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ODY MARS GAMMA RAY SPECTROMETER 5 AHD V1.0

The Odyssey Gamma Ray Spectrometer (GRS) Averaged HEND Data (AHD) products are temporally and spatially binned neutron counting rates and fluxes that can be used to create global maps. These products are generated from the Derived HEND Data (DHD) product, which in turn are derived from HEND EDRs.

MESSENGER E/V/H GRNS 5 GAMMA RAY SPECTROMETER DAP V1.0

Abstract ======== The GRS experiment is a gamma-ray spectrometer designed to observe spectra of gamma rays emitted from Mercury's surface in the energy range from 0.1 to 10 MeV. This data set consists of the MESSENGER GRS advanced data products (DAPs), which are jpeg2000 maps of gamma-ray count rates or elemental abundances derived from summed GRS data, each with a corresponding one standard deviation error map.

ODY MARS GAMMA RAY SPECTROMETER 2 EDR V1.0

The Odyssey Gamma Ray Spectrometer (GRS) Experiment Data Records (EDRs) are raw, uncalibrated spectra and ancillary data acquired by the Gamma Ray Subsystem -- the Gamma Sensor Head (GSH), the Neutron Spectrometer (NS), and the High Energy Neutron Detector (HEND).

ULY JUP GRB SOLAR X-RAY/COSMIC GAMMA-RAY RAW COUNT RATE

The archived data consist of count rates from the sum of two hemispherical detectors covering 4 pi steradians and operating continuously. The detectors are 3 mm thick CsI scintillators coupled to photomultiplier tubes. The nominal energy range is 25-150 keV, but the below table should be consulted to find the accurate thresholds for any day of the mission. A more complete description of the instrument may be found in [HURLEYETAL1992] and [COTINETAL1983]. Although the prime objectives of this investigation are the study of solar and cosmic x- and gamma-ray bursts, it should be noted that the experiment is also sensitive to solar protons and electrons. The former deposit energy directly in the scintillator if they are energetic enough, while the latter may produce x- radiation locally by bremsstrahlung. Thus although the counting rates are generally stable at about 500 c/s over the long term, there are periods of weeks to a month or so when the rates increase considerably due to particles. Examples may be found in March 1991 (solar protons) and February 1992 (particles in the Jovian magnetosphere). The time resolution of the data takes on one of four values depending on the telemetry rate and instrument operating mode: 0.25, 0.5, 1, or 2 seconds.

ODY MARS GAMMA RAY SPECTROMETER 5 ELEMENT CONCENTRATION V1.0

The ODY MARS GAMMA RAY SPECTROMETER 5 ELEMENTS data set consists of a set of maps and underlying data products originally released to the public in March 2006. They contain data that was collected by the 2001 Mars Odyssey Gamma-ray Spectrometer between June 4, 2002 and April 3, 2005. These data are highly processed, and represent the fully corrected, CO2 frost free elemental concentrations. Data for all non-radioactive species have been masked to exclude polar regions where we currently cannot adequately deal with dilution by the large amounts of water ice.

ODY MARS GAMMA RAY SPECTROMETER 4 CGS V1.0

The Mars Odyssey Gamma-Ray Spectrometer (GRS) is a suite of three instruments working together to collect data that will permit the mapping of elemental concentrations on the surface of Mars. The suite of three instruments, the gamma sensor head (GS), the neutron spectrometer (NS) and the high-energy neutron detector (HEND), are a complimentary set of instruments in that the neutron instruments have better counting statistics and sample to a greater depth than the GS, but the GS determines the abundance of many more elements. A full description of the Mars Odyssey Gamma-Ray Spectrometer instrument can be found in [BOYNTONETAL2002].

ODY MARS GAMMA RAY SPECTROMETER 4 DHD V1.0

Prism counting rates, normalizations, corrections, and thermal, epithermal, and fast neutron counting rates derived from neutron data collected by the Neutron Spectrometer of the Odyssey GRS instrument suite.

Gamma-Ray Astrophysics NSSTC Fermi GBM

The Fermi Gamma-Ray Burst Monitor (GBM) is not a pointed or imaging instrument. To determine fluxes for known sources, we measure the change in the count rate observed in the NaI (or BGO) detectors when the source enters or exits Earth occultation. The measured counts in each energy channel are converted to fluxes using an assumed spectrum for each source. For these measurements we currently use CTIME data, with 0.256-s resolution and 8 energy channels covering 8 keV to 1 MeV. Our technique uses all 8 energy channels, but for most sources the majority of the signal is in the 12-25 keV and 25-50 keV bands. The fluxes listed in the table are for the 12-25 keV band and are the mission long average, the 5-day average flux for the most recent 5 days, and the 2-day average flux for the most recent 2 days. The fluxes are normalized to units of mCrab based on the Crab flux over the period from MJD 54690 to 54790, during which the Crab flux is relatively constant as measured by GBM.

MESSENGER E/V/H GRNS 3 GAMMA RAY SPECTROMETER CALIBDATA V1.0

Abstract ======== This data set consists of the MESSENGER GRS calibrated observations (CDRs) and the reduced data product (RDR). The GRS experiment is a gamma ray spectrometer designed to observe spectra of gamma rays emitted from Mercury's surface in the energy range from 0.1 to 10 MeV. There are seven basic GRS CDR data products: the Ge raw spectra data (GRS_CAL_RAW), the anti-coincidence spectra data (GRS_CAL_AC), the shield spectra data (GRS_CAL_SH, GRS_CAL_SH2, GRS_CAL_SH3), the shield count rate (GRS_CAL_SCR) and the engineering data (GRS_ENG). There is one GRS RDR product (GRS_RDR_SUM), a spectral sum of the GRS_CAL_RAW and GRS_CAL_AC spectra.

MESSENGER E/V/H GRNS 2 GAMMA RAY SPECTROMETER RAW DATA V1.0

Abstract ======== This data set consists of the MESSENGER GRS uncalibrated observations, also known as EDRs. The GRS experiment is a gamma ray spectrometer designed to observe spectrum of gamma rays emitted from Mercury's surface in the energy range from 0.1 to 10 MeV. There are ten GRS EDR data products: the raw spectra data, the spectra data from the shield (2 versions), shield count rate data, the anti-coincident spectra data, the microphonics data, the software rate counter data, the status parameters, the state of the instrument, and a GRS instrument command list.

ODY MARS GAMMA RAY SPECTROMETER 4 DND V1.0

The Odyssey GRS Derived Neutron Data (DND) data set includes prism counting rates, normalizations, corrections, and thermal, epithermal, and fast neutron counting rates derived from neutron data collected by the Neutron Spectrometer of the Odyssey GRS instrument suite.

ODY MARS GAMMA RAY SPECTROMETER 5 AND V1.0

The ODY MARS GAMMA RAY SPECTROMETER 5 AND data set is a table of neutron data from the NS sub-system of the Mars Odyssey Gamma-Ray Spectrometer that have been averaged (AND) over 5-degree latitude by 5-degree longitude spatial grids and 15-degrees of aerocentric solar longitude (Ls). The AND are an intermediate data product. These data are calculated from the derived neutron data (DND) and result in maps of thermal,epithermal, and fast neutron counting rates.

LP MOON GAMMA RAY SPECTROMETER 3 RDR V1.0

This data set contains processed LP-GRS time-series data that are used as the fundamental data for deriving composition measurements of the lunar surface using either energy window techniques or the full modeling of the neutron and gamma ray transport processes. These data have been processed to eliminate bad data as well as to make corrections due to time variations in the cosmic ray flux, LP-GRS gain, LP-GRS orientation, and altitude above the lunar surface.

ODY MARS GAMMA RAY SPECTROMETER 5 SGS V1.0

The ODY MARS GAMMA RAY SPECTROMETER 5 SGS (SGS) data set is a collection of data tables that contain a gamma spectrum and the associated engineering data that has been summed over 5-degree by 5-degree latitude longitude cells on the surface of Mars and over a time period of 15 degrees of solar longitude (Ls). The SGS are produced because the individual gamma spectra collected during an approximately 19.7 second collection interval do not contain enough counts to be statistically significant. The SGS are summed over large enough and long enough spatial and temporal intervals to provide a statistically meaningful spectrum that can be used for scientific data analysis.