECP RESAMPLED RDR STEPPING SECTOR 12.8MIN V1.0" DATA_SET_COLLECTION_MEMBER_FLG = N START_TIME = 1986-01-24T00:00:00.000 STOP_TIME = 1986-01-27T00:00:00.000 NATIVE_START_TIME = "N/A" NATIVE_STOP_TIME = "N/A" DATA_OBJECT_TYPE = "TIME SERIES" DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = 4 PRODUCER_FULL_NAME = "DR. BARRY MAUK" PRODUCER_INSTITUTION_NAME = "JOHNS HOPKINS APPLIED PHYSICS LABORATORY" SOFTWARE_FLAG = N DETAILED_CATALOG_FLAG = Y PROCESSING_START_TIME = 1991-07-24 PROCESSING_STOP_TIME = 1991-07-25 DATA_SET_DESC = " Description of the PDS LECP Uranus Step data. This data consists of resampled data from the Low Energy Charged Particle (LECP) Experiment on the Voyager 2 Spacecraft for the period when Voyager 2 was in the vicinity of the planet Uranus. The period covered is 1989/day 24/0000 SCET to 1989/day 27/0000 SCET. This data gives scan plane angle distributions for those periods when the LECP instrument was mechanically scanning. There are periods when the instrument was not scanning, and the corresponding data does not appear here with this Step data. Another data set that is available, the so called Scan data, contains data for these not stepping periods as well as angle averaged data for the stepping periods. The instrument samples 8 directional sectors during a single scan, and thus this Step data contains 8 particle intensity numbers for each channel of data utilized (a ninth sector corresponds to accumulations for which the sector is unknown). Two scanning situations occurred during the time of this data. They are: 1) continuous 48 sec stepping (48 seconds for each of 8 look directions for a total of 6.4 minutes per scan; note that sector 8 is shielded with 2 mm Al), and 2) a special Uranus scan cyclic with the following sequence: 7, scan, scan, 7, scan, scan, repeat; where the 7 represents a 10.4 minute period when the instrument is fixed in sector 7, and where the word scan represents a period of scanning (6 sec stepping for a total scan time of 48 sec). For this Uranus Scan data the two adjacent scans within the Uranus scan cyclic (Mode 2 above) have been averaged together into a single, 96 sec record. The records of the 48 sec stepping mode (mode 1 above) are for 6.4 minutes. The schedule of mode changes is as follows: prior to day 24/ 0420 SCET: Mode (1) 24/0420 to 25/1357: Mode (2) after 25/1357: Mode (1) Please note that the change-over between modes is not instantaneous, and that for a few minutes the state of the scanning is not regular. Note also that there were brief interruptions to, and changes in time phase in, the mode (2) scan cyclic during the transitions into and out of the movable block period that bracketed the close approach position (not shown above). Obviously these stepping mode changes, and the angle sample switching that occurs during stepping mode (2), gives the data a disjointed appearance. The LECP channels utilized with this data set are: EB01: electrons, 22 to 35 keV EB02: electrons, 35 to 61 keV EB03: electrons, 61 to 112 keV EB04: electrons, 112 to 183 keV EG06-EG07: electrons, 252 to 480 keV EG07-EG08: electrons, 480 to 853 keV EG08-EG09: electrons, 853 to 1200 keV PL01: ions, 28 to 43 keV PL02: ions, 43 to 80 keV PL03: ions, 80 to 137 keV PL04: ions, 137 to 215 keV PL05: ions, 215 to 540 keV PL06: ions, 540 to 990 keV PL07: ions, 990 to 2140 keV PL08: ions, 2140 to 3500 keV Please note that 3 of the electron channels are derived from 4 of the instrumental channels by taking differences between adjacent (in energy) channels. The channel data is given in units of intensity: counts/(cm^2.sec.str.keV). For the ions, it has been assumed that they consist only of protons. Intensity is derived from the raw count rates via the relation: I = CR/(eG.(E2-E1), where eG is geometric factor times detector efficiency, and (E2-E1) is the band pass of the channel in energy. The proton values of these parameters were used in deriving the intensities for this data set. To obtain the Intensities under the assumption that some other mass species dominates, one must convert back to count rate (CR) utilizing the proton parameters, and then convert to intensity using the parameters corresponding to the mass species in question. The parameters can be found in Table 1 of Krimigis et al. (Journal of Geophysical Research, V. 86, page 8227, 1981). The corresponding parameters for electrons can be found in Mauk et al. (Journal of Geophysical Research, V. 92, page 15283, 1987). Prior to the conversion to intensity, the count rates have been corrected for: (1) Background, (2) electron contamination of the lower energy ion channels, and (3) solar UV contamination of the lowest energy ion channel. The uncertainty parameters given with the data associated with each channel (expressed as a percent) is the largest of the two quantities: (i) one standard deviation Poisson statistical error, and (ii) a percentage assigned by the data supplier based on the amount of contamination correction that has been performed on each data channel. Also supplied with each record of this data set is the fraction of the data accumulations that correspond to each of the 8 angle sectors. A sector 9 has also been defined corresponding to those accumulations with no known sector assignment. Additionally supplied for each data channel is a one bit code that tells whether that channel had any accumulations at all associated with it (1 = yes; 0 = no). This code must be used to distinguish between accumulations that yielded no counts and situations where the channel simply had no accumulations (results in Intensity = 0.0)." CONFIDENCE_LEVEL_NOTE = " Confidence note for the PDS Uranus LECP Step data. High quality data is available from the LECP instrument throughout the time period addressed with this data set. The data is subject to errors associated with Poisson statistics and associated with various kinds and levels of contamination. The known contaminations are: i) penetrating background, ii) Solar UV contamination within the lowest energy ion channel when the detector faces sunward, and iii) electron contamination of the lower energy ion channels (the contaminating electrons are measured). Corrections have been made to the data in attempts to remove the effects of these contaminations. An error parameter is given for each particle intensity value given in the data set. This error is expressed as a percentage. This number is the larger of the following items: 1) the one standard deviation Poisson error, and 2) a value assigned by the data supplier associated with the degree of correction that was required with regard to the contaminations listed above. Missing data is indicated with a binary flag associated with each energy channel. Each channel's flag will read 1 if at least one instrumental accumulation occurred for that channel and for that record. The flag reads 0 for no accumulations. This parameter must be utilized to distinguish between accumulations that yielded no counts, and the situation where there simply were no accumulations (the error parameter reads 100 for both cases)." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = URANUS END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = 768. MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 768. MINIMUM_AVAILABLE_SAMPLING_INT = 6. SAMPLING_PARAMETER_UNIT = SECOND DATA_SET_PARAMETER_NAME = "PARTICLE FLUX INTENSITY" NOISE_LEVEL = "N/A" DATA_SET_PARAMETER_UNIT = "COUNTS/(CM**2*SECOND*STERRADIAN*KEV)" END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = VG2 INSTRUMENT_ID = LECP END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = KRIMIGISETAL1989 OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "ENERGETIC PARTICLES AT NEPTUNE" JOURNAL_NAME = SCIENCE PUBLICATION_DATE = 1989-12-15 REFERENCE_DESC = " Krimigis, S.M., T.P. Armstrong, W.I. Axford, C.O. Bostrom, A.F. Cheng, G. Gloeckler, D.C. Hamilton, E.P. Keath, L.J. Lanzerotti, B. H. Mauk, J.A. Van Allen, Hot Plasma and Energetic Particles in Neptune's Magnetosphere, Science, 246, 1483, 1989" OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "S. (TOM) KRIMIGIS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "THOMAS P. ARMSTRONG" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "BARRY H. MAUK" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = KRIMIGISETAL1990 OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "ENERGETIC PARTICLES AT NEPTUNE" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH LETTERS" PUBLICATION_DATE = 1990 REFERENCE_DESC = " Krimigis, S.M., B.H. Mauk, A.F. Cheng, E.P. Keath, M. Kane, T.P. Armstrong, G. Gloeckler, L.J. Lanzerotti, Hot Plasma Parameters in Neptune's Magnetosphere, Geophys. Res. Lett., 17, 1685, 1990." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "S. (TOM) KRIMIGIS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "THOMAS P. ARMSTRONG" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "BARRY H. MAUK" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = MAUKETAL1987 OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "ENERGETIC PARTICLES AT URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1987 REFERENCE_DESC = " Mauk, B.H., S.M. Krimigis, E.P. Keath, A.F. Cheng, T.P. Armstrong, L.J. Lanzerotti, G. Gloeckler, D.C. Hamilton, The Hot Plasma and Radiation Environment of the Uranian Magnetosphere, J. Geophys, Res., 92, 15283, 1987." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "BARRY H. MAUK" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "S. (TOM) KRIMIGIS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "THOMAS P. ARMSTRONG" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = KRIMIGISETAL1981 OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "ENERGETIC PARTICLES AT JUPITER" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1981 REFERENCE_DESC = " Krimigis, S.M., J.F. Carbary, E.P. Keath, C.O. Bostrom, W.I. Axford, G. Gloeckler, L.J. Lanzerotti, and T.P. Armstrong, Characteristics of Hot Plasma in the Jovian Magnetosphere: Results from the Voyager Spacecraft, J. Geophys. Res., 86, 8227, 1981." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "S. (TOM) KRIMIGIS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "THOMAS P. ARMSTRONG" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /************* Uranus LECP Summ Scan Average 24 Second Data ******************/ /* MODIFICATIONS */ /* 920831 -- JPLPDS::RMONARREZ */ /* received by ftp */ /* 920914 -- EFRIED */ /* 920918 -- EFRIED */ /* updated Data Set templates according to new std. */ /* Data Set Template -> Spacecraft Data Set Template */ /* event_start_time, event_stop_time -> start_time, stop_time */ /* 920924 -- EFRIED */ /* Revised DATA_SET_ID and DATA_SET_NAME */ /* last changes made */ /* Template: Spacecraft Data Set Template - Rev: 19890121*/ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-LECP-4-SUMM-SCAN-24SEC-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA LECP RESAMPLED SUMMARY SCAN AVERAGED 24SEC V1.0" DATA_SET_COLLECTION_MEMBER_FLG = N START_TIME = 1989-01-24T00:00:00.000 STOP_TIME = 1989-01-27T00:00:00.000 NATIVE_START_TIME = "N/A" NATIVE_STOP_TIME = "N/A" DATA_OBJECT_TYPE = "TIME SERIES" DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = 4 PRODUCER_FULL_NAME = "DR. BARRY MAUK" PRODUCER_INSTITUTION_NAME = "JOHNS HOPKINS APPLIED PHYSICS LABORATORY" SOFTWARE_FLAG = Y DETAILED_CATALOG_FLAG = Y PROCESSING_START_TIME = 1991-07-24 PROCESSING_STOP_TIME = 1991-07-25 DATA_SET_DESC = " Description of the PDS LECP Uranus Scan data. This data consists of resampled data from the Low Energy Charged Particle (LECP) Experiment on the Voyager 2 Spacecraft for the period when Voyager 2 was in the vicinity of the planet Uranus. The period covered is 1986/day 24/0000 SCET to 1986/day 27/0000 SCET. This data approximates a time series of charged particle fluxes from a selection of channels available from the instrument. The word approximates is used because the angle scanning modes of the instrument complicates the nature of the data. At times the instrument mechanically scans, and at times it is fixed to look at a specific direction. With the type of data given here, the fluxes are angle averaged for those time periods when the instrument is scanning, and are time averaged over an arbitrary period (24 seconds) for the periods when the detectors are stationary. The angle averaged records represent periods of time equal to 96 or 384 sec (see below). This kind of data presentation has been called the LECP Scan data. Another form that is also available is the LECP Step data that gives the angle distributions sampled during the scanning periods. Two scanning situations occurred during the time of this data. They are: 1) continuous 48 sec stepping (48 seconds for each of 8 look directions for a total of 6.4 minutes per scan; note that sector 8 is shielded with 2 mm Al), and 2) a special Uranus scan cyclic with the following sequence: 7, scan, scan, 7, scan, scan, repeat; where the 7 represents a 10.4 minute period when the instrument is fixed in sector 7, and where the word scan represents a period of scanning (6 sec stepping for a total scan time of 48 sec). For this Uranus Scan data the two adjacent scans within the Uranus scan cyclic have been averaged together into a single, 96 sec record. The records of the 48 sec stepping mode (Mode 1 above) are for 6.4 minutes. As stated in the first paragraph, the records for the periods of no stepping during the Uranus scan cyclic (mode 2 above) are for 24 sec periods. The schedule of mode changes is as follows: prior to day 24/0420: Mode (1) 24/0420 to 25/ 1357: Mode (2) after day 25/1357: Mode (1) Please note that the change-over between modes is not instantaneous, and that for a few minutes the state of the scanning is not regular. Not also that there were brief interruptions to, and changes in time phase in, the Mode (2) scan cyclic during the transitions into and out of the movable block periods that bracketed the close approach position (not shown above). Obviously these stepping mode changes, and the angle sample switching that occurs during stepping mode (2), gives the data a disjointed appearance. The LECP channels utilized with this data set are: EB01: electrons, 22 to 35 keV EB02: electrons, 35 to 61 keV EB03: electrons, 61 to 112 keV EB04: electrons, 112 to 183 keV EG06-EG07: electrons, 252 to 480 keV EG07-EG08: electrons, 480 to 853 keV EG08-EG09: electrons, 853 to 1200 keV PL01: ions, 28 to 43 keV PL02: ions, 43 to 80 keV PL03: ions, 80 to 137 keV PL04: ions, 137 to 215 keV PL05: ions, 215 to 540 keV PL06: ions, 540 to 990 keV PL07: ions, 990 to 2140 keV PL08: ions, 2140 to 3500 keV Please note that 3 of the electron channels are derived from 4 of the instrumental channels by taking differences between adjacent (in energy) channels. The channel data is given in units of intensity: counts/(cm^2.sec.str.keV). For the ions, it has been assumed that they consist only of protons. Intensity is derived from the raw count rates via the relation: I = CR/(eG.(E2-E1), where eG is geometric factor times detector efficiency, and (E2-E1) is the band pass of the channel in energy. The proton values of these parameters were used in deriving the intensities for this data set. To obtain the Intensities under the assumption that some other mass species dominates, one must convert back to count rate (CR) utilizing the proton parameters, and then convert to intensity using the parameters corresponding to the mass species in question. The parameters can be found in Table 1 of Krimigis et al. (Journal of Geophysical Research, V. 86, page 8227, 1981). The corresponding parameters for electrons can be found in Mauk et al. (Journal of Geophysical Research, V. 92, page 15283, 1987). Prior to the conversion to intensity, the count rates have been corrected for: (1) Background, (2) electron contamination of the lower energy ion channels, and (3) solar UV contamination of the lowest energy ion channel. The uncertainty parameters given with the data associated with each channel (expressed as a percent) is the largest of the two quantities: (i) one standard deviation Poisson statistical error, and (ii) a percentage assigned by the data supplier based on the amount of contamination correction that has been performed on each data channel. Also supplied with each record of this data set is the fraction of the data accumulations that correspond to each of the 8 angle sectors. For example, during a sector 7 stow period, this number will be 1.0 for sector 7 and 0.0 for all of the other sectors. A sector 9 has also been defined corresponding to those accumulations with no known sector assignment. Additionally supplied for each data channel is a one bit code that tells whether that channel had any accumulations at all associated with it (1 = yes; 0 = no). This code must be used to distinguish between accumulations that yielded no counts and situations where the channel simply had no accumulations (results in Intensity = 0.0).<" CONFIDENCE_LEVEL_NOTE = " Confidence note for the PDS Uranus LECP Scan data. High quality data is available from the LECP instrument throughout the time period addressed with this data set. The data is subject to errors associated with Poisson statistics and associated with various kinds and levels of contamination. The known contaminations are: i) penetrating background, ii) Solar UV contamination within the lowest energy ion channel when the detector faces sunward, and iii) electron contamination of the lower energy ion channels (the contaminating electrons are measured). Corrections have been made to the data in attempts to remove the effects of these contaminations. An error parameter is given for each particle intensity value given in the data set. This error is expressed as a percentage. This number is the larger of the following items: 1) the one standard deviation Poisson error, and 2) a value assigned by the data supplier associated with the degree of correction that was required with regard to the contaminations listed above. Missing data is indicated with a binary flag associated with each energy channel. Each channel's flag will read 1 if at least one instrumental accumulation occurred for that channel and for that record. The flag reads 0 for no accumulations. This parameter must be utilized to distinguish between accumulations that yielded no counts, and the situation where there simply were no accumulations (the error parameter reads 100 for both cases)." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = URANUS END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = 24.0 MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 24.0 MINIMUM_AVAILABLE_SAMPLING_INT = 6.0 SAMPLING_PARAMETER_UNIT = SECOND DATA_SET_PARAMETER_NAME = "PARTICLE FLUX INTENSITY" NOISE_LEVEL = "N/A" DATA_SET_PARAMETER_UNIT = "COUNTS/(CM**2*SECOND*STERRADIAN*KEV)" END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = VG2 INSTRUMENT_ID = LECP END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = MAUKETAL1987 OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "ENERGETIC PARTICLES AT URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1987 REFERENCE_DESC = " Mauk, B.H., S.M. Krimigis, E.P. Keath, A.F. Cheng, T.P. Armstrong, L.J. Lanzerotti, G. Gloeckler, D.C. Hamilton, The Hot Plasma and Radiation Environment of the Uranian Magnetosphere, J. Geophys, Res., 92, 15283, 1987." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "BARRY H. MAUK" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "S. (TOM) KRIMIGIS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "THOMAS P. ARMSTRONG" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = KRIMIGISETAL1981 OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "ENERGETIC PARTICLES AT JUPITER" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1981 REFERENCE_DESC = " Krimigis, S.M., J.F. Carbary, E.P. Keath, C.O. Bostrom, W.I. Axford, G. Gloeckler, L.J. Lanzerotti, and T.P. Armstrong, Characteristics of Hot Plasma in the Jovian Magnetosphere: Results from the Voyager Spacecraft, J. Geophys. Res., 86, 8227, 1981." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "S. (TOM) KRIMIGIS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "THOMAS P. ARMSTRONG" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /********************* Electron Rate Parameter *******************************/ /* MODIFICATIONS */ /* 920805 -- SJOY from RMONARREZ 920527 */ /* received by mail */ /* 920916 -- EFRIED */ /* last changes made */ /* Template: Parameter Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID = "VG2" DATA_SET_PARAMETER_NAME = "ELECTRON RATE" INSTRUMENT_PARAMETER_NAME = "ELECTRON RATE" IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /******** Data Set Instrument Parameter Desc. - Elec. Rate ********************/ /* MODIFICATIONS */ /* 920805 -- SJOY from RMONARREZ 920527 */ /* received by mail */ /* revised capitalization (UP -> LC) */ /* 920916 -- EFRIED */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM = "ELECTRON RATE" DATA_SET_OR_INST_PARM_DESC = " A measured parameter equaling the number of electrons hitting a particle detector per specified accumulation interval. The counted electrons may or may not be discriminated as to their energies (e.g. greater than E1, or between E1 and E2)." END_OBJECT = DSINSTPARMD /********************************* ION Rate Parameter ************************/ /* MODIFICATIONS */ /* 920805 -- SJOY from RMONARREZ 920527 */ /* received by mail */ /* 920916 -- EFRIED */ /* last changes made */ /* Template: Parameter Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID = "VG2" DATA_SET_PARAMETER_NAME = "ION RATE" INSTRUMENT_PARAMETER_NAME = "ION RATE" IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /************** Data Set Instrument Parameter Desc. - Ion Rate ****************/ /* MODIFICATIONS */ /* 920805 -- SJOY from RMONARREZ 920527 */ /* received by mail */ /* revised capitalization (UC -> LC) */ /* 920916 -- EFRIED */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM = "ION RATE" DATA_SET_OR_INST_PARM_DESC = " A measured parameter equaling the number of ions striking a particle detector per specified accumulation interval. The counted ions may or may not be discriminated as to their energies (e.g. energy/nucleon or energy/charge between E1 and E2 or greater than E1) and/or as to their ion composition (atomic number Z or mass number greater than Z1 or M1, or between Z1 and z2 or M1 and M2)." END_OBJECT = DSINSTPARMD /****************** Particle Parameter Information ****************************/ /* MODIFICATIONS: */ /* 921001 -- EFRIED */ /* created template */ /* last changes made */ /* Template: Parameter Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID = "VG2" DATA_SET_PARAMETER_NAME = "PARTICLE FLUX INTENSITY" INSTRUMENT_PARAMETER_NAME = "PARTICLE MULTIPLE PARAMETERS" IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /************* Particle Flux Intensity Parameter Description ******************/ /* MODIFICATIONS: */ /* 921001 EFRIED */ /* created template */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM = "PARTICLE FLUX INTENSITY" DATA_SET_OR_INST_PARM_DESC = " The channel data is given in units of intensity: counts/(cm^2.sec.str.keV). For the ions, it has been assumed that they consist only of protons. Intensity is derived from the raw count rates via the relation: I = CR/(eG.(E2-E1), where eG is geometric factor times detector efficiency, and (E2-E1) is the band pass of the channel in energy. The proton values of these parameters were used in deriving the intensities for this data set. To obtain the Intensities under the assumption that some other mass species dominates, one must convert back to count rate (CR) utilizing the proton parameters, and then convert to intensity using the parameters corresponding to the mass species in question. The parameters can be found in Table 1 of Krimigis et al. (Journal of Geophysical Research, V. 86, page 8227, 1981). The corresponding parameters for electrons can be found in Mauk et al. (Journal of Geophysical Research, V. 92, page 15283, 1987). Prior to the conversion to intensity, the count rates have been corrected for: (1) Background, (2) electron contamination of the lower energy ion channels, and (3) solar UV contamination of the lowest energy ion channel." END_OBJECT = DSINSTPARMD /************* Particle Multiple Parameter Description ************************/ /* MODIFICATIONS: */ /* 921001 EFRIED */ /* created template */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM = "PARTICLE MULTIPLE PARAMETERS" DATA_SET_OR_INST_PARM_DESC = " A set of measured parameters which yield multiple pieces of information about each particle (generally ions) that enters the system. These pieces of information can, for example, consist of the energy deposited by a single particle in two or more separate detectors, or the time-of-flight between two different detectors plus the energy deposited in a third, etc.. The multiple pieces of information can be used to perform mass, atomic number, and/or charge state discriminations on ions. The information can be discriminated on-board and telemetered in the form of ion rate channels, or the multiple information about each particle analyzed can be telemetered for obtaining the finest species discriminations." END_OBJECT = DSINSTPARMD /*********************** HG COORDS TEMPLATE ***********************************/ /* MODIFICATIONS: */ /* 921028 -- SJOY */ /* created template */ /* 921125 -- EFRIED */ /* last modification */ /* Template: Coordinate System Template Rev: 19890121 */ /* Note: The following templates form part of a standard */ /* set for the submission of a Coordinate System */ /* to the PDS. */ /* Hierarchy: COORDINATE */ /* COORDINFO */ /* VECTOR */ /* VECTORCOMP */ /* VECTORD */ OBJECT = COORDINATE COORDINATE_SYSTEM_ID = HG OBJECT = COORDINFO COORDINATE_SYSTEM_NAME = "MEAN INERTIAL HG 1950" COORDINATE_SYSTEM_CENTER_NAME = SUN COORDINATE_SYSTEM_REF_EPOCH = "UNK" /* 09-23-1950 */ COORDINATE_SYSTEM_DESC = " The Heliographic coordinate system is defined in the reference epoch of 1950. The unit vectors which define the coordinate system are as follows: X points away from the Sun towards the ascending node, in the solar equatorial plane, Z points along the Sun's spin axis, positive above the equatorial plane, and Y completes the right handed set." END_OBJECT = COORDINFO OBJECT = VECTOR VECTOR_COMPONENT_TYPE = RANGE OBJECT = VECTORCOMP VECTOR_COMPONENT_ID = R REFERENCE_OBJECT_NAME = SUN REFERENCE_TARGET_NAME = SPACECRAFT VECTOR_COMPONENT_UNIT = AU END_OBJECT = VECTORCOMP OBJECT = VECTORD VECTOR_COMPONENT_TYPE_DESC = " The range or R component of the spherical Heliographic coordinate system is the distance from the Sun's position at the reference epoch to the spacecraft measured in AU." END_OBJECT = VECTORD END_OBJECT = VECTOR OBJECT = VECTOR VECTOR_COMPONENT_TYPE = LATITUDE OBJECT = VECTORCOMP VECTOR_COMPONENT_ID = LAT REFERENCE_OBJECT_NAME = SUN REFERENCE_TARGET_NAME = SPACECRAFT VECTOR_COMPONENT_UNIT = DEGREES END_OBJECT = VECTORCOMP OBJECT = VECTORD VECTOR_COMPONENT_TYPE_DESC = " The latitude component of the the spherical Heliographic coordinate system is the angle between the solar equatorial plane of the reference epoch measured in the plane that contains the solar spin axis of that epoch." END_OBJECT = VECTORD END_OBJECT = VECTOR OBJECT = VECTOR VECTOR_COMPONENT_TYPE = LONGITUDE OBJECT = VECTORCOMP VECTOR_COMPONENT_ID = LONG REFERENCE_OBJECT_NAME = SUN REFERENCE_TARGET_NAME = SPACECRAFT VECTOR_COMPONENT_UNIT = DEGREES END_OBJECT = VECTORCOMP OBJECT = VECTORD VECTOR_COMPONENT_TYPE_DESC = " The longitude component of the spherical Heliographic coordinate system is zero in the direction of the ascending node at the reference epoch (X direction) and increases for a body orbiting the Sun as the Earth does." END_OBJECT = VECTORD END_OBJECT = VECTOR OBJECT = VECTOR VECTOR_COMPONENT_TYPE = X OBJECT = VECTORCOMP VECTOR_COMPONENT_ID = X REFERENCE_OBJECT_NAME = SUN REFERENCE_TARGET_NAME = "ASCENDING NODE" VECTOR_COMPONENT_UNIT = AU END_OBJECT = VECTORCOMP OBJECT = VECTORD VECTOR_COMPONENT_TYPE_DESC = " The X component of the Heliographic coordinate system points away from the Sun, towards the ascending node, and lies in the solar equatorial plane." END_OBJECT = VECTORD END_OBJECT = VECTOR OBJECT = VECTOR VECTOR_COMPONENT_TYPE = Y OBJECT = VECTORCOMP VECTOR_COMPONENT_ID = Y REFERENCE_OBJECT_NAME = SUN REFERENCE_TARGET_NAME = "N/A" VECTOR_COMPONENT_UNIT = AU END_OBJECT = VECTORCOMP OBJECT = VECTORD VECTOR_COMPONENT_TYPE_DESC = " The Y vector of the Heliographic coordinate system is formed by the righthanded cross product of the X and Z unit vectors. It lies in the solar equatorial plane and it points away from the Sun, but does not extend in the direction of any particular body." END_OBJECT = VECTORD END_OBJECT = VECTOR OBJECT = VECTOR VECTOR_COMPONENT_TYPE = Z OBJECT = VECTORCOMP VECTOR_COMPONENT_ID = Z REFERENCE_OBJECT_NAME = SUN REFERENCE_TARGET_NAME = "SUN SPIN AXIS" VECTOR_COMPONENT_UNIT = AU END_OBJECT = VECTORCOMP OBJECT = VECTORD VECTOR_COMPONENT_TYPE_DESC = " The Z component of the Heliographic coordinate system is parallel to the Sun's spin axis, taken as positive above the equatorial plane of the Sun." END_OBJECT = VECTORD END_OBJECT = VECTOR END_OBJECT = COORDINATE /*********************** U1 COORDS TEMPLATE ***********************************/ /* MODIFICATIONS: */ /* 921028 -- SJOY */ /* created template */ /* Template: Coordinate System Template Rev: 19890121 */ /* Note: The following templates form part of a standard */ /* set for the submission of a Coordinate System */ /* to the PDS. */ /* Hierarchy: COORDINATE */ /* COORDINFO */ /* VECTOR */ /* VECTORCOMP */ /* VECTORD */ OBJECT = COORDINATE COORDINATE_SYSTEM_ID = U1 OBJECT = COORDINFO COORDINATE_SYSTEM_NAME = "URANUS WEST LONGITUDE SYSTEM" COORDINATE_SYSTEM_CENTER_NAME = "URANUS" COORDINATE_SYSTEM_REF_EPOCH = "UNK" /* 1986-01-24:18:00:00.000 */ COORDINATE_SYSTEM_DESC = " Planetary longitudes are based on a 17.24 hour rotation period (Connerney et al., 1987) adopted by the Voyager Project shortly after the encounter. The zero longitude is defined by the requirement that the West Longitude of the spacecraft at 1800 SCET day 24 (near closest approach) be 302 degrees U1; West Longitudes of the Uranus Longitude System (U1) are simply related to the angle PHI: WLONG = 360. - PHI (degrees) This definition of the zero longitude was adopted by the Voyager Project Steering Group in order to minimize differences in longitudes resulting from changes in the assumed rotation period. " END_OBJECT = COORDINFO OBJECT = VECTOR VECTOR_COMPONENT_TYPE = RANGE OBJECT = VECTORCOMP VECTOR_COMPONENT_ID = R REFERENCE_OBJECT_NAME = URANUS REFERENCE_TARGET_NAME = VOYAGER VECTOR_COMPONENT_UNIT = "RU (Ru = 25,600km)" END_OBJECT = VECTORCOMP OBJECT = VECTORD VECTOR_COMPONENT_TYPE_DESC = " Range from the planet center to the spacecraft in units of Ru where Ru = 25,600km." END_OBJECT = VECTORD END_OBJECT = VECTOR OBJECT = VECTOR VECTOR_COMPONENT_TYPE = LATITUDE OBJECT = VECTORCOMP VECTOR_COMPONENT_ID = LAT REFERENCE_OBJECT_NAME = URANUS REFERENCE_TARGET_NAME = VOYAGER VECTOR_COMPONENT_UNIT = DEGREES END_OBJECT = VECTORCOMP OBJECT = VECTORD VECTOR_COMPONENT_TYPE_DESC = " Spacecraft latitude in degrees. Valid range -90.0 -> +90.0." END_OBJECT = VECTORD END_OBJECT = VECTOR OBJECT = VECTOR VECTOR_COMPONENT_TYPE = LONGITUDE OBJECT = VECTORCOMP VECTOR_COMPONENT_ID = W_LONG REFERENCE_OBJECT_NAME = URANUS REFERENCE_TARGET_NAME = VOYAGER VECTOR_COMPONENT_UNIT = DEGREES END_OBJECT = VECTORCOMP OBJECT = VECTORD VECTOR_COMPONENT_TYPE_DESC = " West longitude where the zero longitude is defined by the requirement that the West Longitude of Voyager 2 at 1986-01-24T18:00:00.00 was 302.0 degrees." END_OBJECT = VECTORD END_OBJECT = VECTOR END_OBJECT = COORDINATE /****************** Uranus Mag U1 1.92 SEC Dataset ***************************/ /* MODIFICATIONS */ /* 920831 -- JPLPDS::RMONARREZ */ /* received by ftp */ /* 920914 -- EFRIED */ /* 920918 -- EFRIED */ /* updated Data Set templates according to new std. */ /* Data Set Template -> Spacecraft Data Set Template */ /* event_start_time, event_stop_time -> start_time, stop_time */ /* 920924 -- EFRIED */ /* Revised DATA_SET_ID and DATA_SET_NAME */ /* 921012 -- EFRIED */ /* Revised AUTHOR_FULL_NAME */ /* last changes made */ /* Template: Spacecraft Data Set Template - Rev: 19890121*/ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-MAG-4-RDR-U1COORDS-1.92SEC-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA MAG RESAMPLED RDR U1 COORDINATES 1.92SEC V1.0" DATA_SET_COLLECTION_MEMBER_FLG = "N" START_TIME = 1986-01-24T07:00:00.005 STOP_TIME = 1986-01-25T03:59:58.001 NATIVE_START_TIME = "26834.07.001" NATIVE_STOP_TIME = "26860.21.769" DATA_OBJECT_TYPE = "TIME SERIES" DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = "4" PRODUCER_FULL_NAME = "DR. NORMAN F. NESS" PRODUCER_INSTITUTION_NAME = "UNIVERSITY OF CALIFORNIA, LOS ANGELES" SOFTWARE_FLAG = "N" DETAILED_CATALOG_FLAG = "Y" PROCESSING_START_TIME = "UNK" PROCESSING_STOP_TIME = "UNK" DATA_SET_DESC = " This data set includes data from the Low Field Magnetometer (LFM) in the during the Uranus encounter. The encounter data (1986-01-24T07:00:00 -> 1986-01-25T04:00:00) have been averaged from the 60ms instrument sample rate to a 1.92 second resampled rate and are provided in the Uranus Longitude (U1) coordinate system. Magnetometer data in the solar wind are given in Heliographic coordinates and are also available in a separate dataset. The dataset consists of the following columns: 1) ctime (decimal seconds since 1966-01-01T00:00:00.000), 2) pdstime (ISO standard time format), 3-5) spacecraft clock (m65536,m60,fds-line), 6) magnetometer id (1 = LFM, 2 = HFM), 7) Br (radial component), 8) Bphi (longitudinal component), 9) Btheta (colatitudinal component), 10) Bmag (magnitude of the average components), 11) avg_Bmag (average of the magnitude of the raw components), 12) Lambda (longitude = tan^-1(Bt/Br)), 13) Delta (latitude = sin^-1(Bn/avg_Bmag) ), 14-16) rms vector (Pythagorean root mean square deviation of the component averages), 17) npts (number of points in average), 18) flag a character string which indicates software or s/c hardware intervention which reduces confidence in the data (NULL flags represent 'good' data). The U1 coordinate system is a non-inertial spherical coordinate system that rotates with Uranus with a period of 17.24 hours. The system components are: R - Radial along the Uranus-S/C line, positive away from Uranus, Phi - east longitudinal component, Theta - colatitudinal component. An ancillary data file containing the derived spacecraft magnetic field is provided with this data at a 48 second sample rate. These data provide zero level offsets used in the data processing. S/C field data is provided in spacecraft coordinates." CONFIDENCE_LEVEL_NOTE = " This dataset contains some data gaps and spikes. The dataset does contain a flag value which has been provided by the PI (Norman Ness) that indicates whether or not a particular record has been contaminated by software error or by spacecraft interference ( a flag value of 1 indicates a bad value, 0 indicates that the record has either not been evaluated or is good). Some records that are obviously contaminated have not been flagged. The hourly summary data will show a contamination code and data quality code of 2 when data in the hour have not been flagged but are obviously in error and a contamination code of 1 when the hour contains flagged records." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = "URANUS" END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = "TIME" SAMPLING_PARAMETER_RESOLUTION = 1.920000 MINIMUM_SAMPLING_PARAMETER = 19770820120000.000000 MAXIMUM_SAMPLING_PARAMETER = "UNK" SAMPLING_PARAMETER_INTERVAL = 1.920000 MINIMUM_AVAILABLE_SAMPLING_INT = 0.060000 SAMPLING_PARAMETER_UNIT = "SECOND" DATA_SET_PARAMETER_NAME = "MAGNETIC FIELD VECTOR" NOISE_LEVEL = 0.006000 DATA_SET_PARAMETER_UNIT = "NANOTESLA" END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = "VG2" INSTRUMENT_ID = "MAG" END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = BEHANNONETAL1977 OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD EXPERIMENT FOR VOYAGER 1 AND 2" JOURNAL_NAME = "SPACE SCIENCE REVIEWS" PUBLICATION_DATE = 1977 REFERENCE_DESC = " Behannon K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, F.M. Neubauer, Magnetic Field Experiment for Voyagers 1 and 2, Space Science Reviews, 21, 235, 1977." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "F.M. NEUBAUER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.F. BURLAGA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R.P. LEPPING" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = BEHANNONETAL1986 OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETOTAIL URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Behannon, K.W., et al, The Magnetotail of Uranus, J. Geophys. Res., 92, 366, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "CONNERNEYETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Connerney, J.E.P., M.H. Acuna, and N.F. Ness, The Magnetic Field of Uranus, J. Geophys. Res., 92, 336, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "JOHN E.P. CONNERNEY" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "LEPPINGETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "SURFACE WAVES URANUS MAGNETOPAUSE" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Lepping, R.P., L.F. Burlaga, and L.W. Klein, Surface Waves of Uranus' Magnetopause, J. Geophys, Res., 92, 353, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.F. BURLAGA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.W. KLIEN" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R.P. LEPPING" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "NESSETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD STUDIES URANUS" JOURNAL_NAME = "SCIENCE" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Ness, N.F., et al, Magnetic Fields at Uranus, Science, 233, 85, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "VOIGTETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD CURRENT STRUCTURES MAGNETOSPHERE URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Voigt, G.H., K.W. Behannon, and N.F. Ness, Magnetic Field and Current Structures in the Magnetosphere of Uranus, J. Geophys. Res., 92, 346, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "G.H. VOIGT" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /************* Uranus MAG U1 96SEC Dataset ************************************/ /* MODIFICATIONS */ /* 920831 -- JPLPDS::RMONARREZ */ /* received by ftp */ /* 920914 -- EFRIED */ /* 920918 -- EFRIED */ /* updated Data Set templates according to new std. */ /* Data Set Template -> Spacecraft Data Set Template */ /* event_start_time, event_stop_time -> start_time, stop_time */ /* 920924 -- EFRIED */ /* Revised DATA_SET_ID and DATA_SET_NAME */ /* 921012 -- EFRIED */ /* Revised AUTHOR_FULL_NAME */ /* last changes made */ /* Template: Spacecraft Data Set Template - Rev: 19890121*/ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-MAG-4-RDR-U1COORDS-9.6SEC-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA MAG RESAMPLED RDR U1 COORDINATES 9.6SEC V1.0" DATA_SET_COLLECTION_MEMBER_FLG = "N" START_TIME = 1986-01-24T07:00:00.005 STOP_TIME = 1986-01-25T03:59:58.001 NATIVE_START_TIME = "26834.07.001" NATIVE_STOP_TIME = "26860.21.769" DATA_OBJECT_TYPE = "TIME SERIES" DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = "4" PRODUCER_FULL_NAME = "DR. NORMAN F. NESS" PRODUCER_INSTITUTION_NAME = "UNIVERSITY OF CALIFORNIA, LOS ANGELES" SOFTWARE_FLAG = "N" DETAILED_CATALOG_FLAG = "Y" PROCESSING_START_TIME = "UNK" PROCESSING_STOP_TIME = "UNK" DATA_SET_DESC = " This data set includes data from the Low Field Magnetometer (LFM) in the during the Uranus encounter. The encounter data (1986-01-24T07:00:00 -> 1986-01-25T04:00:00) have been averaged from the 1.92 second averaged data to a 9.6 second resampled rate and are provided in the Uranus Longitude (U1) coordinate system. Magnetometer data in the solar wind are given in Heliographic coordinates and are also available in a separate dataset. The dataset consists of the following columns: 1) ctime (decimal seconds since 1966-01-01T00:00:00.000), 2) pdstime (ISO standard time format), 3-5) spacecraft clock (m65536,m60,fds-line), 6) magnetometer id (1 = LFM, 2 = HFM), 7) Br (radial component), 8) Bphi (longitudinal component), 9) Btheta (colatitudinal component), 10) Bmag (magnitude of the average components), 11) avg_Bmag (average of the magnitude of the raw components), 12) Lambda (longitude = tan^-1(Bt/Br)), 13) Delta (latitude = sin^-1(Bn/avg_Bmag) ), 14-16) rms vector (Pythagorean root mean square deviation of the component averages), 17) npts (number of points in average), 18) flag a character string which indicates software or s/c hardware intervention which reduces confidence in the data (NULL flags represent 'good' data). The U1 coordinate system is a non-inertial spherical coordinate system that rotates with Uranus with a period of 17.24 hours. The system components are: R - Radial along the Uranus-S/C line, positive away from Uranus, Phi - east longitudinal component, Theta - colatitudinal component. An ancillary data file containing the derived spacecraft magnetic field is provided with this data at a 48 second sample rate. These data provide zero level offsets used in the data processing. S/C field data is provided in spacecraft coordinates." CONFIDENCE_LEVEL_NOTE = " This dataset contains some data gaps and spikes. The dataset does contain a flag value which has been provided by the PI (Norman Ness) that indicates whether or not a particular record has been contaminated by software error or by spacecraft interference ( a flag value of 1 indicates a bad value, 0 indicates that the record has either not been evaluated or is good). Some records that are obviously contaminated have not been flagged. The hourly summary data will show a contamination code and data quality code of 2 when data in the hour have not been flagged but are obviously in error and a contamination code of 1 when the hour contains flagged records." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = "URANUS" END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = "TIME" SAMPLING_PARAMETER_RESOLUTION = 9.6 MINIMUM_SAMPLING_PARAMETER = 19770820120000.000000 MAXIMUM_SAMPLING_PARAMETER = "UNK" SAMPLING_PARAMETER_INTERVAL = 9.6 MINIMUM_AVAILABLE_SAMPLING_INT = 0.060000 SAMPLING_PARAMETER_UNIT = "SECOND" DATA_SET_PARAMETER_NAME = "MAGNETIC FIELD VECTOR" NOISE_LEVEL = 0.006000 DATA_SET_PARAMETER_UNIT = "NANOTESLA" END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = "VG2" INSTRUMENT_ID = "MAG" END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = "BEHANNONETAL1977" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD EXPERIMENT FOR VOYAGER 1 AND 2" JOURNAL_NAME = "SPACE SCIENCE REVIEWS" PUBLICATION_DATE = 1977 REFERENCE_DESC = " Behannon K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, F.M. Neubauer, Magnetic Field Experiment for Voyagers 1 and 2, Space Science Reviews, 21, 235, 1977." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "F.M. NEUBAUER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.F. BURLAGA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R.P. LEPPING" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "BEHANNONETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETOTAIL URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Behannon, K.W., et al, The Magnetotail to Uranus, J. Geophys. Res., 92, 336, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "CONNERNEYETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Connerney, J.E.P., M.H. Acuna, and N.F. Ness, The Magnetofield of Uranus, J Geophys. Res., 92, 336, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "JOHN E.P. CONNERNEY" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "LEPPINGETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "SURFACE WAVES URANUS MAGNETOPAUSE" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Lepping, R.P., L.F. Burlaga, and L.W. Klein, Surface Waves of Uranus' Magnetopause, J. Geophys. Res., 92, 353, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.F. BURLAGA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.W. KLIEN" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R.P. LEPPING" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "NESSETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD STUDIES URANUS" JOURNAL_NAME = "SCIENCE" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Ness, N.F., et al, Magnetic Fields at Uranus, Science, 233, 85, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "VOIGTETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD CURRENT STRUCTURES MAGNETOSPHERE URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Voigt, G.H., K.W. Behannon, and N.F. Ness, Magnetic Field and Current Structures in the Magnetosphere of Uranus, J. Geophys. Res., 92, 346, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "G.H. VOIGT" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /******************* Uranus MAG U1 48 SEC Dataset *****************************/ /* MODIFICATIONS */ /* 920831 -- JPLPDS::RMONARREZ */ /* received by ftp */ /* 920914 -- EFRIED */ /* 920918 -- EFRIED */ /* updated Data Set templates according to new std. */ /* Data Set Template -> Spacecraft Data Set Template */ /* event_start_time, event_stop_time -> start_time, stop_time */ /* 920924 -- EFRIED */ /* Revised DATA_SET_ID and DATA_SET_NAME */ /* 921012 -- EFRIED */ /* Revised AUTHOR_FULL_NAME */ /* last changes made */ /* Template: Spacecraft Data Set Template - Rev: 19890121*/ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-MAG-4-SUMM-U1COORDS-48SEC-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA MAG RESAMPLED SUMMARY U1 COORDINATES 48SEC V1.0" DATA_SET_COLLECTION_MEMBER_FLG = "N" START_TIME = 1986-01-24T07:00:00.005 STOP_TIME = 1986-01-25T03:59:58.001 NATIVE_START_TIME = "26834.07.001" NATIVE_STOP_TIME = "26860.21.769" DATA_OBJECT_TYPE = "TIME SERIES" DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = "4" PRODUCER_FULL_NAME = "DR. NORMAN F. NESS" PRODUCER_INSTITUTION_NAME = "UNIVERSITY OF CALIFORNIA, LOS ANGELES" SOFTWARE_FLAG = "Y" DETAILED_CATALOG_FLAG = "Y" PROCESSING_START_TIME = "UNK" PROCESSING_STOP_TIME = "UNK" DATA_SET_DESC = " This data set includes data from the Low Field Magnetometer (LFM) in the during the Uranus encounter. The encounter data (1986-01-24T07:00:00 -> 1986-01-25T04:00:00) have been averaged from the 9.6 second averages to a 48 second resampled rate and are provided in the Uranus Longitude (U1) coordinate system. Magnetometer data in the solar wind are given in Heliographic coordinates and are also available in a separate dataset. The dataset consists of the following columns: 1) ctime (decimal seconds since 1966-01-01T00:00:00.000), 2) pdstime (ISO standard time format), 3-5) spacecraft clock (m65536,m60,fds-line), 6) magnetometer id (1 = LFM, 2 = HFM), 7) Br (radial component), 8) Bphi (longitudinal component), 9) Btheta (colatitudinal component), 10) Bmag (magnitude of the average components), 11) avg_Bmag (average of the magnitude of the raw components), 12) Lambda (longitude = tan^-1(Bt/Br)), 13) Delta (latitude = sin^-1(Bn/avg_Bmag) ), 14-16) rms vector (Pythagorean root mean square deviation of the component averages), 17) npts (number of points in average), 18) flag a character string which indicates software or s/c hardware intervention which reduces confidence in the data (NULL flags represent 'good' data). The U1 coordinate system is a non-inertial spherical coordinate system that rotates with Uranus with a period of 17.24 hours. The system components are: R - Radial along the Uranus-S/C line, positive away from Uranus, Phi - east longitudinal component, Theta - colatitudinal component. An ancillary data file containing the derived spacecraft magnetic field is provided with this data at a 48 second sample rate. These data provide zero level offsets used in the data processing. S/C field data is provided in spacecraft coordinates." CONFIDENCE_LEVEL_NOTE = " This dataset contains some data gaps and spikes. The dataset does contain a flag value which has been provided by the PI (Norman Ness) that indicates whether or not a particular record has been contaminated by software error or by spacecraft interference ( a flag value of 1 indicates a bad value, 0 indicates that the record has either not been evaluated or is good). Some records that are obviously contaminated have not been flagged. The hourly summary data will show a contamination code and data quality code of 2 when data in the hour have not been flagged but are obviously in error and a contamination code of 1 when the hour contains flagged records." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = "URANUS" END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = "TIME" SAMPLING_PARAMETER_RESOLUTION = 48.0 MINIMUM_SAMPLING_PARAMETER = 19770820120000.000000 MAXIMUM_SAMPLING_PARAMETER = "UNK" SAMPLING_PARAMETER_INTERVAL = 48.0 MINIMUM_AVAILABLE_SAMPLING_INT = 0.060000 SAMPLING_PARAMETER_UNIT = "SECOND" DATA_SET_PARAMETER_NAME = "MAGNETIC FIELD VECTOR" NOISE_LEVEL = 0.006000 DATA_SET_PARAMETER_UNIT = "NANOTESLA" END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = "VG2" INSTRUMENT_ID = "MAG" END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = "BEHANNONETAL1977" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD EXPERIMENT FOR VOYAGER 1 AND 2" JOURNAL_NAME = "SPACE SCIENCE REVIEWS" PUBLICATION_DATE = 1977 REFERENCE_DESC = " Behannonetal K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, and F.M. Neubauer, Magnetic Field Experiment for Voyagers 1 and 2, Space Science Reviews, 21, 235, 1977." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "F.M. NEUBAUER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.F. BURLAGA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R.P. LEPPING" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "BEHANNONETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETOTAIL URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Behannon, K.W., et al, The Magnetotail of Uranus, J. Geophys. Res., 92, 366, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "CONNERNEYETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Connerney, J.E.P., M.H. Acuna, and N.F. Ness, The Magnetic Field of Uranus, J. Geophys. Res., 92, 336, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "JOHN E.P. CONNERNEY" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "LEPPINGETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "SURFACE WAVES URANUS MAGNETOPAUSE" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Lepping, R.P., L.F. Burlaga, and L.W. Klein, Surface Waves of Uranus' Magnetopause, J. Geophys. Res., 92, 353, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.F. BURLAGA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.W. KLIEN" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R.P. LEPPING" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "NESSETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD STUDIES URANUS" JOURNAL_NAME = "SCIENCE" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Ness, N.F., et al, Magnetic Fields at Uranus, Science, 233, 85, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "VOIGTETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD CURRENT STRUCTURES MAGNETOSPHERE URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Voigt, G.H., K.W. Behannon, and N.F. Ness, Magnetic Field and Current Structures in the Magnetosphere of Uranus, J. Geophys. Res., 92, 346, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "G.H. VOIGT" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /*************** Uranus Mag Heliographic 1.92 SEC Dataset *******************/ /* MODIFICATIONS */ /* 920831 -- JPLPDS::RMONARREZ */ /* received by ftp */ /* 920914 -- EFRIED */ /* 920918 -- EFRIED */ /* updated Data Set templates according to new std. */ /* Data Set Template -> Spacecraft Data Set Template */ /* event_start_time, event_stop_time -> start_time, stop_time */ /* 920924 -- EFRIED */ /* Revised DATA_SET_ID and DATA_SET_NAME */ /* 921012 -- EFRIED */ /* Revised AUTHOR_FULL_NAME */ /* last changes made */ /* Template: Spacecraft Data Set Template - Rev: 19890121*/ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-MAG-4-RDR-HGCOORDS-1.92SEC-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA MAG RESAMP RDR HELIOGRAPHIC COORDINATES 1.92SEC V1.0" DATA_SET_COLLECTION_MEMBER_FLG = "N" START_TIME = 1986-01-21T00:00:00.319 STOP_TIME = 1986-01-30T23:59:57.445 NATIVE_START_TIME = "26735.22.001" NATIVE_STOP_TIME = "27035.21.769" DATA_OBJECT_TYPE = "TIME SERIES" DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = 4 PRODUCER_FULL_NAME = "DR. JOHN E. P. CONNERNEY" PRODUCER_INSTITUTION_NAME = "GODDARD SPACE FLIGHT CENTER" SOFTWARE_FLAG = N DETAILED_CATALOG_FLAG = Y PROCESSING_START_TIME = UNK PROCESSING_STOP_TIME = UNK DATA_SET_DESC = " This data set includes data from the Low Field Magnetometer (LFM) in the solar wind the near the Uranus encounter. The actual encounter data (1986-01-24T07:00:00 -> 1986-01-25T04:00:00) are provided in the Uranus Longitude coordinate system. The magnetometer data in the solar wind are given in Heliographic coordinates and the data have been averaged from the 60ms instrument sample rate to a 1.92 second resampled rate. The dataset consists of the following columns: 1) ctime (decimal seconds since 1966-01-01T00:00:00.000), 2) pdstime (ISO standard time format), 3-5) spacecraft clock (m65536,m60,fds-line), 6) magnetometer id (1 = LFM, 2 = HFM), 7), Br (radial component), 8) Bt (tangential component), 9) Bn (normal component), 10) Bmag (magnitude of the average components), 11) avg_Bmag (average of the magnitude of the raw components), 12) Lambda (longitude = tan^-1(Bt/Br)), 13) Delta (latitude = sin^-1(Bn/avg_Bmag) ), 14-16) rms vector (Pythagorean root mean square deviation of the component averages), 17) npts (number of points in average), 18) flag a character string which indicates software or s/c hardware intervention which reduces confidence in the data (NULL flags represent 'good' data). The Heliographic coordinate system is defined by the spacecraft centered R, T, N coordinates whose unit vector are: R - along the Sun-spacecraft line, positive away from the Sun; T - parallel to Sun's equator, positive in the sense of Jupiter's motion; N - equal to R x T. An ancillary data file containing the derived spacecraft magnetic field is provided with this data at a 48 second sample rate. These data provide zero level offsets used in the data processing. S/C field data is provided in spacecraft coordinates." CONFIDENCE_LEVEL_NOTE = " This dataset contains some data gaps and spikes. The dataset does contain a flag value which has been provided by the PI (Norman Ness) that indicates whether or not a particular record has been contaminated by software error or by spacecraft interference ( a NULL flag string indicates good data. Strings which contain characters may be contaminated in one or more ways. Some records that are obviously contaminated have not been flagged." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = URANUS END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = 0.06 MINIMUM_SAMPLING_PARAMETER = 0.06 MAXIMUM_SAMPLING_PARAMETER = 0.06 SAMPLING_PARAMETER_INTERVAL = 1.92 MINIMUM_AVAILABLE_SAMPLING_INT = 1.92 SAMPLING_PARAMETER_UNIT = SECOND DATA_SET_PARAMETER_NAME = "MAGNETIC FIELD VECTOR" NOISE_LEVEL = 0.006 DATA_SET_PARAMETER_UNIT = NANOTESLA END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = VG2 INSTRUMENT_ID = MAG END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = "BEHANNONETAL1977" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD EXPERIMENT FOR VOYAGER 1 AND 2" JOURNAL_NAME = "SPACE SCIENCE REVIEWS" PUBLICATION_DATE = 1977 REFERENCE_DESC = " Behannon K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, and F.M. Neubauer, Magnetic Field Experiment for Voyagers 1 and 2, Space Science Reviews, 21, 235, 1977." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "F.M. NEUBAUER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.F. BURLAGA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R.P. LEPPING" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "BEHANNONETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETOTAIL URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Behannon, K.W., et al, The Magnetotail of Uranus, J. Geophys. Res., 92, 366, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "CONNERNEYETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Connerney, J.E.P., M.H. Acuna, and N.F. Ness, The Magnetic Field of Uranus, J. Geophys. Res., 92, 336, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "JOHN E.P. CONNERNEY" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "LEPPINGETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "SURFACE WAVES URANUS MAGNETOPAUSE" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Lepping, R.P., L.F. Burlaga, and L.W. Klein, Surface Waves of Uranus' Magnetopause, J. Geophys, Res., 92, 353, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.F. BURLAGA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.W. KLIEN" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R.P. LEPPING" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "NESSETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD STUDIES URANUS" JOURNAL_NAME = "SCIENCE" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Ness, N.F., et al, Magnetic Fields at Uranus, Science, 233, 85, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "VOIGTETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD CURRENT STRUCTURES MAGNETOSPHERE URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Voigt, G.H., K.W. Behannon, and N.F. Ness, Magnetic Field and Current Structures in the Magnetosphere of Uranus, J. Geophys. Res., 92, 346, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "G.H. VOIGT" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /***************** Uranus MAG Heliographic 9.6SEC Dataset *********************/ /* MODIFICATIONS */ /* 920831 -- JPLPDS::RMONARREZ */ /* received by ftp */ /* 920914 -- EFRIED */ /* 920918 -- EFRIED */ /* updated Data Set templates according to new std. */ /* Data Set Template -> Spacecraft Data Set Template */ /* event_start_time, event_stop_time -> start_time, stop_time */ /* 920924 -- EFRIED */ /* Revised DATA_SET_ID and DATA_SET_NAME */ /* 921012 -- EFRIED */ /* Revised AUTHOR_FULL_NAME */ /* last changes made */ /* Template: Spacecraft Data Set Template - Rev: 19890121*/ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-MAG-4-RDR-HGCOORDS-9.6SEC-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA MAG RESAMP RDR HELIOGRAPHIC COORDINATES 9.6SEC V1.0" DATA_SET_COLLECTION_MEMBER_FLG = "N" START_TIME = 1986-01-21T00:00:00.319 STOP_TIME = 1986-01-30T23:59:57.445 NATIVE_START_TIME = "26735.22.001" NATIVE_STOP_TIME = "27035.21.769" DATA_OBJECT_TYPE = "TIME SERIES" DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = 4 PRODUCER_FULL_NAME = "DR. JOHN E. P. CONNERNEY" PRODUCER_INSTITUTION_NAME = "GODDARD SPACE FLIGHT CENTER" SOFTWARE_FLAG = N DETAILED_CATALOG_FLAG = Y PROCESSING_START_TIME = UNK PROCESSING_STOP_TIME = UNK DATA_SET_DESC = " This data set includes data from the Low Field Magnetometer (LFM) in the solar wind the near the Uranus encounter. The actual encounter data (1986-01-24T07:00:00 -> 1986-01-25T04:00:00) are provided in the Uranus Longitude coordinate system. The magnetometer data in the solar wind are given in Heliographic coordinates and the data have been averaged from the 1.92 second resampled data to a 9.6 second resampled rate. The dataset consists of the following columns: 1) ctime (decimal seconds since 1966-01-01T00:00:00.000), 2) pdstime (ISO standard time format), 3-5) spacecraft clock (m65536,m60,fds-line), 6) magnetometer id (1 = LFM, 2 = HFM), 7), Br (radial component), 8) Bt (tangential component), 9) Bn (normal component), 10) Bmag (magnitude of the average components), 11) avg_Bmag (average of the magnitude of the raw components), 12) Lambda (longitude = tan^-1(Bt/Br)), 13) Delta (latitude = sin^-1(Bn/avg_Bmag) ), 14-16) rms vector (Pythagorean root mean square deviation of the component averages), 17) npts (number of points in average), 18) flag a character string which indicates software or s/c hardware intervention which reduces confidence in the data (NULL flags represent 'good' data). The Heliographic coordinate system is defined by the spacecraft centered R, T, N coordinates whose unit vector are: R - along the Sun-spacecraft line, positive away from the Sun; T - parallel to Sun's equator, positive in the sense of Jupiter's motion; N - equal to R x T. An ancillary data file containing the derived spacecraft magnetic field is provided with this data at a 48 second sample rate. These data provide zero level offsets used in the data processing. S/C field data is provided in spacecraft coordinates." CONFIDENCE_LEVEL_NOTE = " This dataset contains some data gaps and spikes. The dataset does contain a flag value which has been provided by the PI (Norman Ness) that indicates whether or not a particular record has been contaminated by software error or by spacecraft interference ( a NULL flag string indicates good data. Strings which contain characters may be contaminated in one or more ways. Some records that are obviously contaminated have not been flagged." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = URANUS END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = 0.06 MINIMUM_SAMPLING_PARAMETER = 0.06 MAXIMUM_SAMPLING_PARAMETER = 0.06 SAMPLING_PARAMETER_INTERVAL = 9.6 MINIMUM_AVAILABLE_SAMPLING_INT = 9.6 SAMPLING_PARAMETER_UNIT = SECOND DATA_SET_PARAMETER_NAME = "MAGNETIC FIELD VECTOR" NOISE_LEVEL = 0.006 DATA_SET_PARAMETER_UNIT = NANOTESLA END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = VG2 INSTRUMENT_ID = MAG END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = "BEHANNONETAL1977" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD EXPERIMENT FOR VOYAGER 1 AND 2" JOURNAL_NAME = "SPACE SCIENCE REVIEWS" PUBLICATION_DATE = 1977 REFERENCE_DESC = " Behannon K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, F.M. Neubauer, Magnetic Field Experiment for Voyagers 1 and 2, Space Science Reviews, 21, 235, 1977." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "F.M. NEUBAUER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.F. BURLAGA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R.P. LEPPING" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "BEHANNONETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETOTAIL URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Behannon, K.W., et al, The Magnetotail of Uranus, J. Geophys. Res., 92, 366, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "CONNERNEYETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Connerney, J.E.P., M.H. Acuna, and N.F. Ness, The Magnetic Field of Uranus, J. Geophys. Res., 92, 336, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "JOHN E.P. CONNERNEY" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "LEPPINGETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "SURFACE WAVES URANUS MAGNETOPAUSE" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Lepping, R.P., L.F. Burlaga, and L.W. Klein, Surface Waves of Uranus' Magnetopause, J. Geophys, Res., 92, 353, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.F. BURLAGA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.W. KLIEN" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R.P. LEPPING" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "NESSETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD STUDIES URANUS" JOURNAL_NAME = "SCIENCE" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Ness, N.F., et al, Magnetic Fields at Uranus, Science, 233, 85, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "VOIGTETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD CURRENT STRUCTURES MAGNETOSPHERE URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Voigt, G.H., K.W. Behannon, N.F. Ness, Magnetic Field and Current Structures in the Magnetosphere of Uranus, J. Geophys. Res., 92, 346, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "G.H. VOIGT" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /****************** Uranus MAG Heliographic 48 SEC Dataset ********************/ /* MODIFICATIONS */ /* 920831 -- JPLPDS::RMONARREZ */ /* received by ftp */ /* 920914 -- EFRIED */ /* 920918 -- EFRIED */ /* updated Data Set templates according to new std. */ /* Data Set Template -> Spacecraft Data Set Template */ /* event_start_time, event_stop_time -> start_time, stop_time */ /* 920924 -- EFRIED */ /* Revised DATA_SET_ID and DATA_SET_NAME */ /* 921012 -- EFRIED */ /* Revised AUTHOR_FULL_NAME */ /* last changes made */ /* Template: Spacecraft Data Set Template - Rev: 19890121*/ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-MAG-4-SUMM-HGCOORDS-48SEC-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA MAG RESAMP SUMMARY HELIOGRAPHIC COORDS 48SEC V1.0" DATA_SET_COLLECTION_MEMBER_FLG = "N" START_TIME = 1986-01-21T00:00:00.319 STOP_TIME = 1986-01-30T23:59:57.445 NATIVE_START_TIME = "26735.22.001" NATIVE_STOP_TIME = "27035.21.769" DATA_OBJECT_TYPE = "TIME SERIES" DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = 4 PRODUCER_FULL_NAME = "DR. JOHN E. P. CONNERNEY" PRODUCER_INSTITUTION_NAME = "GODDARD SPACE FLIGHT CENTER" SOFTWARE_FLAG = Y DETAILED_CATALOG_FLAG = Y PROCESSING_START_TIME = UNK PROCESSING_STOP_TIME = UNK DATA_SET_DESC = " This data set includes data from the Low Field Magnetometer (LFM) in the solar wind the near the Uranus encounter. The actual encounter data (1986-01-24T07:00:00 -> 1986-01-25T04:00:00) are provided in the Uranus Longitude coordinate system. The magnetometer data in the solar wind are given in Heliographic coordinates and the data have been averaged from the 9.6 second resampled data to a 48.0 second sampled rate. The dataset consists of the following columns: 1) ctime (decimal seconds since 1966-01-01T00:00:00.000), 2) pdstime (ISO standard time format), 3-5) spacecraft clock (m65536,m60,fds-line), 6) magnetometer id (1 = LFM, 2 = HFM), 7), Br (radial component), 8) Bt (tangential component), 9) Bn (normal component), 10) Bmag (magnitude of the average components), 11) avg_Bmag (average of the magnitude of the raw components), 12) Lambda (longitude = tan^-1(Bt/Br)), 13) Delta (latitude = sin^-1(Bn/avg_Bmag) ), 14-16) rms vector (Pythagorean root mean square deviation of the component averages), 17) npts (number of points in average), 18) flag a character string which indicates software or s/c hardware intervention which reduces confidence in the data (NULL flags represent 'good' data). The Heliographic coordinate system is defined by the spacecraft centered R, T, N coordinates whose unit vector are: R - along the Sun-spacecraft line, positive away from the Sun; T - parallel to Sun's equator, positive in the sense of Jupiter's motion; N - equal to R x T. An ancillary data file containing the derived spacecraft magnetic field is provided with this data at a 48 second sample rate. These data provide zero level offsets used in the data processing. S/C field data is provided in spacecraft coordinates." CONFIDENCE_LEVEL_NOTE = " This dataset contains some data gaps and spikes. The dataset does contain a flag value which has been provided by the PI (Norman Ness) that indicates whether or not a particular record has been contaminated by software error or by spacecraft interference ( a NULL flag string indicates good data. Strings which contain characters may be contaminated in one or more ways. Some records that are obviously contaminated have not been flagged." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = URANUS END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = 0.06 MINIMUM_SAMPLING_PARAMETER = 0.06 MAXIMUM_SAMPLING_PARAMETER = 0.06 SAMPLING_PARAMETER_INTERVAL = 48.0 MINIMUM_AVAILABLE_SAMPLING_INT = 48.0 SAMPLING_PARAMETER_UNIT = SECOND DATA_SET_PARAMETER_NAME = "MAGNETIC FIELD VECTOR" NOISE_LEVEL = 0.006 DATA_SET_PARAMETER_UNIT = NANOTESLA END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = VG2 INSTRUMENT_ID = MAG END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = "BEHANNONETAL1977" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD EXPERIMENT FOR VOYAGER 1 AND 2" JOURNAL_NAME = "SPACE SCIENCE REVIEWS" PUBLICATION_DATE = 1977 REFERENCE_DESC = " Behannon K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, F.M. Neubauer, Magnetic Field Experiment for Voyagers 1 and 2, Space Science Reviews, 21, 235, 1977." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "F.M. NEUBAUER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.F. BURLAGA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R.P. LEPPING" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "BEHANNONETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETOTAIL URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Behannon, K.W., et al, The Magnetotail of Uranus J. Geophys. Res., 92, 366, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "CONNERNEYETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Connerney, J.E.P., M.H. Acuna, and N.F. Ness, The Magnetic Field of Uranus, J. Geophys. Res., 92, 336, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "JOHN E.P. CONNERNEY" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "LEPPINGETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "SURFACE WAVES URANUS MAGNETOPAUSE" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Lepping, R.P., L.F. Burlaga, and L.W. Klein, Surface Waves of Uranus' Magnetopause, J. Geophys, Res., 92, 353, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.F. BURLAGA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.W. KLIEN" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R.P. LEPPING" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "NESSETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD STUDIES URANUS" JOURNAL_NAME = "SCIENCE" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Ness, N.F., et al, Magnetic Fields at Uranus, Science, 233, 85, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "VOIGTETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD CURRENT STRUCTURES MAGNETOSPHERE URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Voigt, G.H., K.W. Behannon, N.F. Ness, Magnetic Field and Current Structures in the Magnetosphere of Uranus, J. Geophys. Res., 92, 346, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "G.H. VOIGT" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /***********************MAG Parameter Template ********************************/ /* MODIFICATIONS: */ /* From: JPLPDS::RMONARREZ 6-AUG-1992 13:38:59.22 */ /* 92-08 EFRIED */ /* 920916 EFRIED */ /* last changes made */ /* Template: Parameter Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID ="VG2" DATA_SET_PARAMETER_NAME ="MAGNETIC FIELD VECTOR" INSTRUMENT_PARAMETER_NAME ="MAGNETIC FIELD COMPONENT" IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /***********************MAG Parameter Desc. Template **************************/ /* MODIFICATIONS: */ /* From: JPLPDS::RMONARREZ 6-AUG-1992 13:38:59.22 */ /* 92-08 EFRIED */ /* 920916 EFRIED */ /* changed capitalization */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM = "MAGNETIC FIELD VECTOR" DATA_SET_OR_INST_PARM_DESC = " A derived parameter which combines the 3 orthogonal magnetic field component measurements." END_OBJECT = DSINSTPARMD /***********************MAG Parameter Desc. Template **************************/ /* MODIFICATIONS: */ /* 921001 -- EFRIED */ /* created template */ /* NEED DESCRIPTION */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM = "MAGNETIC FIELD COMPONENT" DATA_SET_OR_INST_PARM_DESC = " A measured parameter equaling the magnetic field strength (e.g. in nanoteslas) along a particular axis direction. Usually the three orthogonal axis components are measured by three different sensors." END_OBJECT = DSINSTPARMD /*************** PLS Uranus Electron dataset *****************************/ /* MODIFICATIONS */ /* 920831 -- JPLPDS::RMONARREZ */ /* received by ftp */ /* 920914 -- EFRIED */ /* 920918 -- EFRIED */ /* updated Data Set templates according to new std. */ /* Data Set Template -> Spacecraft Data Set Template */ /* event_start_time, event_stop_time -> start_time, stop_time */ /* 920924 -- EFRIED */ /* Revised DATA_SET_ID and DATA_SET_NAME */ /* last changes made */ /* Template: Spacecraft Data Set Template Rev: 19890121 */ /* */ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-PLS-5-RDR-ELEFIT-48SEC-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA PLS DERIVED RDR ELECTRON FIT 48SEC V1.0" DATA_SET_COLLECTION_MEMBER_FLG = "N" START_TIME = 1986-01-24T07:06:31.204 STOP_TIME = 1986-01-24T23:59:19.137 NATIVE_START_TIME = "UNK" NATIVE_STOP_TIME = "UNK" DATA_OBJECT_TYPE = "TIME SERIES" DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = "5" PRODUCER_FULL_NAME = "JOHN D. RICHARDSON" PRODUCER_INSTITUTION_NAME = "MASSACHUSETTS INSTITUTE OF TECHNOLOGY" SOFTWARE_FLAG = "Y" DETAILED_CATALOG_FLAG = "Y" PROCESSING_START_TIME = "UNK" PROCESSING_STOP_TIME = "UNK" DATA_SET_DESC = " This data set contains electron parameters in the PLS energy range (10-5950 eV) at Uranus during the Voyager 2 encounter. Parameters are calculated in several ways. Total moment density and temperature are given. Each electron spectrum is also fit with a thermal component and 1-3 hot components depending on how many Maxwellians are needed to fit the entire distribution. The moment density and temperature of the hot component is calculated after the thermal component is subtracted from the spectrum. The CHI-Square value for each fit is given. The spacecraft charge is not calculated consistently, and may result in factor of 2-3 errors in the thermal electron density. Data is unreliable inside 5 RU and in the occultation regions. At Uranus measurements were taken using both a long and a short integration time. Each 48 SEC measurement frame contained either an E1-Short and an E2-Long measurement or an E2-Short and an EI-Long. To reduce systematic errors, complete electron spectra were obtained only by combining two long or two short spectra. The instrument threshold is at a density of about 0.001 CM-3; thus fits which yield data close to this value should be treated with caution. Flags in the data indicate whether the full analysis could be performed and if the data was contaminated by LECP stepping. A complete description of this data set is in Sittler et al. (1987). THE PARAMETER DEFINITIONS ARE: NAME TYPE DEFINITION TIME A*24 YR,MON,DAY,HR,MIN,SEC,MSEC IFLY ' Flag = 0 for Cruise, 1 for Magnetosphere, -2 for rough moment estimate only, -5 for no analysis LECPF ' Flag = 1 for LECP contamination, 0 otherwise EDATA(1) R*4 THBN(angle between DCUP normal and B vector) 2 ' RNE moment electron density (/CM**3) 3 ' RTE ' ' temperature (eV) 4 ' PHISC spacecraft potential (Volts) 5 ' RNC cold electron density (/CM**3) 6 ' SGNC standard deviation of RNC (/CM**3) 7 ' RTC cold electron temperature (eV) 8 ' SGTC standard deviation of RTC (eV) 9 ' CHIC CHI-Square of cold fit 10 ' RNH1 1st hot electron density (/CM**3) 11 ' SGNH1 standard deviation of RNH1 (/CM**3) 12 ' TH1 1st hot electron temperature (eV) 13 ' SGTH1 standard deviation of TH1 (eV) 14 ' CHIH1 CHI-Square of 1st hot fit 15 ' RNH2 2nd hot electron density (/CM**3) 16 ' SGNH2 standard deviation of RNH2 (/CM**3) 17 ' TH2 2nd hot electron temperature (eV) 18 ' SGTH2 standard deviation of th2 (eV) 19 ' CHIH2 CHI-Square of 2nd hot fit 20 ' RNH3 3rd hot electron density (/CM**3) 21 ' SGNH3 standard deviation of RNH3 (/CM**3) 22 ' TH3 3rd hot electron temperature (eV) 23 ' SGTH3 standard deviation of TH3 (eV) 24 ' CHIH3 CHI-square of 3rd hot fit 25 ' CHI CHI-Square for total fit 26 ' RNH moment hot electron density (/CM**3) 27 ' RTH moment hot electron temperature (eV) In computing RNH1,TH1 we used the 3rd to 7th channels above the breakpoint energy EB1 and subtracted the cold component FC from FE (observed) before doing the fit. In reality this fit was done iteratively between the cold and hot component fits (FC=FE-FH and FH=FE-FC etc.). A similar approach was used in computing RNH3,TH3 for which a Maxwellian fit was done to those channels above EB2. The parameters RNH2,TH2 were fit to the upper 5 (3 MIN) channels (generally above EB2). This fit was primarily done to allow proper estimation of FE to the high energy portion of the spectrum. In many cases there are not sufficient points to compute RNH3,TH3 AND RNH2,TH2 do provide a fair representation of the spectrum. If RNH1=RNH2=RNH3 then you should not use the 2nd and 3rd fit parameters. Values of 1.E32 indicate that the parameter could not be obtained from the data using the standard analysis technique. Additional information about this dataset and the instrument which produced it can be found elsewhere in this catalog. An overview of the data in this data set can be found in Sittler et al. (1987) and a complete instrument description can be found in Bridge (1977)." CONFIDENCE_LEVEL_NOTE = " This data set provides an estimate of the electron parameters in the PLS energy range (10-5950 eV). The thermal electron parameters may be underestimated in some regions due to negative spacecraft charging which is not corrected for. Electron parameters may also be unreliable between 1736 and 1854 SCET on Jan 24 where electron temperatures are below the instrument energy threshold. Between 1920 and 2150 SCET on Jan 24 The spacecraft had a large (several hundred volt) negative potential, so electron parameters in this region should also be treated with caution. The instrument threshold for detecting electrons is a density of about 0.001 CM-3. At times when the density is near this value all derived parameters are suspect. From 1621 to 1649 on Jan. 24 sunlight created an artificial signal so this data should be discarded. The LECP stepper motor is also creates a spurious signal in the PLS detector; times when this occurs are flagged." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = "URANUS" END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = "TIME" SAMPLING_PARAMETER_RESOLUTION = 48.000000 MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 48.000000 MINIMUM_AVAILABLE_SAMPLING_INT = 48.000000 SAMPLING_PARAMETER_UNIT = "SECOND" DATA_SET_PARAMETER_NAME = "ELECTRON DENSITY" NOISE_LEVEL = "N/A" DATA_SET_PARAMETER_UNIT = "CM-3" END_OBJECT = DSPARMINFO OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = "TIME" SAMPLING_PARAMETER_RESOLUTION = 48.000000 MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 48.000000 MINIMUM_AVAILABLE_SAMPLING_INT = 48.000000 SAMPLING_PARAMETER_UNIT = "SECOND" DATA_SET_PARAMETER_NAME = "ELECTRON TEMPERATURE" NOISE_LEVEL = "N/A" DATA_SET_PARAMETER_UNIT = "CM-3" END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = "VG2" INSTRUMENT_ID = "PLS" END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = "SITTLERETAL1987" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "URANUS ELECTRONS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1987 REFERENCE_DESC = " Sittler, E.C., Jr., K.W. Ogilvie and R.S. Selesnick, Survey of Electrons in the Uranian Magnetosphere: Voyager 2 Observations, J. Geophys. Res., 92, 15263-15281, 1987." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "E .C. SITTLER, JR." END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K. W. OGILVIE" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R. S. SELESNICK" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /**************** PLS Uranus Ion Browse dataset **************************/ /* MODIFICATIONS */ /* 920831 -- JPLPDS::RMONARREZ */ /* received by ftp */ /* 920914 -- EFRIED */ /* 920918 -- EFRIED */ /* updated Data Set templates according to new std. */ /* Data Set Template -> Spacecraft Data Set Template */ /* event_start_time, event_stop_time -> start_time, stop_time */ /* 920924 -- EFRIED */ /* Revised DATA_SET_ID and DATA_SET_NAME */ /* last changes made /* Template: Spacecraft Data Set Template Rev: 19890121 */ /* */ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-PLS-5-SUMM-IONBR-48SEC-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA PLS DERIVED SUMMARY ION FIT 48SEC V1.0" DATA_SET_COLLECTION_MEMBER_FLG = "N" START_TIME = 1986-01-24T15:01:48.451 STOP_TIME = 1986-01-24T19:55:24.431 NATIVE_START_TIME = UNK NATIVE_STOP_TIME = UNK DATA_OBJECT_TYPE = "TIME SERIES" DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = "5" PRODUCER_FULL_NAME = "JOHN D. RICHARDSON" PRODUCER_INSTITUTION_NAME = "MASSACHUSETTS INSTITUTE OF TECHNOLOGY" SOFTWARE_FLAG = "Y" DETAILED_CATALOG_FLAG = "Y" PROCESSING_START_TIME = "N/A" PROCESSING_STOP_TIME = "N/A" DATA_SET_DESC = " This data set contains the total ion density obtained from Voyager 2 PLS data (voltage range 10-5950 eV/Q) at Uranus by fitting the measured spectra with isotropic Maxwellian distributions. It is a subset of the data set VG2-U-PLS-5-RDR-IONFIT-48SEC. Up to three isotropic proton components (warm, hot and intermediate) were used to match the observations. These were then summed to give total ion density. This determination does not include possible plasma outside the PLS energy range; limits on a cold component can be derived in the charging region from 1939-2158 on day 24. It is found that if a cold component exists it will increase the total ion density by at most a factor of two. uncertainties in plasma parameters are a factor of 2 in the charging region, less than 20% elsewhere. A complete description of this data set is given in McNutt et al. (1987) and Selesnick and McNutt (1987). Data format: first six columns are time tags (6I4), last column is total ion density in CM-3 (E11.3). Values of 1.E32 indicate that the parameter could not be obtained from the data using the standard analysis technique. Additional information about this dataset and the instrument which produced it can be found elsewhere in this catalog. An overview of the data in this data set can be found in McNutt et al. (1987) and Selesnick and McNutt (1987) and a complete instrument description can be found in Bridge (1977)." CONFIDENCE_LEVEL_NOTE = " This data set provides a reliable estimate of the total ion density in the PLS energy range (10-5950 eV) throughout the region where data is provided. Formal 1 SIGMA uncertainties for the derived densities and thermal speeds are given in the complete data set and range from a few to 20%. underestimates of ion density and temperature due to ions outside the PLS energy range are less than 10%." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = "URANUS" END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = "TIME" SAMPLING_PARAMETER_RESOLUTION = 48.000000 MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 48.000000 MINIMUM_AVAILABLE_SAMPLING_INT = 24.000000 SAMPLING_PARAMETER_UNIT = "SECOND" DATA_SET_PARAMETER_NAME = "ION DENSITY" NOISE_LEVEL = "N/A" DATA_SET_PARAMETER_UNIT = "CM-3" END_OBJECT = DSPARMINFO OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = "TIME" SAMPLING_PARAMETER_RESOLUTION = 48.000000 MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 48.000000 MINIMUM_AVAILABLE_SAMPLING_INT = 24.000000 SAMPLING_PARAMETER_UNIT = "SECOND" DATA_SET_PARAMETER_NAME = "ION THERMAL SPEED" NOISE_LEVEL = "N/A" DATA_SET_PARAMETER_UNIT = "KM/S" END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = "VG2" INSTRUMENT_ID = "PLS" END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = "MCNUTTETAL1987" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "URANUS IONS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1987 REFERENCE_DESC = " McNutt, R.L., Jr., R. Selesnick and J. Richardson, Low Energy Plasma Observations in the Magnetosphere of Uranus, J. Geophys. Res., 92, 4399-4410, 1987." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "J. D. RICHARDSON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R. L. MCNUTT, JR." END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R. S. SELESNICK" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO OBJECT = DSREFINFO REFERENCE_KEY_ID = "SELESNICK&MCNUTT1987" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "URANUS IONS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1987 REFERENCE_DESC = " Selesnick, R.S., and R.L. McNutt, Jr., Voyager 2 Plasma Ion Observations in the Magnetosphere of Uranus, J. Geophys. Res., 92, 15249-15262, 1987." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R. L. MCNUTT, JR." END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R. S. SELESNICK" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /**************** PLS Uranus Ion Fit dataset *****************************/ /* MODIFICATIONS */ /* 920831 -- JPLPDS::RMONARREZ */ /* received by ftp */ /* 920914 -- EFRIED */ /* 920918 -- EFRIED */ /* updated Data Set templates according to new std. */ /* Data Set Template -> Spacecraft Data Set Template */ /* event_start_time, event_stop_time -> start_time, stop_time */ /* 920924 -- EFRIED */ /* Revised DATA_SET_ID and DATA_SET_NAME */ /* last changes made /* Template: Spacecraft Data Set Template Rev: 19890121 */ /* */ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-PLS-5-RDR-IONFIT-48SEC-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA PLS DERIVED RDR ION FIT 48SEC V1.0" DATA_SET_COLLECTION_MEMBER_FLG = "N" START_TIME = 1986-01-24T15:01:48.451 STOP_TIME = 1986-01-24T19:55:24.431 NATIVE_START_TIME = UNK NATIVE_STOP_TIME = UNK DATA_OBJECT_TYPE = "TIME SERIES" DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = "5" PRODUCER_FULL_NAME = "JOHN D. RICHARDSON" PRODUCER_INSTITUTION_NAME = "MASSACHUSETTS INSTITUTE OF TECHNOLOGY" SOFTWARE_FLAG = "Y" DETAILED_CATALOG_FLAG = "Y" PROCESSING_START_TIME = "N/A" PROCESSING_STOP_TIME = "N/A" DATA_SET_DESC = " This data set contains the ion densities and temperatures along with formal 1 Sigma errors obtained from Voyager 2 PLS data (voltage range 10-5950 eV/Q) at Uranus by fitting the measured spectra with isotropic Maxwellian distributions. Up to three isotropic proton components (warm, hot and intermediate) were used to match the observations. The plasma was assumed to be rigidly corotating. Uncertainties in plasma parameters are a factor of 2 in the charging region from 1939-2158 on day 24, less than 20% elsewhere. A complete description of this data set is given in McNutt et al. (1987) and Selesnick and McNutt (1987). DATASET PARAMETERS: Each data record consists of six lines: 1. Time of measurement Mode (A3): L or M. 3-6. Cup identifier (A1): A, B, C, or D. Number of sets of channels used in fit (I3). Beginning and ending channel of each set (2I4 repeated for each set). 7-19.Density (CM-3) and 1 sigma uncertainty for first fit component (2E10.3). Same for second fit component (2E10.3). Same for third fit component (2E10.3). Thermal speed (KM/S) and 1 sigma uncertainty for First fit component (2E10.3). Same for second fit component (2E10.3). Same for third fit component (2E10.3). Values of 1.E32 indicate that the parameter could not be obtained from the data using the standard analysis technique. Additional information about this dataset and the instrument which produced it can be found elsewhere in this catalog. An overview of the data in this data set can be found in McNutt et al. (1987) and Selesnick and McNutt (1987) and a complete instrument description can be found in Bridge (1977)." CONFIDENCE_LEVEL_NOTE = " This data set provides a reliable estimate of the ion density and energy in the PLS energy range (10-5950 eV) throughout the region where data is provided. All ion components are fit with Maxwellians although they may not be Maxwellian in nature. Formal 1 sigma uncertainties for the derived densities and thermal speeds are given in the data set and range from a few to 20%. Underestimates of ion density and temperature due to ions outside the PLS energy range are less than 10%." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = "URANUS" END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = "TIME" SAMPLING_PARAMETER_RESOLUTION = 48.000000 MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 48.000000 MINIMUM_AVAILABLE_SAMPLING_INT = 24.000000 SAMPLING_PARAMETER_UNIT = "SECOND" DATA_SET_PARAMETER_NAME = "ION DENSITY" NOISE_LEVEL = "N/A" DATA_SET_PARAMETER_UNIT = "CM-3" END_OBJECT = DSPARMINFO OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = "TIME" SAMPLING_PARAMETER_RESOLUTION = 48.000000 MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 48.000000 MINIMUM_AVAILABLE_SAMPLING_INT = 24.000000 SAMPLING_PARAMETER_UNIT = "SECOND" DATA_SET_PARAMETER_NAME = "ION THERMAL SPEED" NOISE_LEVEL = "N/A" DATA_SET_PARAMETER_UNIT = "KM/S" END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = "VG2" INSTRUMENT_ID = "PLS" END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = "MCNUTTETAL1987" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "URANUS IONS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1987 REFERENCE_DESC = " McNutt, R.L., Jr., R. Selesnick and J. Richardson, Low Energy Plasma Observations in the Magnetosphere of Uranus, J. Geophys. Res., 92, 4399-4410, 1987." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "J. D. RICHARDSON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R. L. MCNUTT, JR." END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R. S. SELESNICK" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /******************* Uranus PLS ELEBR 48SEC ***********************************/ /* MODIFICATIONS: */ /* 921029 SJOY */ /* created template */ /* Template: Spacecraft Data Set Template - Rev: 19890121 */ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDATASET */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = 'VG2-U-PLS-5-SUMM-ELEBR-48SEC-V1.0' OBJECT = DATASETINFO DATA_SET_NAME = 'VG2 URA PLS DERIVED SUMM ELECTRON BROWSE 48SEC V1.0' START_TIME = 1986-01-24T07:06:31.204 STOP_TIME = 1986-01-24T23:59:19.137 NATIVE_START_TIME = 'UNK' NATIVE_STOP_TIME = 'UNK' DATA_OBJECT_TYPE = 'TIME SERIES' DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = '5' PRODUCER_FULL_NAME = 'JOHN D. RICHARDSON' PRODUCER_INSTITUTION_NAME = 'MASSACHUSETTS INSTITUTE OF TECHNOLOGY' SOFTWARE_FLAG = 'Y' DETAILED_CATALOG_FLAG = 'Y' PROCESSING_START_TIME = 'UNK' PROCESSING_STOP_TIME = 'UNK' DATA_SET_DESC = " This data set contains the thermal electron density and temperature in the PLS energy range (10-5950 eV) from Voyager 2 at Uranus derived by fitting the low energy electron component with a Maxwellian distribution, and the moment density and temperature of the hot electrons calculated after the signal from the thermal component is subtracted from the electron spectra. The moment density and temperature obtained by integrating over the entire measured distribution function are also given. This is a subset of the data set VG2-U-PLS-5-RDR-ELEFIT-48SEC which should be obtained before this data is used, since it contains information on the type of fit performed and LECP contamination of the data. Spacecraft charging may result in underestimation of thermal electron density in some regions. The first six columns are the time tag (year, day, hour, min, sec, msec), columns 7 and 8 are the total moment density and temperature, columns 9 and 10 are the fit density and temperature of the thermal electron component, and 11 and 12 are the moment density and temperature of the suprathermal electrons. Each row has the format (6I4,6E12.4). Values of 1.E32 indicate that the parameter could not be obtained from the data using the standard analysis technique. Additional information about this dataset and the instrument which produced it can be found elsewhere in this catalog. An overview of the data in this data set can be found in Sittler et al. (1987) and a complete instrument description can be found in bridge (1977)." CONFIDENCE_LEVEL_NOTE = " This data set provides an estimate of the electron parameters in the PLS energy range (10-5950 eV). The thermal electron parameters may be underestimated in some regions due to negative spacecraft charging which is not corrected for. Electron parameters may also be unreliable between 1736 and 1854 scet on Jan 24 where electron temperatures are below the instrument energy threshold. Between 1920 and 2150 scet on Jan 24 the spacecraft had a large (several hundred volt) negative potential, so electron parameters in this region should also be treated with caution. The instrument threshold for detecting electrons is a density of about 0.001 cm-3. At times when the density is near this value all derived parameters are suspect. From 1621 to 1649 on Jan. 24 sunlight created an artificial signal so this data should be discarded. The LECP stepper motor is also creates a spurious signal in the PLS detector." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = 'URANUS' END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = 'TIME' SAMPLING_PARAMETER_RESOLUTION = 48.000000 MINIMUM_SAMPLING_PARAMETER = 'N/A' MAXIMUM_SAMPLING_PARAMETER = 'N/A' SAMPLING_PARAMETER_INTERVAL = 48.000000 MINIMUM_AVAILABLE_SAMPLING_INT= 48.000000 SAMPLING_PARAMETER_UNIT = 'SECOND' DATA_SET_PARAMETER_NAME = 'ELECTRON DENSITY' NOISE_LEVEL = 'N/A' DATA_SET_PARAMETER_UNIT = 'CM-3' END_OBJECT = DSPARMINFO OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = 'TIME' SAMPLING_PARAMETER_RESOLUTION = 48.000000 MINIMUM_SAMPLING_PARAMETER = 'N/A' MAXIMUM_SAMPLING_PARAMETER = 'N/A' SAMPLING_PARAMETER_INTERVAL = 48.000000 MINIMUM_AVAILABLE_SAMPLING_INT= 48.000000 SAMPLING_PARAMETER_UNIT = 'SECOND' DATA_SET_PARAMETER_NAME = 'ELECTRON TEMPERATURE' NOISE_LEVEL = 'N/A' DATA_SET_PARAMETER_UNIT = 'CM-3' END_OBJECT = DSPARMINFO OBJECT = SCDATASET INSTRUMENT_HOST_ID = 'VG2' INSTRUMENT_ID = 'PLS' END_OBJECT = SCDATASET OBJECT = DSREFINFO REFERENCE_KEY_ID = 'SITTLERETAL1987' OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = 'URANUS ELECTRONS' JOURNAL_NAME = 'JOURNAL OF GEOPHYSICAL RESEARCH' PUBLICATION_DATE = '1987' REFERENCE_DESC = " Sittler, E.C., Jr., K.W. Ogilvie and R.S. Selesnick, Survey of Electrons in the Uranian Magnetosphere: Voyager 2 Observations, J. Geophys. Res., 92, 15263-15281, 1987." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = 'E .C. SITTLER, JR.' END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = 'K. W. OGILVIE' END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = 'R. S. SELESNICK' END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /******************************************************************************/ /* MODIFICATIONS: */ /* 921001 EFRIED */ /* created template */ /* Template: Parameter Template Rev: 19890121 */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID = VG2 DATA_SET_PARAMETER_NAME = "ELECTRON DENSITY" INSTRUMENT_PARAMETER_NAME = "ELECTRON CURRENT" IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /*************** Electron Density Parm. Description Template ******************/ /* MODIFICATIONS: */ /* From: JPLPDS::RMONARREZ 6-AUG-1992 13:38:59.22 */ /* 92-08 EFRIED */ /* 920916 EFRIED */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM = 'ELECTRON DENSITY' DATA_SET_OR_INST_PARM_DESC = " A DERIVED PARAMETER EQUALING THE NUMBER OF ELECTRONS PER UNIT VOLUME OVER A SPECIFIED RANGE OF ELECTRON ENERGY. Different forms of electron density are derived distinguished by method of derivation (Maxwellian fit, method of moments) or by the some selection criteria (i.e., hot electron and cold electron density). In general, if more than one electron component is analyzed, either by moment or fit, a total density will be provided which is the sum of the electron densities. If the electron do not have a Maxwellian distribution the actual distribution can be represented as the sum of several Maxwellians, in which case the density of each Maxwellian is given." END_OBJECT = DSINSTPARMD /*************** Electron Current Parm. Description Template ******************/ /* MODIFICATIONS: */ /* From: JPLPDS::RMONARREZ 6-AUG-1992 13:38:59.22 */ /* 92-08 EFRIED */ /* 920916 EFRIED */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM = 'ELECTRON CURRENT' DATA_SET_OR_INST_PARM_DESC = " A measured parameter equaling the rate at which negative charge is collected by a particle detector. The electrons contributing to this current may be restricted by energy. Electrons always have a charge of 1, so this quantity corresponds directly to the electron rate." END_OBJECT = DSINSTPARMD /******************************************************************************/ /* MODIFICATIONS: */ /* 921028 SJOY */ /* created template */ /* Template: Parameter Template Rev: 19890121 */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID = VG2 DATA_SET_PARAMETER_NAME = "ELECTRON DENSITY" INSTRUMENT_PARAMETER_NAME = "ELECTRON RATE" IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /**************** Electron Rate Parameter Desc. Template ********************/ /* MODIFICATIONS: */ /* 921102 EFRIED */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM = "ELECTRON RATE" DATA_SET_OR_INST_PARM_DESC = " A measured parameter equaling the number of electrons hitting a particle detector per specified accumulation interval. The counted electrons may or may not be discriminated as to their energies (e.g. greater than E1, or between E1 and E2)." END_OBJECT = DSINSTPARMD /******************************************************************************/ /* MODIFICATIONS: */ /* 921028 SJOY */ /* created template */ /* Template: Parameter Template Rev: 19890121 */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID = VG2 DATA_SET_PARAMETER_NAME = "ELECTRON TEMPERATURE" INSTRUMENT_PARAMETER_NAME = "ELECTRON RATE" IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /******************************************************************************/ /* MODIFICATIONS: */ /* 921001 EFRIED */ /* created template */ /* Template: Parameter Template Rev: 19890121 */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID = VG2 DATA_SET_PARAMETER_NAME = "ELECTRON TEMPERATURE" INSTRUMENT_PARAMETER_NAME = "ELECTRON CURRENT" IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /*************** Electron Temperature Parm. Description Template **************/ /* MODIFICATIONS: */ /* From: JPLPDS::RMONARREZ 6-AUG-1992 13:38:59.22 */ /* 92-08 EFRIED */ /* 920916 EFRIED */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM = 'ELECTRON TEMPERATURE' DATA_SET_OR_INST_PARM_DESC = " A derived parameter giving an indication of the mean energy/electron, assuming the shape of the electron energy spectrum to be Maxwellian (i.e. highest entropy shape). Given that the electron energy spectrum is not exactly Maxwellian, the electron temperature can be defined integrally (whereby the mean energy obtained by integrating under the actual electron energy spectrum is set equal to the integral under a Maxwellian, where the temperature is a free parameter for which to solve), or differentially (whereby the slopes of the actually electron energy spectrum at various energies are matched to the slopes of a corresponding Maxwellian). The temperature parameter is often qualified with a range of applicable energies. temperatures can be angularly anisotropic. If the electrons do not have a Maxwellian distribution the actual distribution can be represented as the sum of several Maxwellians, each with a separate temperature." END_OBJECT = DSINSTPARMD /******************************************************************************/ /* MODIFICATIONS: */ /* 921001 EFRIED */ /* created template */ /* Template: Parameter Template Rev: 19890121 */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID = VG2 DATA_SET_PARAMETER_NAME = "ION DENSITY" INSTRUMENT_PARAMETER_NAME = "ION CURRENT" IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /****************** ION Density Parameter Desc. Template ********************/ /* MODIFICATIONS: */ /* From: JPLPDS::RMONARREZ 6-AUG-1992 13:38:59.22 */ /* 92-08 EFRIED */ /* 920916 EFRIED */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM = 'ION DENSITY' DATA_SET_OR_INST_PARM_DESC = " A derived parameter equaling the number of ions per unit volume over a specified range of ion energy, energy/charge, or energy/nucleon. Discrimination with regard to mass and or charge state is necessary to obtain this quantity, however, mass and charge state are often assumed due to instrument limitations. Many different forms of ion density are derived. Some are distinguished by their composition (N+, proton, ion, etc.) or their method of derivation (Maxwellian fit, method of moments). In some cases, more than one type of density will be provided in a single dataset. In general, if more than one ion species is analyzed, either by moment or fit, a total density will be provided which is the sum of the ion densities. If a plasma component does not have a Maxwellian distribution the actual distribution can be represented as the sum of several Maxwellians, in which case the density of each Maxwellian is given." END_OBJECT = DSINSTPARMD /*************** Ion Current Parm. Description Template ***********************/ /* MODIFICATIONS: */ /* 921001 EFRIED */ /* created template */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM = "ION CURRENT" DATA_SET_OR_INST_PARM_DESC = " A measured parameter equaling the rate at which positive charge is collected by a particle detector. The ions contributing to this current may be restricted by energy and/or mass. Since ion charge states may be greater than one, this quantity generally is greater than the corresponding ion rate." END_OBJECT = DSINSTPARMD /******************************************************************************/ /* MODIFICATIONS: */ /* 921001 EFRIED */ /* created template */ /* Template: Parameter Template Rev: 19890121 */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID = VG2 DATA_SET_PARAMETER_NAME = "ION THERMAL SPEED" INSTRUMENT_PARAMETER_NAME = "ION CURRENT" IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /*********** ION Thermal Speed Parm. Description Template *********************/ /* MODIFICATIONS: */ /* From: JPLPDS::RMONARREZ 6-AUG-1992 13:38:59.22 */ /* 92-08 EFRIED */ /* 920916 EFRIED */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM = 'ION THERMAL SPEED' DATA_SET_OR_INST_PARM_DESC = " ION THERMAL SPEED: A measure of the velocity associated with the temperature of the ions. It is formally defined as the Ion Thermal Speed squared equals two times K (Boltzmann's constant) times T (temperature of ion) divided by M (ion mass). Each component of a plasma has a thermal speed associated with it." END_OBJECT = DSINSTPARMD /******************************************************************************/ /* MODIFICATIONS: */ /* 921001 EFRIED */ /* created template */ /* Template: Parameter Template Rev: 19890121 */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID = VG2 DATA_SET_PARAMETER_NAME = "ION TEMPERATURE" INSTRUMENT_PARAMETER_NAME = "ION CURRENT" IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /*************** Ion Temperature Parm. Description Template *******************/ /* MODIFICATIONS: */ /* 921001 EFRIED */ /* created template from electron temperature (electron -> ion) */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM = 'ION TEMPERATURE' DATA_SET_OR_INST_PARM_DESC = " A derived parameter giving an indication of the mean energy/ion, assuming the shape of the ion energy spectrum to be Maxwellian (i.e. highest entropy shape). Given that the ion energy spectrum is not exactly Maxwellian, the ion temperature can be defined integrally (whereby the mean energy obtained by integrating under the actual ion energy spectrum is set equal to the integral under a Maxwellian, where the temperature is a free parameter for which to solve), or differentially (whereby the slopes of the actually ion energy spectrum at various energies are matched to the slopes of a corresponding Maxwellian). The temperature parameter is often qualified with a range of applicable energies. temperatures can be angularly anisotropic. If the ions do not have a Maxwellian distribution the actual distribution can be represented as the sum of several Maxwellians, each with a separate temperature." END_OBJECT = DSINSTPARMD /******************************************************************************/ /* MODIFICATIONS: */ /* 921001 EFRIED */ /* created template */ /* Template: Parameter Template Rev: 19890121 */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID = VG2 DATA_SET_PARAMETER_NAME = "ION VELOCITY" INSTRUMENT_PARAMETER_NAME = "ION CURRENT" IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /************ ION Velocity Parm Description Template **************************/ /* MODIFICATIONS: */ /* From: JPLPDS::RMONARREZ 6-AUG-1992 13:38:59.22 */ /* 92-08 EFRIED */ /* 920916 EFRIED */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM = 'ION VELOCITY' DATA_SET_OR_INST_PARM_DESC = " A derived parameter giving the average speed and direction of motion of a plasma or plasma component. The velocity can be obtained by taking the first moment of the distribution function or by simulating the observations with some known distribution function, usually a Maxwellian, to the distribution. Velocities may be given in any of the following coordinate systems: RTN coordinate system: R is radially away from sun, T is in plane of sun's equator and positive in the direction of solar rotation N completes right-handed system rho, phi, z (cylindrical) rho is radial distance from the planet's spin axis phi is parallel to spin equator and perpendicular to rho and positive in direction of planetary rotation. z completes right-handed system parallel, perpendicular: parallel or perpendicular to the magnetic field direction." END_OBJECT = DSINSTPARMD /*************** POS HG 48SEC DATASET TEMPLATE ********************************/ /* MODIFICATIONS: */ /* 921028 -- SJOY */ /* created template */ /* 921103 -- EFRIED */ /* last modifications */ /* Template: Spacecraft Data Set Template Rev: 19890121 */ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-POS-5-SUMM-HGCOORDS-48SEC-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA TRAJECTORY DERIV SUMM HELIOGRAPHIC COORDS 48SEC V1.0" DATA_SET_COLLECTION_MEMBER_FLG = N START_TIME = 1989-08-22T00:00:00.319 STOP_TIME = 1989-08-29T23:59:11.365 NATIVE_START_TIME = "26735:22:001" NATIVE_STOP_TIME = "27035:59:001" DATA_OBJECT_TYPE = TIME_SERIES DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = 4 PRODUCER_FULL_NAME = "DR. RONALD J. LEPPING" PRODUCER_INSTITUTION_NAME = "GODDARD SPACE FLIGHT CENTER" SOFTWARE_FLAG = Y DETAILED_CATALOG_FLAG = Y PROCESSING_START_TIME = UNK PROCESSING_STOP_TIME = UNK DATA_SET_DESC = " This dataset contains Voyager 2 position vectors relative to the Sun in both cartesian and spherical Heliographic coordinates for the time when Voyager 2 was near Uranus but not within its magnetosphere. The position vectors are given every 48 seconds. The units of the vector components are Au and degrees. Vectors are stored as 4-byte floating point values. The Heliographic coordinate system is defined in the reference epoch of 1950. The unit vectors which define the coordinate system are as follows: X points away from the Sun towards the ascending node, in the solar equatorial plane, Z points along the Sun's spin axis, positive above the equatorial plane, and Y completes the right handed set." CONFIDENCE_LEVEL_NOTE = " This dataset was provided by the Voyager Magnetometer team. There is a significant problem with loss of precision in the spacecraft position. This is not an artifact of the Mag teams processing or handling of the data but in the precision of the Supplemental Experimenter Data Records (SEDR) for Voyager." END_OBJECT = DATASETINFO /* Template: Data Set Target Template Rev: 19890121 */ /* Note: This template shall be repeated for each */ /* target associated with the data set id in */ /* the dataset template. */ OBJECT = DATASETTARG TARGET_NAME = URANUS END_OBJECT = DATASETTARG /* Template: Data Set Parameter Information Template Rev: 19890121 */ /* Note: This template shall be repeated for each */ /* dataset sampling parameter pair utilized */ /* by the dataset id in the dataset template. */ OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = 96.0 MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 48.0 MINIMUM_AVAILABLE_SAMPLING_INT = 48.0 SAMPLING_PARAMETER_UNIT = SECONDS DATA_SET_PARAMETER_NAME = "POSITION VECTOR" NOISE_LEVEL = "N/A" DATA_SET_PARAMETER_UNIT = "AU OR DEGREES" END_OBJECT = DSPARMINFO /* Template: Spacecraft Data Set Host Template Rev: 19890121 */ /* Note: This template shall be completed if the */ /* data set in the dataset template is */ /* associated with a spacecraft. */ OBJECT = SCDSHOST INSTRUMENT_HOST_ID = "VG2" INSTRUMENT_ID = "POS" END_OBJECT = SCDSHOST /* Template: Data Set Reference Information Template Rev: 19890121 */ /* Note: The following templates form part of a standard */ /* set for the submission of a publication reference */ /* to the PDS and also may be used to reference an */ /* existing publication reference. */ OBJECT = DSREFINFO REFERENCE_KEY_ID = "UNK" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "N/A" JOURNAL_NAME = "N/A" PUBLICATION_DATE = "N/A" REFERENCE_DESC = "N/A" OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N/A" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /*************** U1 48SEC DATASET TEMPLATE ************************************/ /* MODIFICATIONS: */ /* 921028 -- SJOY */ /* created template */ /* 921103 -- EFRIED */ /* last modifications */ /* Template: Spacecraft Data Set Template Rev: 19890121 */ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-POS-5-SUMM-U1COORDS-48SEC-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA TRAJECTORY DERIVED SUMM U1 COORDS 48SEC V1.0" DATA_SET_COLLECTION_MEMBER_FLG = N START_TIME = 1986-01-24T06:59:12.005 STOP_TIME = 1986-01-25T04:00:47.921 NATIVE_START_TIME = "26834:07:001" NATIVE_STOP_TIME = "26860:21:001" DATA_OBJECT_TYPE = TIME_SERIES DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = 4 PRODUCER_FULL_NAME = "DR. RONALD J. LEPPING" PRODUCER_INSTITUTION_NAME = "GODDARD SPACE FLIGHT CENTER" SOFTWARE_FLAG = Y DETAILED_CATALOG_FLAG = Y PROCESSING_START_TIME = UNK PROCESSING_STOP_TIME = UNK DATA_SET_DESC = " This dataset contains Voyager 2 spacecraft position vectors relative ^M to Uranus in minus U1 coordinates. The U1 or Uranus West Longitude ^M System coordinate system is a planetocentric system fixed to Uranus ^M which is rotating with a 17.24 hour period. ^M ^M The prime meridian of the this system is defined such that at^M 1986-01-24T18:00:00.000 the Voyager 2 spacecraft was at 302^M degrees west longitude (58 degrees east longitude).^M ^M For the PDS archive dataset, the original data archive has been^M converted to an east longitude (righthanded) coordinate ^M system minus U1 (-U1). This is achieved by subtracting the ^M U1 longitude from 360.0 degrees. The data are provided in units^M of Uranian radii which was taken to be 25,600km by the Voyager ^M project. Angles are given in degrees. Both cartesian and spherical^M coordinates are provided."^M ^M The Cartesian coordinate system is defined as follows:^M - X lies in the equatorial plane of Uranus, positive away from the ^M planet, and through the prime meridian at the reference epoch.^M - Z is parallel to the Uranus spin axis, positive in the southern ^M hemisphere in ecliptic (orbital) coordinates, and,^M - Y is Z x X (righthanded)^M ^M The Cartesian coordinate system does not rotate with the planet.^M CONFIDENCE_LEVEL_NOTE = " There is no dataset confidence information archived with this dataset. The data provider has included a flag value which is included in the mag dataset which may reduce confidence in individual vectors due to telemetry or software errors." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = URANUS END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = 96.0 MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 48.0 MINIMUM_AVAILABLE_SAMPLING_INT = 48.0 SAMPLING_PARAMETER_UNIT = SECONDS DATA_SET_PARAMETER_NAME = "POSITION VECTOR" NOISE_LEVEL = "N/A" DATA_SET_PARAMETER_UNIT = "URANUS RADII (25,600km) OR DEGREES" END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = VG2 INSTRUMENT_ID = POS END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = "CONNERNEYETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Connerney, J.E.P., M.H. Acuna, and N.F. Ness, The Magnetic Field of Uranus, J. Geophys. Res., 92, 336, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "JOHN E.P. CONNERNEY" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /********************* HG COORDS TEMPLATE *************************************/ /* MODIFICATIONS: */ /* 921028 -- SJOY */ /* created template */ /* Template: Coordinate System Template Rev: 19890121 */ /* Note: The following templates form part of a standard */ /* set for the submission of a Coordinate System */ /* to the PDS. */ /* Hierarchy: COORDINATE */ /* COORDINFO */ /* VECTOR */ /* VECTORCOMP */ /* VECTORD */ OBJECT = COORDINATE COORDINATE_SYSTEM_ID = HG OBJECT = COORDINFO COORDINATE_SYSTEM_NAME = "MEAN INERTIAL HG 1950" COORDINATE_SYSTEM_CENTER_NAME = SUN COORDINATE_SYSTEM_REF_EPOCH = "UNK" /* 09-23-1950 */ COORDINATE_SYSTEM_DESC = " The Heliographic coordinate system is defined in the reference epoch of 1950. The unit vectors which define the coordinate system are as follows: X points away from the Sun towards the ascending node, in the solar equatorial plane, Z points along the Sun's spin axis, positive above the equatorial plane, and Y completes the right handed set." END_OBJECT = COORDINFO OBJECT = VECTOR VECTOR_COMPONENT_TYPE = RANGE OBJECT = VECTORCOMP VECTOR_COMPONENT_ID = R REFERENCE_OBJECT_NAME = SUN REFERENCE_TARGET_NAME = SPACECRAFT VECTOR_COMPONENT_UNIT = AU END_OBJECT = VECTORCOMP OBJECT = VECTORD VECTOR_COMPONENT_TYPE_DESC = " The range or R component of the spherical Heliographic coordinate system is the distance from the Sun's position at the reference epoch to the spacecraft measured in AU." END_OBJECT = VECTORD END_OBJECT = VECTOR OBJECT = VECTOR VECTOR_COMPONENT_TYPE = LATITUDE OBJECT = VECTORCOMP VECTOR_COMPONENT_ID = LAT REFERENCE_OBJECT_NAME = SUN REFERENCE_TARGET_NAME = SPACECRAFT VECTOR_COMPONENT_UNIT = DEGREES END_OBJECT = VECTORCOMP OBJECT = VECTORD VECTOR_COMPONENT_TYPE_DESC = " The latitude component of the the spherical Heliographic coordinate system is the angle between the solar equatorial plane of the reference epoch measured in the plane that contains the solar spin axis of that epoch." END_OBJECT = VECTORD END_OBJECT = VECTOR OBJECT = VECTOR VECTOR_COMPONENT_TYPE = LONGITUDE OBJECT = VECTORCOMP VECTOR_COMPONENT_ID = LONG REFERENCE_OBJECT_NAME = SUN REFERENCE_TARGET_NAME = SPACECRAFT VECTOR_COMPONENT_UNIT = DEGREES END_OBJECT = VECTORCOMP OBJECT = VECTORD VECTOR_COMPONENT_TYPE_DESC = " The longitude component of the spherical Heliographic coordinate system is zero in the direction of the ascending node at the reference epoch (X direction) and increases for a body orbiting the Sun as the Earth does." END_OBJECT = VECTORD END_OBJECT = VECTOR OBJECT = VECTOR VECTOR_COMPONENT_TYPE = X OBJECT = VECTORCOMP VECTOR_COMPONENT_ID = X REFERENCE_OBJECT_NAME = SUN REFERENCE_TARGET_NAME = "ASCENDING NODE" VECTOR_COMPONENT_UNIT = AU END_OBJECT = VECTORCOMP OBJECT = VECTORD VECTOR_COMPONENT_TYPE_DESC = " The X component of the Heliographic coordinate system points away from the Sun, towards the ascending node, and lies in the solar equatorial plane." END_OBJECT = VECTORD END_OBJECT = VECTOR OBJECT = VECTOR VECTOR_COMPONENT_TYPE = Y OBJECT = VECTORCOMP VECTOR_COMPONENT_ID = Y REFERENCE_OBJECT_NAME = SUN REFERENCE_TARGET_NAME = "N/A" VECTOR_COMPONENT_UNIT = AU END_OBJECT = VECTORCOMP OBJECT = VECTORD VECTOR_COMPONENT_TYPE_DESC = " The Y vector of the Heliographic coordinate system is formed by the righthanded cross product of the X and Z unit vectors. It lies in the solar equatorial plane and it points away from the Sun, but does not extend in the direction of any particular body." END_OBJECT = VECTORD END_OBJECT = VECTOR OBJECT = VECTOR VECTOR_COMPONENT_TYPE = Z OBJECT = VECTORCOMP VECTOR_COMPONENT_ID = Z REFERENCE_OBJECT_NAME = SUN REFERENCE_TARGET_NAME = "SUN SPIN AXIS" VECTOR_COMPONENT_UNIT = AU END_OBJECT = VECTORCOMP OBJECT = VECTORD VECTOR_COMPONENT_TYPE_DESC = " The Z component of the Heliographic coordinate system is parallel to the Sun's spin axis, taken as positive above the equatorial plane of the Sun." END_OBJECT = VECTORD END_OBJECT = VECTOR END_OBJECT = COORDINATE /********************* U1 COORDS TEMPLATE *************************************/ /* MODIFICATIONS: */ /* 921028 -- SJOY */ /* created template */ /* Template: Coordinate System Template Rev: 19890121 */ /* Note: The following templates form part of a standard */ /* set for the submission of a Coordinate System */ /* to the PDS. */ /* Hierarchy: COORDINATE */ /* COORDINFO */ /* VECTOR */ /* VECTORCOMP */ /* VECTORD */ OBJECT = COORDINATE COORDINATE_SYSTEM_ID = U1 OBJECT = COORDINFO COORDINATE_SYSTEM_NAME = "URANUS WEST LONGITUDE SYSTEM" COORDINATE_SYSTEM_CENTER_NAME = "URANUS" COORDINATE_SYSTEM_REF_EPOCH = "1986-01-24:18:00:00.000" COORDINATE_SYSTEM_DESC = " Planetary longitudes are based on a 17.24 hour rotation period (Connerney et al., 1987) adopted by the Voyager Project shortly after the encounter. The zero longitude is defined by the requirement that the West Longitude of the spacecraft at 1800 SCET day 24 (near closest approach) be 302 degrees U1; West Longitudes of the Uranus Longitude System (U1) are simply related to the angle PHI: WLONG = 360. - PHI (degrees) This definition of the zero longitude was adopted by the Voyager Project Steering Group in order to minimize differences in longitudes resulting from changes in the assumed rotation period. " END_OBJECT = COORDINFO OBJECT = VECTOR VECTOR_COMPONENT_TYPE = RANGE OBJECT = VECTORCOMP VECTOR_COMPONENT_ID = R REFERENCE_OBJECT_NAME = URANUS REFERENCE_TARGET_NAME = VOYAGER VECTOR_COMPONENT_UNIT = "RU (Ru = 25,600km)" END_OBJECT = VECTORCOMP OBJECT = VECTORD VECTOR_COMPONENT_TYPE_DESC = " Range from the planet center to the spacecraft in units of Ru where Ru = 25,600km." END_OBJECT = VECTORD END_OBJECT = VECTOR OBJECT = VECTOR VECTOR_COMPONENT_TYPE = LATITUDE OBJECT = VECTORCOMP VECTOR_COMPONENT_ID = LAT REFERENCE_OBJECT_NAME = URANUS REFERENCE_TARGET_NAME = VOYAGER VECTOR_COMPONENT_UNIT = DEGREES END_OBJECT = VECTORCOMP OBJECT = VECTORD VECTOR_COMPONENT_TYPE_DESC = " Spacecraft latitude in degrees. Valid range -90.0 -> +90.0." END_OBJECT = VECTORD END_OBJECT = VECTOR OBJECT = VECTOR VECTOR_COMPONENT_TYPE = LONGITUDE OBJECT = VECTORCOMP VECTOR_COMPONENT_ID = W_LONG REFERENCE_OBJECT_NAME = URANUS REFERENCE_TARGET_NAME = VOYAGER VECTOR_COMPONENT_UNIT = DEGREES END_OBJECT = VECTORCOMP OBJECT = VECTORD VECTOR_COMPONENT_TYPE_DESC = " West longitude where the zero longitude is defined by the requirement that the West Longitude of Voyager 2 at 1986-01-24T18:00:00.00 was 302.0 degrees." END_OBJECT = VECTORD END_OBJECT = VECTOR END_OBJECT = COORDINATE /********************* Uranus 48 Second Browse Data ***************************/ /* MODIFICATIONS */ /* 920831 -- JPLPDS::RMONARREZ */ /* received by mail */ /* 920914 -- EFRIED */ /* 920918 -- EFRIED */ /* updated Data Set templates according to new std. */ /* Data Set Template -> Spacecraft Data Set Template */ /* event_start_time, event_stop_time -> start_time, stop_time */ /* 920922 -- EFRIED */ /* Revised DATA_SET_ID and DATA_SET_NAME */ /* 021002 -- EFRIED */ /* Revised DATA_SET_PARAMETER_NAME */ /* last changes made /* Template: Spacecraft Data Set Template Rev: 19890121 */ /* */ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-PRA-4-SUMM-BROWSE-48SEC-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA PRA RESAMPLED SUMMARY BROWSE 48SEC V1.0" DATA_SET_COLLECTION_MEMBER_FLG = N START_TIME = 1986-01-19T00:00:00.000 STOP_TIME = 1986-01-31T23:59:59.999 NATIVE_START_TIME = "N/A" NATIVE_STOP_TIME = "N/A" DATA_OBJECT_TYPE = "TIME SERIES" DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = 4 PRODUCER_FULL_NAME = "DR. DAVID R. EVANS" PRODUCER_INSTITUTION_NAME = "RADIOPHYSICS, INCORPORATED" SOFTWARE_FLAG = "Y" DETAILED_CATALOG_FLAG = "N" PROCESSING_START_TIME = "UNK" PROCESSING_STOP_TIME = 1991-07-30 DATA_SET_DESC = " This dataset consists of edited browse data derived from an original dataset obtained from the Voyager 2 Planetary Radio Astronomy (PRA) instrument in the vicinity of Uranus. 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 1986:019:00:00 through 1986:031:23:59. In order to produce this dataset 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 dataset; 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 milliBels (mB) about a reference flux density. The value of 0 mB represents a voltage of 1 microvolt across the front end of the receiver. To convert a returned quantity to flux, use the formula: flux = 7.0x10^(-22)x10^(Mb/1000) W m-2 Hz-1" CONFIDENCE_LEVEL_NOTE = " This dataset 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 dataset. The two most obvious examples of this interference are low-frequency spikes which occur every twelve minutes throughout the dataset (due to LECP operation), and a strong, wandering interference (from PPS) that occurs in the range 200 to 600 kHz at various times throughout the encounter. An example of the latter is to be found at 1986-01-24 09:00:00 SCET. The separation into Left Hand Circular (LHC) and Right Hand Circular (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. The table below has been produced using a wire-frame model of the spacecraft comprising 168 separate elements, and derived using the method of moments procedure. IT IS ONLY A MODEL, not a measurement; but appears to be very accurate for the low band of the PRA instrument. THETA PHI AFP 0 0 -0.99960 10 0 -0.99727 10 10 -0.99723 10 20 -0.99715 10 30 -0.99706 10 40 -0.99696 10 50 -0.99688 10 60 -0.99681 10 70 -0.99679 10 80 -0.99683 10 90 -0.99692 10 100 -0.99708 10 110 -0.99729 10 120 -0.99754 10 130 -0.99782 10 140 -0.99809 10 150 -0.99832 10 160 -0.99851 10 170 -0.99862 10 180 -0.99866 10 190 -0.99862 10 200 -0.99850 10 210 -0.99833 10 220 -0.99812 10 230 -0.99789 10 240 -0.99767 10 250 -0.99747 10 260 -0.99730 10 270 -0.99719 10 280 -0.99711 10 290 -0.99709 10 300 -0.99710 10 310 -0.99713 10 320 -0.99718 10 330 -0.99723 10 340 -0.99727 10 350 -0.99728 20 0 -0.99613 20 10 -0.99591 20 20 -0.99537 20 30 -0.99455 20 40 -0.99350 20 50 -0.99228 20 60 -0.99099 20 70 -0.98969 20 80 -0.98849 20 90 -0.98744 20 100 -0.98661 20 110 -0.98600 20 120 -0.98562 20 130 -0.98541 20 140 -0.98534 20 150 -0.98534 20 160 -0.98535 20 170 -0.98533 20 180 -0.98528 20 190 -0.98519 20 200 -0.98512 20 210 -0.98510 20 220 -0.98520 20 230 -0.98546 20 240 -0.98590 20 250 -0.98655 20 260 -0.98738 20 270 -0.98837 20 280 -0.98949 20 290 -0.99068 20 300 -0.99189 20 310 -0.99305 20 320 -0.99410 20 330 -0.99499 20 340 -0.99565 20 350 -0.99604 30 0 -0.99745 30 10 -0.99686 30 20 -0.99529 30 30 -0.99278 30 40 -0.98942 30 50 -0.98537 30 60 -0.98080 30 70 -0.97595 30 80 -0.97102 30 90 -0.96622 30 100 -0.96171 30 110 -0.95763 30 120 -0.95404 30 130 -0.95098 30 140 -0.94842 30 150 -0.94634 30 160 -0.94475 30 170 -0.94365 30 180 -0.94309 30 190 -0.94316 30 200 -0.94395 30 210 -0.94551 30 220 -0.94785 30 230 -0.95095 30 240 -0.95471 30 250 -0.95900 30 260 -0.96367 30 270 -0.96853 30 280 -0.97344 30 290 -0.97823 30 300 -0.98277 30 310 -0.98691 30 320 -0.99052 30 330 -0.99349 30 340 -0.99570 30 350 -0.99704 40 0 -0.99973 40 10 -0.99855 40 20 -0.99515 40 30 -0.98957 40 40 -0.98198 40 50 -0.97261 40 60 -0.96178 40 70 -0.94988 40 80 -0.93730 40 90 -0.92446 40 100 -0.91170 40 110 -0.89936 40 120 -0.88770 40 130 -0.87697 40 140 -0.86741 40 150 -0.85926 40 160 -0.85286 40 170 -0.84853 40 180 -0.84663 40 190 -0.84741 40 200 -0.85100 40 210 -0.85732 40 220 -0.86608 40 230 -0.87684 40 240 -0.88906 40 250 -0.90218 40 260 -0.91567 40 270 -0.92906 40 280 -0.94198 40 290 -0.95413 40 300 -0.96525 40 310 -0.97514 40 320 -0.98362 40 330 -0.99049 40 340 -0.99557 40 350 -0.99870 50 0 -0.99822 50 10 -0.99614 50 20 -0.98981 50 30 -0.97929 50 40 -0.96479 50 50 -0.94669 50 60 -0.92548 50 70 -0.90173 50 80 -0.87609 50 90 -0.84919 50 100 -0.82165 50 110 -0.79406 50 120 -0.76705 50 130 -0.74130 50 140 -0.71760 50 150 -0.69696 50 160 -0.68052 50 170 -0.66947 50 180 -0.66488 50 190 -0.66738 50 200 -0.67706 50 210 -0.69334 50 220 -0.71512 50 230 -0.74097 50 240 -0.76936 50 250 -0.79890 50 260 -0.82839 50 270 -0.85690 50 280 -0.88375 50 290 -0.90848 50 300 -0.93074 50 310 -0.95028 50 320 -0.96683 50 330 -0.98017 50 340 -0.99002 50 350 -0.99612 60 0 -0.98327 60 10 -0.97987 60 20 -0.96916 60 30 -0.95122 60 40 -0.92640 60 50 -0.89528 60 60 -0.85861 60 70 -0.81728 60 80 -0.77225 60 90 -0.72447 60 100 -0.67489 60 110 -0.62449 60 120 -0.57437 60 130 -0.52585 60 140 -0.48065 60 150 -0.44091 60 160 -0.40915 60 170 -0.38792 60 180 -0.37938 60 190 -0.38472 60 200 -0.40386 60 210 -0.43537 60 220 -0.47683 60 230 -0.52529 60 240 -0.57777 60 250 -0.63164 60 260 -0.68479 60 270 -0.73567 60 280 -0.78320 60 290 -0.82667 60 300 -0.86562 60 310 -0.89966 60 320 -0.92846 60 330 -0.95165 60 340 -0.96880 60 350 -0.97948 70 0 -0.93784 70 10 -0.93265 70 20 -0.91587 70 30 -0.88772 70 40 -0.84885 70 50 -0.80029 70 60 -0.74333 70 70 -0.67940 70 80 -0.61001 70 90 -0.53664 70 100 -0.46074 70 110 -0.38380 70 120 -0.30751 70 130 -0.23393 70 140 -0.16570 70 150 -0.10605 70 160 -0.58708E-01 70 170 -0.27369E-01 70 180 -0.15059E-01 70 190 -0.23404E-01 70 200 -0.52162E-01 70 210 -0.99231E-01 70 220 -0.16109 70 230 -0.23348 70 240 -0.31212 70 250 -0.39319 70 260 -0.47360 70 270 -0.55104 70 280 -0.62388 70 290 -0.69098 70 300 -0.75152 70 310 -0.80483 70 320 -0.85026 70 330 -0.88706 70 340 -0.91444 70 350 -0.93161 80 0 -0.83577 80 10 -0.82843 80 20 -0.80429 80 30 -0.76395 80 40 -0.70874 80 50 -0.64057 80 60 -0.56170 80 70 -0.47456 80 80 -0.38152 80 90 -0.28485 80 100 -0.18662 80 110 -0.88899E-01 80 120 0.61719E-02 80 130 0.96112E-01 80 140 0.17796 80 150 0.24824 80 160 0.30315 80 170 0.33897 80 180 0.35274 80 190 0.34287 80 200 0.30954 80 210 0.25477 80 220 0.18202 80 230 0.95629E-01 80 240 0.14867E-03 80 250 -0.10017 80 260 -0.20167 80 270 -0.30144 80 280 -0.39722 80 290 -0.48725 80 300 -0.57007 80 310 -0.64432 80 320 -0.70863 80 330 -0.76146 80 340 -0.80125 80 350 -0.82644 90 0 -0.64612 90 10 -0.63686 90 20 -0.60599 90 30 -0.55482 90 40 -0.48577 90 50 -0.40206 90 60 -0.30732 90 70 -0.20513 90 80 -0.98827E-01 90 90 0.86836E-02 90 100 0.11490 90 110 0.21763 90 120 0.31479 90 130 0.40422 90 140 0.48353 90 150 0.55008 90 160 0.60105 90 170 0.63378 90 180 0.64612 90 190 0.63686 90 200 0.60599 90 210 0.55482 90 220 0.48577 90 230 0.40206 90 240 0.30732 90 250 0.20513 90 260 0.98827E-01 90 270 -0.86834E-02 90 280 -0.11490 90 290 -0.21763 90 300 -0.31479 90 310 -0.40422 90 320 -0.48353 90 330 -0.55008 90 340 -0.60105 90 350 -0.63378 100 0 -0.35274 100 10 -0.34287 100 20 -0.30954 100 30 -0.25477 100 40 -0.18202 100 50 -0.95629E-01 100 60 -0.14887E-03 100 70 0.10017 100 80 0.20167 100 90 0.30144 100 100 0.39722 100 110 0.48725 100 120 0.57007 100 130 0.64433 100 140 0.70863 100 150 0.76146 100 160 0.80125 100 170 0.82644 100 180 0.83577 100 190 0.82843 100 200 0.80429 100 210 0.76395 100 220 0.70874 100 230 0.64057 100 240 0.56170 100 250 0.47456 100 260 0.38152 100 270 0.28485 100 280 0.18662 100 290 0.88899E-01 100 300 -0.61720E-02 100 310 -0.96112E-01 100 320 -0.17796 100 330 -0.24824 100 340 -0.30315 100 350 -0.33896 110 0 0.15059E-01 110 10 0.23404E-01 110 20 0.52161E-01 110 30 0.99231E-01 110 40 0.16109 110 50 0.23348 110 60 0.31212 110 70 0.39319 110 80 0.47360 110 90 0.55104 110 100 0.62388 110 110 0.69098 110 120 0.75152 110 130 0.80483 110 140 0.85026 110 150 0.88706 110 160 0.91444 110 170 0.93161 110 180 0.93784 110 190 0.93265 110 200 0.91587 110 210 0.88772 110 220 0.84885 110 230 0.80029 110 240 0.74333 110 250 0.67940 110 260 0.61001 110 270 0.53664 110 280 0.46074 110 290 0.38380 110 300 0.30751 110 310 0.23393 110 320 0.16570 110 330 0.10605 110 340 0.58708E-01 110 350 0.27369E-01 120 0 0.37938 120 10 0.38472 120 20 0.40386 120 30 0.43537 120 40 0.47683 120 50 0.52529 120 60 0.57777 120 70 0.63164 120 80 0.68479 120 90 0.73567 120 100 0.78320 120 110 0.82667 120 120 0.86562 120 130 0.89966 120 140 0.92846 120 150 0.95165 120 160 0.96880 120 170 0.97948 120 180 0.98327 120 190 0.97987 120 200 0.96916 120 210 0.95122 120 220 0.92640 120 230 0.89528 120 240 0.85861 120 250 0.81728 120 260 0.77225 120 270 0.72447 120 280 0.67489 120 290 0.62449 120 300 0.57437 120 310 0.52585 120 320 0.48065 120 330 0.44091 120 340 0.40915 120 350 0.38792 130 0 0.66488 130 10 0.66738 130 20 0.67706 130 30 0.69334 130 40 0.71512 130 50 0.74096 130 60 0.76936 130 70 0.79890 130 80 0.82839 130 90 0.85690 130 100 0.88375 130 110 0.90848 130 120 0.93074 130 130 0.95028 130 140 0.96683 130 150 0.98017 130 160 0.99002 130 170 0.99612 130 180 0.99822 130 190 0.99614 130 200 0.98981 130 210 0.97929 130 220 0.96479 130 230 0.94669 130 240 0.92548 130 250 0.90173 130 260 0.87609 130 270 0.84919 130 280 0.82165 130 290 0.79406 130 300 0.76705 130 310 0.74130 130 320 0.71760 130 330 0.69696 130 340 0.68052 130 350 0.66947 140 0 0.84663 140 10 0.84741 140 20 0.85100 140 30 0.85732 140 40 0.86608 140 50 0.87684 140 60 0.88906 140 70 0.90218 140 80 0.91567 140 90 0.92906 140 100 0.94198 140 110 0.95413 140 120 0.96525 140 130 0.97514 140 140 0.98362 140 150 0.99049 140 160 0.99557 140 170 0.99870 140 180 0.99973 140 190 0.99855 140 200 0.99515 140 210 0.98957 140 220 0.98198 140 230 0.97261 140 240 0.96178 140 250 0.94988 140 260 0.93730 140 270 0.92446 140 280 0.91170 140 290 0.89936 140 300 0.88770 140 310 0.87697 140 320 0.86741 140 330 0.85926 140 340 0.85286 140 350 0.84853 150 0 0.94309 150 10 0.94316 150 20 0.94395 150 30 0.94551 150 40 0.94785 150 50 0.95095 150 60 0.95471 150 70 0.95900 150 80 0.96367 150 90 0.96853 150 100 0.97344 150 110 0.97823 150 120 0.98277 150 130 0.98691 150 140 0.99052 150 150 0.99349 150 160 0.99570 150 170 0.99704 150 180 0.99745 150 190 0.99686 150 200 0.99529 150 210 0.99278 150 220 0.98942 150 230 0.98537 150 240 0.98080 150 250 0.97595 150 260 0.97102 150 270 0.96622 150 280 0.96171 150 290 0.95763 150 300 0.95404 150 310 0.95098 150 320 0.94842 150 330 0.94634 150 340 0.94475 150 350 0.94365 160 0 0.98528 160 10 0.98519 160 20 0.98512 160 30 0.98510 160 40 0.98520 160 50 0.98546 160 60 0.98590 160 70 0.98655 160 80 0.98738 160 90 0.98837 160 100 0.98949 160 110 0.99068 160 120 0.99189 160 130 0.99305 160 140 0.99410 160 150 0.99499 160 160 0.99565 160 170 0.99604 160 180 0.99613 160 190 0.99591 160 200 0.99537 160 210 0.99455 160 220 0.99350 160 230 0.99228 160 240 0.99099 160 250 0.98969 160 260 0.98849 160 270 0.98744 160 280 0.98661 160 290 0.98600 160 300 0.98562 160 310 0.98541 160 320 0.98534 160 330 0.98534 160 340 0.98535 160 350 0.98533 170 0 0.99866 170 10 0.99862 170 20 0.99850 170 30 0.99833 170 40 0.99812 170 50 0.99789 170 60 0.99767 170 70 0.99747 170 80 0.99730 170 90 0.99719 170 100 0.99711 170 110 0.99709 170 120 0.99710 170 130 0.99713 170 140 0.99718 170 150 0.99723 170 160 0.99727 170 170 0.99728 170 180 0.99727 170 190 0.99723 170 200 0.99715 170 210 0.99706 170 220 0.99696 170 230 0.99688 170 240 0.99681 170 250 0.99679 170 260 0.99683 170 270 0.99692 170 280 0.99708 170 290 0.99729 170 300 0.99754 170 310 0.99782 170 320 0.99809 170 330 0.99832 170 340 0.99851 170 350 0.99862 180 0 0.99960" END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = "URANUS" END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = "TIME" SAMPLING_PARAMETER_RESOLUTION = 0.001 MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 48.0 MINIMUM_AVAILABLE_SAMPLING_INT = 12.0 SAMPLING_PARAMETER_UNIT = "SECOND" DATA_SET_PARAMETER_NAME = "RADIO WAVE SPECTRUM" NOISE_LEVEL = 2400 DATA_SET_PARAMETER_UNIT = "MILLIBEL" END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = "VG2" INSTRUMENT_ID = "PRA" END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = "WARWICKETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "VG2 PRA URANUS OVERVIEW" JOURNAL_NAME = "SCIENCE" PUBLICATION_DATE = 1986-07-04 REFERENCE_DESC = " Warwick, J.W., D.R. Evans, J.H. Romig, C.B. Sawyer, M.D. Desch, M.L. Kaiser, J.K. Alexander, T.D. Carr, D.H. Staelin, S. Gulkis, R.L. Poynter, M. Aubier, A. Boischot, Y. Leblanc, A. Lecacheux, B.M. Pedersen, P. Zarka, Voyager 2 Radio Observations of Uranus, Science, 233, 102, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. JAMES W. WARWICK" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. DAVID R. EVANS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. JOSEPH H. ROMIG" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. CONSTANCE B. SAWYER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. MICHAEL D. DESCH" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "MR. MICHAEL L. KAISER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "MR. JOSEPH K. ALEXANDER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. THOMAS D. CARR" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. DAVID H. STAELIN" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. SAMUEL GULKIS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. ROBERT L. POYNTER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. MONIQUE AUBIER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. ANDRE BOISCHOT" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. YOLANDE LEBLANC" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. ALAIN LECACHEUX" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. BENT M. PEDERSEN" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. PHILLIPE ZARKA" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /****************************** Uranus High Rate Data *************************/ /*MODIFICATIONS */ /* 921027 -- SJOY */ /* Modified from Browse dataset template */ /* 921104 -- EFRIED */ /* last changes made */ /* Template: Spacecraft Data Set Template - Rev: 19890121*/ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-PRA-2-RDR-HIGHRATE-60MS-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA PRA EDITED RDR HIGH RATE 60MS V1.0" DATA_SET_COLLECTION_MEMBER_FLG = N START_TIME = 'UNK' STOP_TIME = 'UNK' NATIVE_START_TIME = "08634:05:001" NATIVE_STOP_TIME = "12397:43:001" DATA_OBJECT_TYPE = "TIME SERIES" DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = 4 PRODUCER_FULL_NAME = "DR. DAVID R. EVANS" PRODUCER_INSTITUTION_NAME = "RADIOPHYSICS, INCORPORATED" SOFTWARE_FLAG = 'N' DETAILED_CATALOG_FLAG = 'N' PROCESSING_START_TIME = 'UNK' PROCESSING_STOP_TIME = 'UNK' DATA_SET_DESC = " Each file within the dataset represents a single PRA high rate frame, of duration 48 seconds. Each file contains a 28 octet header, followed by 1280000 octets of data. The format of these constituents is as follows: Length (bytes) Name Contents 2 Year Year A.D. 2 Day Day of year (1 Jan == 1) 1 Hour Hour of day (midnight == 0) 1 Minute Minute of hour (o'clock = 0) 1 Second Second of Minute (exact minute == 0) 1 Spacecraft 1 == V1, 2 == V2 2 Integral FDS Integer part of FDS count 1 Fractional FDS Fractional part of FDS count 4 Freq. 1 Frequency of 1st channel (Hz) 4 Freq. 2 Frequency of 2nd channel (Hz) 4 Freq. 3 Frequency of 3rd channel (Hz) 4 Freq. 4 Frequency of 4th channel (Hz) 1 Bandwidth Bandwidth (kHz) All values are unsigned, and multi-octet values are presented with the most significant byte first. The data are 16 bit numbers, most significant byte first, with 0 indicating unavailable data. The data are presented as a single stream of 16 bit numbers. The frame is logically divided into lines (although there is no indication of the lines within the file). This terminology comes from the fact that in this high rate mode, the PRA data are treated exactly as if they were imaging data, and a 48 second image comprises 800 horizontal scan lines. Similarly, there are 800 logical lines within a PRA frame. Each line comprises 800 values, representing 400 data pairs. In the high rate mode, the PRA measures the flux at two frequencies _simultaneously_ and returns these two data sequentially. A sample pair is acquired every (actually every 138.88... microseconds), through an RC filter with a 100 microsecond time constant. A single line comprises 60 milliseconds of data. Lines are NOT contiguous in time. There is a 4444.44... microsecond gap between the ending of one line and the start of the succeeding line. The PRA samples a frequency pair in this manner for 24 seconds. It then has the option of switching to a second pair for the final 24 seconds. These frequencies are designated Freq. 1 through Freq. 4 in the header. The data are presented such that the higher of the relevant frequency pair is presented first." CONFIDENCE_LEVEL_NOTE = " Permitted downlink bit error rates are considerably higher for high rate operation than for low rate. Consequently, it is not uncommon for there to be considerable noise in a high rate frame. The probability of any particular datum being incorrect is small, but there are a lot of data in a frame. Generally, a datum should not be assumed to be real if it forms no part of a pattern and is markedly different from its neighbors. Bit error rates are as likely to result in a falsely low reading as a falsely high one. The data presented are calibrated but not otherwise manipulated. An improvement in data quality can often be obtained by making allowance for the 2.4 kHz spacecraft switching power supply, whose signal is clearly superimposed on much of the PRA high rate data. The noise background is considerably higher for these data than for low rate data. This is because of the wide bandwidth usually used (200 kHz instead of the 1 kHz used for low rate), which permits many harmonics of the spacecraft power supply to appear in the data, as well as many of the noise products of other spacecraft subsystems. However, most naturally occurring signals last for (at least) several samples and have an appearance quite unlike the distinctly regular artificial interferences." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = 'URANUS' END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = 'TIME' SAMPLING_PARAMETER_RESOLUTION = 'N/A' MINIMUM_SAMPLING_PARAMETER = 'N/A' MAXIMUM_SAMPLING_PARAMETER = 'N/A' SAMPLING_PARAMETER_INTERVAL = 138.8 MINIMUM_AVAILABLE_SAMPLING_INT = 138.8 SAMPLING_PARAMETER_UNIT = 'MICROSECOND' DATA_SET_PARAMETER_NAME = "RADIO WAVE SPECTRUM" NOISE_LEVEL = 2400 DATA_SET_PARAMETER_UNIT = 'MILLIBEL' END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = 'VG2' INSTRUMENT_ID = 'PRA' END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = "WARWICKETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "VG2 PRA URANUS OVERVIEW" JOURNAL_NAME = "SCIENCE" PUBLICATION_DATE = 1986-07-04 REFERENCE_DESC = " Warwick, J.W., D.R. Evans, J.H. Romig, C.B. Sawyer, M.D. Desch, M.L. Kaiser, J.K. Alexander, T.D. Carr, D.H. Staelin, S. Gulkis, R.L. Poynter, M. Aubier, A. Boischot, Y. Leblanc, A. Lecacheux, B.M. Pedersen, P. Zarka, Voyager 2 Radio Observations of Uranus, Science, 233, 102, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. JAMES W. WARWICK" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. DAVID R. EVANS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. JOSEPH H. ROMIG" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. CONSTANCE B. SAWYER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. MICHAEL D. DESCH" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "MR. MICHAEL L. KAISER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "MR. JOSEPH K. ALEXANDER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. THOMAS D. CARR" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. DAVID H. STAELIN" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. SAMUEL GULKIS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. ROBERT L. POYNTER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. MONIQUE AUBIER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. ANDRE BOISCHOT" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. YOLANDE LEBLANC" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. ALAIN LECACHEUX" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. BENT M. PEDERSEN" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. PHILLIPE ZARKA" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /******************************************************************************/ /* MODIFICATIONS: */ /* 921013 EFRIED */ /* Created template */ /* Template: Data Set Processing Template Rev: 19890121 */ /* Note: This template shall be repeated for each */ /* source dataset id used in production of the */ /* dataset id in the dataset template. */ /* Hierarchy: DSPROCESSING */ OBJECT = DSPROCESSING SOURCE_DATA_SET_ID = "N/A" SOFTWARE_NAME = "UNK" PRODUCT_DATA_SET_ID = "VG2-U-PRA-4-SUMM-BROWSE-48SEC-V1.0" END_OBJECT = DSPROCESSING /******************************************************************************/ /* MODIFICATIONS: */ /* 921013 EFRIED */ /* 921029 SJOY */ /* Created template */ /* Template: Data Set Processing Template Rev: 19890121 */ /* Note: This template shall be repeated for each */ /* source dataset id used in production of the */ /* dataset id in the dataset template. */ /* Hierarchy: DSPROCESSING */ OBJECT = DSPROCESSING SOURCE_DATA_SET_ID = 'N/A' SOFTWARE_NAME = 'UNK' PRODUCT_DATA_SET_ID = 'VG2-U-PRA-2-RDR-HIGHRATE-60MS-V1.0' /* PROCESSING_DESCRIPTION = " /* The header has been produced by extracting relevant /* information from the original JPL data tapes and /* augmenting this with information contained in /* configuration commands uplinked to the spacecraft. /* Where the original tapes present a discrepancy or /* invalid values in the date/time and FDS fields /* the FDS fields have taken precedence and the /* correct time for that FDS count has been placed /* in the header of these files. /* /* The data themselves have been calibrated as best /* we know how and reordered from the original tapes /* so as to present a consistent sequence in this dataset." END_OBJECT = DSPROCESSING /******************************************************************************/ /* MODIFICATIONS: */ /* 921002 EFRIED */ /* Created template */ /* Template: Parameter Template Rev: 19890121 */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID = VG2 DATA_SET_PARAMETER_NAME = "RADIO WAVE SPECTRUM" INSTRUMENT_PARAMETER_NAME = "WAVE FLUX DENSITY" IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /****************** Radio Wave Spectrum Parameter Desc. Template ************/ /* MODIFICATIONS: */ /* 921002 EFRIED */ /* Created template */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM = 'RADIO WAVE SPECTRUM' DATA_SET_OR_INST_PARM_DESC = " A set of derived parameters consisting of power fluxes at various contiguous frequencies over a range of frequencies. The MKS units are: (HERTZ.METER**2)." END_OBJECT = DSINSTPARMD /*************** Wave Flux Density Parameter Desc. Template *****************/ /* MODIFICATIONS: */ /* 921002 EFRIED */ /* Created template */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM = "WAVE FLUX DENSITY" DATA_SET_OR_INST_PARM_DESC = "None provided" END_OBJECT = DSINSTPARMD /******* Uranus Uncalibrated 4 Second Spectrum Analyzer Data *****************/ /* MODIFICATIONS */ /* 920831 -- JPLPDS::RMONARREZ */ /* received by ftp */ /* 920914 -- EFRIED */ /* 920918 -- EFRIED */ /* updated Data Set templates according to new std. */ /* Data Set Template -> Spacecraft Data Set Template */ /* event_start_time, event_stop_time -> start_time, stop_time */ /* 920924 -- EFRIED */ /* Revised DATA_SET_ID and DATA_SET_NAME */ /* last changes made /* Template: Spacecraft Data Set Template Rev: 19890121 */ /* */ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-PWS-2-RDR-SA-4SEC-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA PWS EDITED RDR UNCALIB SPECTRUM ANALYZER 4SEC V1.0" DATA_SET_COLLECTION_MEMBER_FLG = N START_TIME = 1986-01-23T00:00:00.000 STOP_TIME = 1986-01-31T00:00:00.000 NATIVE_START_TIME = "N/A" NATIVE_STOP_TIME = "N/A" DATA_OBJECT_TYPE = "TIME SERIES" DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = "2" PRODUCER_FULL_NAME = "DR. WILLIAM S. KURTH" PRODUCER_INSTITUTION_NAME = "UNIVERSITY OF IOWA" SOFTWARE_FLAG = "Y" DETAILED_CATALOG_FLAG = "Y" PROCESSING_START_TIME = 1988-08-01 PROCESSING_STOP_TIME = "N/A" DATA_SET_DESC = " This data set consists of 4-second edited, wave electric field intensities from the Voyager 2 Plasma Wave Receiver spectrum analyzer obtained in the vicinity of the Uranian magnetosphere. For each 4-second interval, a 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 scan. During data gaps where complete 4-second 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. Data are edited but not calibrated. The data numbers in this data set can be plotted in raw form for event searches and simple trend analysis since they are roughly proportional to the log of the electric field strength. Calibration procedures and tables are provided for use with this data set; the use of these is described below. Use of Voyager PWS Calibration Tables The Voyager PWS calibration tables are given in two plain ASCII text files named VG1PWSCL.TAB and VG2PWSCL.TAB (for Voyagers-1 and -2, respectively). These provide information to convert the uncalibrated `data number' output of the PWS 16-channel spectrum analyzer to calibrated antenna voltages for each frequency channel. Following is a brief description of these files and a tutorial in their application. The first column lists an uncalibrated data number followed by the corresponding value in calibrated volts for each of the 16 frequency channels of the PWS spectrum analyzer. Each line contains calibrations for successive data number values ranging from 0 through 255. (Data number 0 actually represents the lack of data since the baseline noise values for each channel are all above that.) A data analysis program may load the appropriate table into a data structure and thus provide a simple look-up scheme to obtain the appropriate voltage for a given data number and frequency channel. For example, the following VAX FORTRAN code may be used to load a calibration array for Voyager 2 PWS: real*4 cal (16,0:255) open ( unit=10, file='vg2pwscl.tab', status='old' ) do i=0,38 read (10,*) ! skip 38 lines of label info end do do i=0,255 read (10,*) idn, (cal(ichan,i),ichan=1,16) end do close (10) Then, given an uncalibrated data value idn for the frequency channel ichan, the corresponding calibrated antenna voltage would be given by the following array reference: volts = cal (ichan, idn) This may be converted to a wave electric field amplitude by dividing by the effective antenna length in meters, 7.07m. That is: efield = cal(ichan, idn) / 7.07 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. specdens = (cal(ichan,idn)/7.07)**2 / bandwidth(ichan) Finally, power flux may be obtained by dividing the spectral density by the impedance of free space in ohms: pwrflux=((cal(ichan,idn)/7.07)**2/bandwidth(ichan))/376.73 Of course, for a particular application, it may be more efficient to apply the above conversions to the calibration table directly. The center frequencies and bandwidths of each PWS spectrum analyzer channel for the Voyager 2 PWS are given below: VOYAGER 2 PWS SPECTRUM ANALYZER Voyager-2 Channel Center Frequency Bandwidth 1 10.0 Hz 2.16 Hz 2 17.8 Hz 3.58 Hz 3 31.1 Hz 4.50 Hz 4 56.2 Hz 10.7 Hz 5 100. Hz 13.8 Hz 6 178. Hz 28.8 Hz 7 311. Hz 39.8 Hz 8 562. Hz 75.9 Hz 9 1.00 kHz 75.9 Hz 10 1.78 kHz 151. Hz 11 3.11 kHz 324. Hz 12 5.62 kHz 513. Hz 13 10.0 kHz 832. Hz 14 17.8 kHz 1260. Hz 15 31.1 kHz 2400. Hz 16 56.2 kHz 3800. Hz A failure in the Voyager 2 Flight Data System which occurred about 3 months after launch has adversely affected the calibration of PWS channels 9 through 16. An algorithm has been devised to partially correct for this failure, and has proven useful for Voyager 2 Jupiter, Saturn, and Uranus encounters, but is not valid for Earth-Jupiter cruise and may be modified in the future. The following implementation of this correction algorithm in VAX FORTRAN assumes that uncalibrated data numbers are stored in a 16-element integer array, idn, with the array index equal to the PWS channel number: real*4 tonl(9:16) ! the old noise level for v2 data tonl/2.0,1.0,-1.0,-2.0,-3.0,1.0,2.0,1.0/ do ichan=9,16 if (idn(ichan).gt.0) then if(idn(ichan).lt.64) idn(ichan)=64 if (idn(ichan).le.72) then idn(ichan)=int(tonl(ichan)-530.4+8.6 *real(idn(ichan))) else idn(ichan)=int(tonl(ichan)+20.113+0.99 *real(idn(ichan))) end if end if end do This correction should not be applied permanently to the Voyager 2 calibration table since it is valid for a limited time span and may be modified in the future. Additional information about this dataset and the instrument which produced it can be found elsewhere in this catalog. An overview of the data in this data set can be found in Gurnett et al. [1986] and 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 set 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 PLS. The 'bad' points remain in the data set as negative numbers with the same absolute value as the original data point so that the point can be skipped in normal data processing by testing for negative values or recovered for special inspection by converting the sign back to a positive one. Other possible sources of noise which have not been eliminated include random intense spikes of noise below 1 kiloHertz due to the operation of attitude control thrusters. Other randomly occurring spikes or time periods of intense spikes over the entire frequency range are indicative of telemetry errors. No attempt has been made to remove spikes since some could be valid data, i.e. real bursts of wave activity. 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. A failure in the Voyager 2 flight data system a few months after launch has decreased the sensitivity and the calibration accuracy of the upper 8 spectrum analyzer channels (i.e. 1 kiloHertz and higher)." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = URANUS END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = 4.000000 MINIMUM_SAMPLING_PARAMETER = 197708201553.000000 MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 4.000000 MINIMUM_AVAILABLE_SAMPLING_INT = 4.000000 SAMPLING_PARAMETER_UNIT = "SECOND" DATA_SET_PARAMETER_NAME = "PLASMA WAVE SPECTRUM" NOISE_LEVEL = 0.000005 DATA_SET_PARAMETER_UNIT = "VOLT/METER" END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = "VG2" INSTRUMENT_ID = "PWS" END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = "GURNETTETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "VG2 PWS URANUS OVERVIEW" JOURNAL_NAME = SCIENCE PUBLICATION_DATE = 1986-07-04 REFERENCE_DESC = " Gurnett, D.A., W.S. Kurth, F.L. Scarf, R.L. Poynter, The first plasma wave observations at Uranus, Science, 233, 106, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. DONALD A. GURNETT" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. FREDERICK L. SCARF" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. ROBERT L. POYNTER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. WILLIAM S. KURTH" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /******* Uranus 48 Second Spectrum Analyzer Browse Data **********************/ /* MODIFICATIONS */ /* 920831 -- JPLPDS::RMONARREZ */ /* received by ftp */ /* 920914 -- EFRIED */ /* 920918 -- EFRIED */ /* updated Data Set templates according to new std. */ /* Data Set Template -> Spacecraft Data Set Template */ /* event_start_time, event_stop_time -> start_time, stop_time */ /* 920922 -- EFRIED */ /* Revised DATA_SET_ID and DATA_SET_NAME */ /* last changes made */ /* Template: Spacecraft Data Set Template Rev: 19890121 */ /* */ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-PWS-4-SUMM-SA-48SEC-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA PWS RESAMPLED SUMMARY SPECTRUM ANALYZER 48SEC V1.0" DATA_SET_COLLECTION_MEMBER_FLG = N START_TIME = 1986-01-23T00:00:00.000 STOP_TIME = 1986-01-31T00:00:00.000 NATIVE_START_TIME = "N/A" NATIVE_STOP_TIME = "N/A" DATA_OBJECT_TYPE = "TIME SERIES" DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = "4" PRODUCER_FULL_NAME = "DR. WILLIAM S. KURTH" PRODUCER_INSTITUTION_NAME = "UNIVERSITY OF IOWA" SOFTWARE_FLAG = "Y" DETAILED_CATALOG_FLAG = "Y" PROCESSING_START_TIME = 1988-08-01 PROCESSING_STOP_TIME = "N/A" DATA_SET_DESC = " This data set consists of 48-second calibrated, averaged wave electric field intensities from the Voyager 2 Plasma Wave Receiver spectrum analyzer obtained in the vicinity of the Uranian magnetosphere. For each 48-second interval, a geometric average field strength is determined for each of the 16 spectrum analyzer channels whose center frequencies range from 10 Hertz to 56.2 kilo- Hertz and which are logarithmically spaced in frequency, four channels per decade. The time associated with each set of averages is the beginning of the averaging interval. Averages are stored in units of volt/meter. During data gaps where complete 48-second intervals are missing, no entries exist in the file, that is, the gaps are not zero-filled or tagged in any other way. Additional information about this dataset and the instrument which produced it can be found elsewhere in this catalog. An overview of the data in this data set can be found in Gurnett et al. [1986] and 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 set 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 PLS. The averages do not include these noise spikes. Other possible sources of noise which have not been eliminated include random intense spikes of noise below 1 kiloHertz due to the operation of attitude control thrusters. Other randomly occurring spikes or time periods of intense spikes over the entire frequency range are indicative of telemetry errors. No attempt has been made to remove spikes since some could be valid data, i.e. real bursts of wave activity. 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. A failure in the Voyager 2 flight data system a few months after launch has decreased the sensitivity and the calibration accuracy of the upper 8 spectrum analyzer channels (i.e. 1 kiloHertz and higher)." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = URANUS END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = 48.000000 MINIMUM_SAMPLING_PARAMETER = 197708201553.000000 MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 48.000000 MINIMUM_AVAILABLE_SAMPLING_INT = 4.000000 SAMPLING_PARAMETER_UNIT = SECOND DATA_SET_PARAMETER_NAME = "PLASMA WAVE SPECTRUM" NOISE_LEVEL = 0.000005 DATA_SET_PARAMETER_UNIT = "VOLT/METER" END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = "VG2" INSTRUMENT_ID = "PWS" END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = "GURNETTETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "VG2 PWS URANUS OVERVIEW" JOURNAL_NAME = "SCIENCE" PUBLICATION_DATE = 1986-07-04 REFERENCE_DESC = " Gurnett, D.A., W.S. Kurth. F.L. Scarf, and R.L. Poynter, The first plasma wave observations at Uranus, Science, 233, 106, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. DONALD A. GURNETT" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. FREDERICK L. SCARF" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. ROBERT L. POYNTER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. WILLIAM S. KURTH" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /**************** PWS Uranus High Rate Waveform Data **************************/ /* MODIFICATIONS */ /* 920831 -- JPLPDS::RMONARREZ */ /* received by ftp */ /* 920914 -- EFRIED */ /* 920918 -- EFRIED */ /* updated Data Set templates according to new std. */ /* Data Set Template -> Spacecraft Data Set Template */ /* event_start_time, event_stop_time -> start_time, stop_time */ /* 920922 -- EFRIED */ /* Revised DATA_SET_ID and DATA_SET_NAME */ /* 920925 -- RMONARREZ */ /* Updated PROCESSING_LEVEL_ID to match DATA_SET_ID */ /* last changes made */ /* Template: Spacecraft Data Set Template Rev: 19890121 */ /* */ /* Note: The following templates form part of a standard set */ /* for the submission of a single dataset to the PDS. */ /* */ /* Hierarchy: SCDATASET */ /* DATASETINFO */ /* DATASETTARG */ /* DSPARMINFO */ /* SCDSHOST */ /* DSREFINFO */ /* REFERENCE */ /* REFAUTHORS */ OBJECT = SCDATASET DATA_SET_ID = "VG2-U-PWS-1-EDR-WFRM-60MS-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "VG2 URA PWS RAW EXPERIMENT WAVEFORM 60MS V1.0" DATA_SET_COLLECTION_MEMBER_FLG = N START_TIME = 1985-11-08T07:04:08.649 STOP_TIME = 1986-02-22T20:41:34.186 NATIVE_START_TIME = "24524.12" NATIVE_STOP_TIME = "27721.14" DATA_OBJECT_TYPE = "TIME SERIES" DATA_SET_RELEASE_DATE = 1993-02-01 PROCESSING_LEVEL_ID = 1 PRODUCER_FULL_NAME = "DR. WILLIAM S. KURTH" PRODUCER_INSTITUTION_NAME = "UNIVERSITY OF IOWA" SOFTWARE_FLAG = N DETAILED_CATALOG_FLAG = N PROCESSING_START_TIME = "N/A" PROCESSING_STOP_TIME = 1992-04-06 DATA_SET_DESC = "This data set consists of electric field waveform samples from the Voyager 2 Plasma Wave Receiver waveform receiver obtained during the Uranus encounter. The waveforms are collections of 4-bit samples of the electric field measured by the dipole electric antenna at a rate of 28,800 samples per second. 1600 samples are collected in 55.56 msec followed by a 4.44-msec gap. Each 60-msec interval constitutes a line of waveform samples. The data set includes about 271 frames of waveform samples consisting of up to 800 lines, each. The telemetry format for the waveform data is identical to that for images, hence the use of line and frame as constructs in describing the form of the data. The waveform is sampled through a bandpass filter with a passband of 40 Hz to 12 kHz. The 4-bit samples provide sixteen digital values of the electric field with a linear amplitude scale, but the amplitude scale is arbitrary because of the automatic gain control used in the waveform receiver. The instantaneous dynamic range afforded by the 4 bit samples is about 23 db, but the automatic gain control allows the dominant signal in the passband to be set at the optimum level to fit within the instantaneous dynamic range. With the gain control, the overall dynamic range of the waveform receiver is about 100 db. The automatic gain control gain setting is not returned to the ground, hence, there is no absolute calibration for the data. However, by comparing the waveform spectrum derived by Fourier transforming the waveform to the spectrum provided by the spectrum analyzer data, an absolute calibration may be obtained in most cases. The data may be plotted in raw form to show the actual waveform; this is useful for studying events such as dust impacts on the spacecraft. But the normal method of analyzing the waveform data is by Fourier transforming the samples from each line to arrive at an amplitude versus frequency spectrum. By stacking the spectra side-by-side in time order, a frequency- time spectrogram can be produced. Additional information about this dataset and the instrument which produced it can be found elsewhere in this catalog. An overview of the data in this data set can be found in Gurnett et al. [1986] and a complete instrument description can be found in Scarf and Gurnett [1977]." CONFIDENCE_LEVEL_NOTE = " This data set includes all available waveform receiver data obtained during the Uranus encounter. There has been no attempt to clean various interference signals from the data. Most of these can normally be easily seen in frequency-time spectrograms as narrowband, fixed-frequency tones. The most common include narrow- band tones at 2.4 and 4.8 kHz which are power supply harmonics. There is sometimes a tone near 1.7 kHz which is associated with the operation of the spacecraft gyros. The spacecraft tape recorder results in a rather intense band in the frequency range of a few hundred Hz. There are few times when the data in this frequency range can be used. However, there are times when the real signals in this frequency range can exceed the intensity of the interference sufficiently so that the frequency range near a few hundred Hz can be used. Use of the spectrum analyzer data can be of use to determine when these time periods occur. The stepper motor of the LECP instrument also interferes in the frequency range of a few hundred Hz, but for periods of a few seconds. The LECP interference is very intense and captures the automatic gain control so that real signals, even where there is no interference, will appear to decrease in amplitude until the LECP interference fades in amplitude. The PLS instrument periodically interferes at 400 Hz and odd harmonics because of a 400-Hz square wave used to modulate a grid in the detector. The PLS interference lasts for several seconds and ends abruptly. Telemetry errors result in a fairly graceful degradation of the waveform data. Assuming the telemetry errors are randomly occurring bursts, they typically appear as an enhanced background level in the spectrum. Since the bursts are short, their Fourier transform is a broadband spectrum. When looking for relatively narrowband features or features with distinct frequency-time characteristics, the result of the bursts simply reduce the signal-to-noise in the spectrum. One way of reducing the effect of burst telemetry errors is to pass the waveform data through a low-pass filter to despike it, prior to running the Fourier transform. The waveform data is not subject to the negative effects of the failure in the Voyager 2 Flight Data System which reduces the sensitivity of the spectrum analyzer and affects the calibration above 1 kHz. In fact, use of the 1 - 12 kHz waveform data is an effective way of avoiding the problems with the spectrum analyzer data in this frequency range." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = URANUS END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = 0.000034722 MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = 0.000034722 MINIMUM_AVAILABLE_SAMPLING_INT = 0.000034722 SAMPLING_PARAMETER_UNIT = SECOND DATA_SET_PARAMETER_NAME = "PLASMA WAVE WAVEFORM" NOISE_LEVEL = 0.000005 DATA_SET_PARAMETER_UNIT = "VOLT/METER" /* Data not absolutely */ /* calibrated */ END_OBJECT = DSPARMINFO OBJECT = SCDSHOST INSTRUMENT_HOST_ID = VG2 INSTRUMENT_ID = PWS END_OBJECT = SCDSHOST OBJECT = DSREFINFO REFERENCE_KEY_ID = GURNETTETAL1986 OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "VG2 PWS URANUS OVERVIEW" JOURNAL_NAME = SCIENCE PUBLICATION_DATE = 1986-07-04 REFERENCE_DESC = " Gurnett, D. A., W. S. Kurth, F. L. Scarf, R. L. Poynter, 'First plasma wave observations at Uranus,' Science, 233, 106, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. DONALD A. GURNETT" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. WILLIAM S. KURTH" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. FREDERICK L. SCARF" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "DR. ROBERT L. POYNTER" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = SCDATASET /**************** Plasma Wave Spectrum Parameter ******************************/ /* MODIFICATIONS: */ /* 920806 JPLPDS::RMONARREZ */ /* received by mail */ /* 92-08 EFRIED */ /* 920916 EFRIED */ /* last changes made */ /* Template: Parameter Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID ='VG2' DATA_SET_PARAMETER_NAME ='PLASMA WAVE SPECTRUM' INSTRUMENT_PARAMETER_NAME ='WAVE MAGNETIC FIELD INTENSITY' IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /************************** Parameter Description *****************************/ /* MODIFICATIONS: */ /* 920806 JPLPDS::RMONARREZ */ /* received by mail */ /* 92-08 EFRIED */ /* 920916 EFRIED */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM= 'PLASMA WAVE SPECTRUM' DATA_SET_OR_INST_PARM_DESC = " A set of derived parameters consisting of wave electric field intensities or electric field spectral densities at various contiguous frequencies over a range of frequencies. The MKS units are: Volts/Meter or Volts**2/(Hertz.Meter**2), respectively." END_OBJECT = DSINSTPARMD /************** Wave Magnetic Field Intensity Parameter Description ***********/ /* MODIFICATIONS: */ /* 921002 EFRIED */ /* created template */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM= "WAVE MAGNETIC FIELD INTENSITY" DATA_SET_OR_INST_PARM_DESC = " A measured parameter equaling the magnetic field strength in a specific frequency passband (in MKS unit: VOLTS/METER) measured in a single sensor or antenna." END_OBJECT = DSINSTPARMD /**************** Plasma Wave Waveform Parameter ******************************/ /* MODIFICATIONS: */ /* 921002 EFRIED */ /* created template */ /* last changes made */ /* Template: Parameter Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID ='VG2' DATA_SET_PARAMETER_NAME ="PLASMA WAVE WAVEFORM" INSTRUMENT_PARAMETER_NAME ='WAVE MAGNETIC FIELD INTENSITY' IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /************ Wave Electrical Field Intensity Parameter Description ***********/ /* MODIFICATIONS: */ /* 921002 EFRIED */ /* created template */ /* NEED DESCRIPTION */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM= "PLASMA WAVE WAVEFORM" DATA_SET_OR_INST_PARM_DESC = " A plasma wave waveform is a time series of measurements of the electric or magnetic field component of the wave spectrum taken through a broadband filter. The temporal sample rate is normally such that samples are made at more than twice the analysis filter bandwidth. A typical waveform will consist of the order of 1000 contiguous samples of between 4 and 12 bits each. For a 10-kHz analysis bandwidth, the sample rate would normally be approximately 25 kHz or 25,000 samples/second. Once received, the waveforms are typically Fourier transformed in order to provide an amplitude versus frequency spectrum across the analysis bandwidth. The sample rate, then, is required to be at least a factor of two greater than the filter bandwidth in order to avoid aliasing in the transformed spectrum. The spectra can be stacked side-by-side in time to build a frequency-time spectrogram (that is, amplitude as a function of time and frequency) in order to identify the temporal and spectral variations in the wave spectrum. Alternately, the untransformed time series can be used to study the details of the waveform. This has been useful for measuring small-scale structures in the plasma and for identifying the signature of micron-sized dust impact on the spacecraft." END_OBJECT = DSINSTPARMD /**************** Plasma Wave Waveform Parameter ******************************/ /* MODIFICATIONS: */ /* 921002 EFRIED */ /* created template */ /* last changes made */ /* Template: Parameter Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID ='VG2' DATA_SET_PARAMETER_NAME ="PLASMA WAVE WAVEFORM" INSTRUMENT_PARAMETER_NAME ='WAVE ELECTRIC FIELD INTENSITY' IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /************ Wave Electrical Field Intensity Parameter Description ***********/ /* MODIFICATIONS: */ /* 921002 EFRIED */ /* created template */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM= "WAVE ELECTRIC FIELD INTENSITY" DATA_SET_OR_INST_PARM_DESC = " A measured parameter equaling the electric field strength in a specific frequency passband (in MKS unit: VOLTS/METER) measured in a single sensor or antenna." END_OBJECT = DSINSTPARMD /**************** Plasma Wave Spectrum Parameter ******************************/ /* MODIFICATIONS: */ /* 921009 EFRIED */ /* created template */ /* last changes made */ /* Template: Parameter Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID ='VG2' DATA_SET_PARAMETER_NAME ='PLASMA WAVE SPECTRUM' INSTRUMENT_PARAMETER_NAME ='WAVE ELECTRIC FIELD INTENSITY' IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /**************** Plasma Wave Waveform Parameter ******************************/ /* MODIFICATIONS: */ /* 921009 EFRIED */ /* created template */ /* last changes made */ /* Template: Parameter Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID ='VG2' DATA_SET_PARAMETER_NAME ="PLASMA WAVE WAVEFORM" INSTRUMENT_PARAMETER_NAME ='ELECTRIC FIELD COMPONENT' IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /************ Electrical Field Component Parameter Description ****************/ /* MODIFICATIONS: */ /* 921009 EFRIED */ /* created template */ /* NEED DESCRIPTION */ /* last changes made */ /* Template: Data Set Instrument Parameter Description Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for any */ /* data set or instrument parameter description. */ /* */ /* Hierarchy: DSINSTPARMD */ OBJECT = DSINSTPARMD DATA_SET_OR_INSTRUMENT_PARM_NM= "ELECTRIC FIELD COMPONENT" DATA_SET_OR_INST_PARM_DESC = " A measured parameter equaling the electric field strength (e.g. in milli-Volts per meter) along a particular axis direction." END_OBJECT = DSINSTPARMD /**************** Plasma Wave Spectrum Parameter ******************************/ /* MODIFICATIONS: */ /* 921009 EFRIED */ /* created template */ /* last changes made */ /* Template: Parameter Template Rev: 19890121 */ /* */ /* Note: This template shall be completed for each combination */ /* of data set parameter name, instrument parameter */ /* name and instrument host id associated with a dataset. */ /* */ /* Hierarchy: PARAMETER */ OBJECT = PARAMETER INSTRUMENT_HOST_ID ='VG2' DATA_SET_PARAMETER_NAME ='PLASMA WAVE SPECTRUM' INSTRUMENT_PARAMETER_NAME ='ELECTRIC FIELD COMPONENT' IMPORTANT_INSTRUMENT_PARMS = 1 END_OBJECT = PARAMETER /********************* CDMAKE Software *************************************/ /* MODIFICATIONS: */ /* 920806 JPLPDS::RMONARREZ */ /* received by mail */ /* 92-08 EFRIED */ /* 920916 EFRIED */ /* last changes made */ /* Template: Software Information Template Rev: 19890121 */ /* */ /* Note: This template is completed for each node */ /* software application referenced in the PDS. */ /* */ /* Hierarchy: SOFTWARE */ OBJECT = SOFTWARE SOFTWARE_NAME = CDMAKE NODE_ID = "PPI-IOWA" SOFTWARE_RELEASE_DATE = 1988-08-01 SOFTWARE_TYPE = "N/A" COGNIZANT_FULL_NAME = "MR. LARRY J. GRANROTH" SOFTWARE_ACCESSIBILITY_DESC = "N/A" SOFTWARE_DESC = " CDMAKE is primarily a data format translation routine which is used to convert Voyager Plasma Wave Spectrometer (PWS) MSF tape files to CD files. The MSF, or Master Science Files, are produced at the University of Iowa as the primary, ordered, full-information PWS spectrum analyzer data set. The CD files contain uncalibrated, full-resolution PWS data with minimal ancillary data in a simplified format which may be used in CDROM production. NOTE: SOFTWARE IS NOT AVAILABLE FOR PUBLIC USE." END_OBJECT = SOFTWARE /************************** V2U48 Software ********************************/ /* MODIFICATIONS: */ /* 920806 JPLPDS::RMONARREZ */ /* received by mail */ /* 92-08 EFRIED */ /* 920916 EFRIED */ /* last changes made */ /* Template: Software Information Template Rev: 19890121 */ /* */ /* Note: This template is completed for each node */ /* software application referenced in the PDS. */ /* */ /* Hierarchy: SOFTWARE */ OBJECT = SOFTWARE SOFTWARE_NAME = V2U48 NODE_ID = "PPI-IOWA" SOFTWARE_RELEASE_DATE = 1988-08-01 SOFTWARE_TYPE = "N/A" COGNIZANT_FULL_NAME = "MR. LARRY J. GRANROTH" SOFTWARE_ACCESSIBILITY_DESC = "N/A" SOFTWARE_DESC = " V2U48 is a specialized, hard-coded routine to process a specific interval of Voyager 2 Plasma Wave Spectrometer (PWS) spectrum analyzer data around Uranus encounter. Input is from MSF or CD data sets produced and stored at the University of Iowa, and output is to ASCII text files which are compatible with PDS data loading procedures. These files contain information corresponding to the VG2-N-PWS-4-SUMM-SA-48SEC-V1.0 and VG2-U-PWS-4-SUMM-SA-48SEC data set. NOTE: SOFTWARE IS NOT AVAILABLE FOR PUBLIC USE." END_OBJECT = SOFTWARE /************************** CDREF Software *********************************/ /* MODIFICATIONS: */ /* 920806 JPLPDS::RMONARREZ */ /* received by mail */ /* 92-08 EFRIED */ /* 920916 EFRIED */ /* last changes made */ /* Template: Software Information Template Rev: 19890121 */ /* */ /* Note: This template is completed for each node */ /* software application referenced in the PDS. */ /* */ /* Hierarchy: SOFTWARE */ OBJECT = SOFTWARE SOFTWARE_NAME = CDREF NODE_ID = "IMAGING" SOFTWARE_RELEASE_DATE = 1990-04-07 SOFTWARE_TYPE = "N/A" COGNIZANT_FULL_NAME = "MR. JASON J. HYON" SOFTWARE_ACCESSIBILITY_DESC = "N/A" SOFTWARE_DESC = " CDREF is primarily a data format translation routine which is used to convert Voyager PWS EDR tape files to CD-ROM files. CDREF is written in FORTRAN and is not available for public use. The EDR, or Engineering Data Records, are produced at Multi-mission Image Processing Laboratory at JPL as the uncalibrated, full-resolution PWS spectrum analyzer data set. The CD files contain uncalibrated, full-resolution PWS data with minimal ancillary data in a simplified format which may be used in CDROM production." END_OBJECT = SOFTWARE