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Wind Plasma and Radio Waves (WAVES) Time Domain Sampler (TDS) Dust Impact, Level 3, 1 s Data

Wind WAVES Time Domain Sampler, TDS, Dust Data File References: 1) Bougeret, J.-L., et al., WAVES: The Radio and Plasma Wave Investigation on the Wind Spacecraft, Space Sci. Rev., 71, 231-263, 1995, doi:10.1007/BF00751331. 2) Malaspina, D.M., M. Horanyi, A. Zaslavsky, K. Goetz, L.B. Wilson III, and K. Kersten, Interplanetary and Interstellar Dust observed by the Wind/WAVES Electric Field Instrument, Geophys. Res. Lett., 41, 266-272, 2014, doi:10.1002/2013GL058786. 3) Malaspina, D.M., and L.B. Wilson III, A Database of Interplanetary and Interstellar Dust Detected by the Wind Spacecraft, J. Geophys. Res., 121, 9369-9377, 2016, doi:10.1002/2016JA023209.

VEGA1 DUST PARTICLE IMPACT PLASMA DETECTOR DATA V1.0

The SP-1 experiment on Vega spacecraft was intended for studying the spatial and mass distributions of dust particles in the cometary coma over the mass range 1.e-16 to 1.e-6 g. Covering such a broad mass range was made possible by using sensors of two types, namely, impact plasma and acoustic.

GALILEO DUST DETECTION SYSTEM V2.0

This data set contains information on the dust environment in interplanetary space within the inner solar system and in the Jupiter system, within and without the Jovian magnetosphere and around the Galilean satellites.

ULYSSES DUST DETECTION SYSTEM V3.0

This data set contains the data from the Ulysses dust detector system (UDDS) from start of mission through the end of mission, 1990-2007. (As the dust detector was turned off after Nov. 30, 2007, this is the last date for which UDDS data is recorded.) Included are the dust impact data, noise data, laboratory calibration data, and location and orientation of the spacecraft and instrument.

ULYSSES DUST DETECTOR SYSTEM V1.0

Version 1.1 =========== This data set, ULY-D-UDDS-5-DUST-V1.1, differs slightly from the data set UL-D-UDDS-5-DUST-V1.0 created and reviewed at the PDS/Small Bodies Dust Subnode. In addition to the change in Data set ID, the following changes have been made:

VEGA2 DUST PARTICLE IMPACT PLASMA DETECTOR DATA V1.0

A number of datasets from the VEGA missions were submitted by Dyachkov at IKI as FITS files (binary data) using the GROUPS form or multidimensioned arrays. In addition, little information was provided except for the date, spacecraft, and experiment. Sometimes in the GROUPS parameters (Pvalues), there were experiment parameters such as 'time' indicated and by inference this could be determined to be exposure time versus a clock time. Since there was at least one extensive set of observations (TVS images), that were provided by IKI in this manner and a separate facility (KFKI) with the proper IHW keywords, it was possible to make estimates as to the meaning of 'time' with proper units (seconds).

VEGA1 PUMA DUST MASS SPECTROMETER DATA V1.0

The PUMA data were submitted by IKI in two unique forms, a GROUPS FITS file and undocumented binary file. In one original form, the data in this set were received as 4,027 separate FITS files, one for each spectrum. These files have been reformatted and combined into four tables, one for each of the PUMA instrument operating modes. Within each table, the spectra are in order of original FITS file number. This order is assumed to be chronological, based on time given by the BLISI clock, in sec.

MSX ZODIACAL DUST DATA V1.0

The Midcourse Space Experiment (MSX) mid-infrared emission measurements from the zodiacal dust cloud in spectral bands centered at 8.3 12, 15, and 21 microns.

GALILEO DUST DETECTION SYSTEM V4.1

This data set contains the data from the Galileo dust detector system (GDDS) from start of mission through the end of mission. Included are the dust impact data, noise data, laboratory calibration data, and location and orientation of the spacecraft and instrument.

VEGA2 DUST PARTICLE IMPACT DETECTOR DATA V1.0

The SP-2 experiment on Vega spacecraft was intended for studying the spatial and mass distributions of dust particles in the cometary coma over the mass range 1.e-16 to 1.e-6 g. Covering such a broad mass range was made possible by using sensors of two types, namely, impact plasma and acoustic.

GALILEO DUST DETECTION SYSTEM V3.0

Detector responses and derived quantities from the Galileo dust detector as well as spacecraft geometry information for reliable impacts from launch through 2001. See Gruen et al. (Plan. Sp. Sci. 43, 953-969, 1995) and Krueger et al. (Plan. Sp. Sci. 47, 85-106, 1999; Plan. Sp. Sci. 49, 1285-1301, 2001) for more information.

LADEE LUNAR DUST EXPERIMENT

This archive bundle includes data taken by the Lunar Dust Experiment (LDEX) instrument aboard the Lunar Atmosphere and Dust Environment Explorer (LADEE) spacecraft. These data are generated by dust impacts on the LDEX detector. Both reduced and calibrated data are included in this bundle.

CASSINI COSMIC DUST ANALYZER CALIBRATED/RESAMPLED DATA

The Cosmic Dust Analyzer (CDA) is an instrument on the Cassini Orbiter that studies the physical properties of dust particles hitting the detector. This data set includes all data from the CDA with the exception of the High Rate Detector (HRD). Please refer to [SRAMAETAL2004B] (see CDAREFS.CAT) for a detailed CDA description.

GIOTTO DUST IMPACT DETECTOR SYSTEM DATA V1.0

Dust Impact Detection System (DIDSY) consists of six independent subsystems with the primary aim of registering the impacts of all particulates of significant mass incident on the probe during the post-perihelion encounter with Comet Halley in 1986. Mounted on Giotto's front dust shield, the detectors will determine the mass spectrum of the dust, with a limiting sensitivity of some 10^^-17^^ g, increasing to the largest grain masses encountered along Giotto's trajectory through the cometary environment with an ultimate spatial resolution of some 70 km. An additional detector is located on the rear shield to monitor those dust particles (m > ~ 5 X 10^^-7^^ g) that are able to penetrate the front dust shield. An ambient plasma monitor is also incorporated into DIDSY to measure the inJpact plasma generated by both dust and gas impacts on the spacecraft. The system is controlled and its data processed by a microprocessor-based system that allows the wide range of anticipated impact rates (varying from a few per minute, to ~ 10^6 s^^-1^^ at closest approach) to be handled. The instrument weighs 2.26 kg and consumes 1.9 W of power during normal operation.

VEGA1 DUST PARTICLE IMPACT DETECTOR DATA V1.0

Lunar Atmosphere and Dust Environment Explorer (LADEE) Ultraviolet-Visible Spectrometer (UVS) Archive Bundle

GIOTTO PARTICLE IMPACT ANALYZER DUST MASS SPECTRA V1.0

The PIA data was acquired in four modes of data compression, termed mode 0 (the least compressed), and modes 1, 2, and 3, each with increasing degrees of compression. With each spectrum are a PIA assigned sequence number and event numbers, a unique ID-number, instrument settings, and the relative approach time. The PIA time is a 16-bit counter that starts with zero after switch-on. As the Spacecraft Time Signal (STS) is used to reset the internal PIA time counter, the TIM highest possible value is 48960 counts. STS-pulses are given after the transimssion of 256 formats. This results for format F1/F2 and high bitrate (46080 bps) in 5802.67 s. (= 256 formats * 64 frames * 2040 bytes * 8 bit/byte/46080 bps) The time resolution is DTIM = 1/ (138240 HZ /2**14 ) = 0.1185 s. Each STS defines the time for an event with TIM = 0. Therefore, SCET = GRT(STS) + (TIM * DTIM) - propogation delay (8:00.1 sec). where SCET = Spacecraft Event Time, GRT = Ground Reception Time.