NOTICE:

This Legacy journal article was published in Volume 7, June 1998, and has not been updated since publication. Please use the search facility above to find regularly-updated information about this topic elsewhere on the HEASARC site.
The Reconfigured HEASARC CGRO Data Archive

C. Meetre, S. Digel (COSSC/Raytheon),
J. Bonnell, T. Bridgman, K. Watanabe, C. Shrader (COSSC/USRA)
F. Pelaez (HEASARC/USRA)


  1. Overview

    The Compton Gamma-Ray Observatory (CGRO), one of NASA’s Great Observatories, was launched from the Space-Shuttle Atlantis in April of 1991. The CGRO Science Support Center (COSSC), in collaboration with the HEASARC, has been providing support and archival services since then. During the past year, and continuing for the next several months, a gradual reconfiguration of our archive and the systems that make it available has been evolving. We have accomplished the following:

    • revamped our Web presence to be simpler and more compelling
    • added new products, and reorganized the directory structure of our products
    • enabled W3Browse of some products with the remainder coming on line during 1998
    • improved our documentation and the number of analysis tools - particularly FTOOLS
    • transferred data to two new jukeboxes with a more robust directory architecture
    • created a permanent disk-based cache of BATSE trigger data with backup in the jukebox to speed access and increase redundancy
    • retired several obsolete systems in order to streamline operations

    Several new FTOOLS have been developed (see below) and several others are under way and may be available by the publication of this article. Some of these FTOOLS transform CGRO data for use by standard packages like XSPEC. New non-FTOOL utilities available include a Web-based mission timeline and OSSE field-of-view tools. URLs referred to in the text are collated in Appendix A.

    This article briefly discusses the scientific objectives of the mission and the four CGRO experiments that comprise it. This is followed by a description, experiment by experiment, of available products and the tools for their use. Finally, appendices give useful ancillary information such as the names and affiliations of Principal Investigators, a selection of Web/FTP sites, e-mail addresses, and a short bibliography.

  2. Mission Science CGRO was designed to study gamma-ray emissions from the following sources:

    • pulsars and accreting compact objects, e.g. white dwarfs, neutron stars and black holes
    • the decay of radioactive nuclei that are byproducts of novae, supernovae, and nuclear reactions in the core of massive stars
    • the Galactic diffuse emission resulting from cosmic-ray interactions with matter and photons in the Milky Way
    • radio galaxies and active galactic nuclei such as Seyfert galaxies, BL Lacertae objects, and quasars
    • the extragalactic diffuse emission and a search for the emission of primordial black holes which might have formed in the early universe
    • gamma-ray burst origins
    • sources yet to be discovered or identified.

    2.1   CGRO Scientific Discoveries

    CGRO data have contributed to a number of recent discoveries in the field of high-energy astrophysics both alone and in concert with data from other missions. Each instrument has contributed its share of discoveries as the following highlights show.

    2.1.1   BATSE

    • isotropic and radially non-uniform distribution of gamma-ray bursts on the sky
    • enormous statistical diversity of GRB time profiles
    • bursting pulsar GR0 J1744-28
    • X-ray transient in Scorpius (GRO J1655-40) and correlations between X-rays and radio jets
    • discovery of several new X-ray pulsars and black hole X-ray
    • long term frequency histories of X-ray pulsars
    • terrestrial Gamma-ray flashess

    2.1.2 EGRET

    • blazars as prodigious gamma-ray emitters
    • high energy tails of gamma-ray bursts and delayed emission
    • Galactic origins of cosmic rays
    • radio-quiet pulsar nature of the source Geminga
    • sensitive map of the diffuse gamma-ray emission of the Milky Way
    • spectrum and map of the of extra-galactic, isotropic diffuse emission.

    2.1.3   OSSE

    • maps of electron-positron annihilation radiation from the center of the Galaxy.
    • spectra of blazar and Seyfert active galaxies
    • spectral break at 100-200 keV in Seyfert Active Galaxies
    • 57Co emission from supernova 1987A
    • limits on 44Ti and 56Co emissions from Cas A and SN 1991T respectively
    • hard X-ray continuum in SN 1993J
    • thermal and non-thermal spectral states in black hole candidates
    • nuclear gamma ray emission from solar flares.

    2.1.4   COMPTEL

    • fundamental insight into the high-energy physics of solar flares. For example, temporal variations as fast as 0.1 s are observed at energies above 10 MeV constraining acceleration models.
    • detection of 57Co emission from SN 1987A.
    • limits on 22Na emission from ONeMg novae, tightly constraining nova models.
    • first all-sky map of Galactic 26Al, tracing sites of recent stellar nucleosynthesis.
    • results on the extragalactic diffuse gamma-ray emission compatible with power-law extrapolations and showing no evidence for an MeV excess.

  3.   Instruments

    3.1   BATSE

    The primary objective of BATSE, the Burst And Transient Source Experiment, is the detection, location and study of gamma-ray bursts. BATSE’s large area detectors (LADs) , spectral detectors (SDs) and versatile data system, provide sensitive and comprehensive observations of gamma-ray bursts. The Earth occultation technique detects transient sources above 20 keV and permits studies of variability in stronger sources. Many pulsars can be observed by BATSE using the temporal characteristics of the sources - data are epoch folded onboard or on the ground. BATSE instrument details are on our Web site (see Appendix A) and in the instrument paper (see Appendix B).

    3.2   EGRET

    The Energetic Gamma Ray Experiment Telescope (EGRET) detects gamma rays using a spark chamber for direction measurement and, at its base, a NaI(Tl) calorimeter, the Total Absorption Shower Counter (TASC), for energy measurement. The spark chamber has interleaved tantalum foils and tracking layers where a fraction of incoming gamma rays interacts to produce high-energy positron-electron pairs, which are tracked through subsequent layers and absorbed by the TASC. Reconstruction on the ground of the energies and directions of the positron-electron pairs yields the energies and directions of the incident photons. A plastic scintillator anti-coincidence shield and time-of-flight measurement system prevent false triggers on charged particles or upward-moving events. A complete description of the EGRET experiment can be found at our Web site and in the instrument paper (see Appendices).

    Figure 1: Egret All-Sky Map

    The spark chamber gas, a noble gas-hydrocarbon mixture, needs to be changed periodically as the gas 'ages' from sparking. Egret was launched with enough extra gas for five refills. Now, well beyond the nominal three-year lifetime of Egrent, only enough gas remains for a partial refill. As a result, in Cycle 8, only approximately six weeks of reduced field-of-view observations will be scheduled.

    3.3   OSSE

    The Oriented Scintillation Spectrometer Experiment, consists of four NaI(Tl)-CsI(Tl) phoswichs and permits offset pointing on two-minute timescales for background accumulations and observations of two sources during each orbit. The detectors are generally pointed in co-axial pairs in the x-z plane of the CGRO spacecraft. The instrument can be operated in an on-source/off-source mode to handle background subtraction from point sources and also a scanning mode to map extended sources. The broad field-of-view enables coverage of diffuse emission from the galactic center and galactic plane for observation of nuclear lines associated with radioactive decay of products from explosive nucleosynthesis and from the interaction of cosmic rays and the interstellar medium. OSSE’s slewing capability permits pointing to selected events (typically Gamma-ray or solar flares) detected by BATSE.

    3.4   COMPTEL

    Interactions in the telescope occur in a two stage process: first a Compton collision occurs in one of seven (low-Z) liquid scintillators and is usually then completely absorbed in one of fourteen (high-Z) NaI(Tl) scintillators. The unusual aspect of this detector is that the location of the gamma-ray on the sky is given by an annulus and not a point. The correlation of many events enables the localization of point sources or the creation of sky maps. Time-of-flight measurements, pulse shape discrimination and anti-coincidence shields are used to reject background events. CompTel has a wide field of view (about 1 steradian) and an angular resolution under optimal conditions of about 1o. Its energy resolution ranges from 5-10% at 1 MeV. During Phase 1 of the mission, COMPTEL completed the first all-sky survey between 0.75-30 MeV (in four energy bands). In addition, COMPTEL can measure energy spectra of solar flares or bright cosmic gamma-ray bursts between 0.1-10 MeV, and neutrons from solar flares.

    Figure 2: First COMPTEL map of the plane of the Milky Way Galaxy in the emission of 1.809-MeV gamma-rays from the radioactive decay of 26-Aluminum

  4. The CGRO archive

    The archive contains public-domain data products from each of the four instruments, packaged into FITS or other standard format. Products are listed by experiment below.

    Reprocessed data is archived on receipt and BATSE trigger and daily data are now on an accelerated delivery schedule to be available from the archive shortly after acquisition and processing. Most other products, however, become public closer to a year after acquisition although a more aggressive schedule is likely in future.

    BATSE trigger data (our most requested data set) has recently been placed on disk as well as in the jukebox, permitting faster access and an on-line backup to speed scientific work and reduce strain on the jukeboxes. Other data may be similarly configured in future. During 1998, most CGRO data will become accessible through the W3Browse system maintained by the HEASARC. Also in 1998 much previously inaccessible or reprocessed data will become available for OSSE and COMPTEL -neither of which has previously provided FITS formatted data.

    Of special interest, the EGRET low-level ('Primary Database') data set will be made available in its entirety for the first time. These data are undergoing FITS wrapping and transfer from the EGRET archive during Spring of 1998 and will be available shortly thereafter. The Primary Database contains raw EGRET data for reconstructing the tracks of Gamma-ray events. It also contains spectra recorded in the TASC throughout the mission and all housekeeping data.

    FTP access to all CGRO holdings can be made anonymously. Products can be browsed and downloaded in a variety of forms, including tar files. All data except text files are compressed using the GNU utility GZIP. Access to the data - and to much ancillary information - can also be made through our Web site. Detailed descriptions of the GRO data are contained in 'Appendix G' (the technical appendix to the CGRO NRA) at http://cossc.gsfc.nasa.gov/cossc/nra/appendix_g.html, which is available on the Web. Requests for assistance in using the data should be addressed to the COSSC at grohelp@cossc.gsfc.nasa.gov(see Appendix A of this document for electronic access information)

    4.1   BATSE

    Data are divided into four groups: trigger, daily, occultation, and pulsar. Each group has structured directories beneath it containing data ordered by an appropriate criterion. Typically, several files of data are necessary to form a complete set of data for a particular entity.

    Trigger data (ordered by trigger number) are the most-requested data type. Each identified trigger is classified as a flare, burst, sgr (soft gamma-ray repeater), tgf (terrestrial gamma flash), or tagged with the name of a known source. Not all triggers pass the acceptance tests, so not all numbers are present. The 4th burst catalog is available on the Web at http://cossc.gsfc.nasa.gov/cossc/batse/4Bcatalog/4b_catalog.html A physical copy can be obtained by sending email to grohelp@cossc.gsfc.nasa.gov.

    Each trigger directory contains a collection of FITS files that represent the raw data sources and some higher-level products. Table 4.1-1 summarizes these. Spectral (SD) data are prefixed with an 's' (e.g. 'sher'). Not all data types are available for all triggers due to instrument mode differences. Available data taken prior to the trigger may contain the beginning of the triggering event before it satisfied the triggering criteria. Background-type files can be used to remove background signal levels from the triggered period. The BFITS data files - containing burst and background spectral data as a function of time - and the detector response matrices (DRM) - modeling the instrument response to account for scattering and other effects - are extremely useful for gamma-ray burst analysis. Also, the BFITS and DRM files can be converted to PHA-II and RMF format for analysis with XSPEC using available FTOOLS. File types listed in the table are the most useful. Other types exist and advice on their use is obtainable at grohelp@cossc.gsfc.nasa.gov.

    OCCULTATION: The BATSE occultation data set is organized by source, and within the source, by TJD. FTOOLS are available to transform these data sets for use by XSPEC by creating summed PHA files and their associated detector response matrices. Light curves may be obtained from these data.

    PULSAR: The BATSE pulsar data are organized similarly to the OCCULTATION data set with the difference being in the filename extensions: 'olc' files contain on-board folded light curves, 'pll' files contain pulsar low level data.

    DAILY: BATSE daily data sets are the largest BATSE data set and have, as a result, more directory levels based on TJD to permit their effective management. (The number of directory levels was increased in 1997). These data are the backdrop against which the triggers occur, and contain lower time-resolution data samples from the BATSE detectors. Generally, only two file types are available: CONT and DISCLA.

    Figure 3: Batse Light Curve for Trigger 143

    Table 4.1-1 Summary of BATSE data files and their contents

    Naming convention

    Contents

    tte_bfits_YYYY.fits

    time-sequenced 4-energy channel data bracketing trigger; combines discla, preb, discsc, and tte.

    discsc_bfits_YYYY.fits

    time-sequenced 4-energy channel data bracketing time of burst trigger for triggered detectors; combines data types discla, preb and discsc.

    (s)her_bfits_X_YYYY.fits

    time-sequenced 128 energy channel data bracketing time of burst trigger for specified detector; combines datatypes her and herb - suggested data type for 128 energy channel burst analysis.

    mer_bfits_YYYY.fits

    time-sequenced 16-energy channel data for times bracketing burst trigger - triggered detectors only; combines mer and cont datatypes - suggested for 16-energy channel burst analysis.

    discsc_drm_YYYY.fits

    detector response matrix for 4 energy channel burst data triggered detectors only; used with 4-energy channel data to determine burst photon spectra.

    her_drm_X_YYYY.fits

    detector response matrix for 128-energy channel burst data for specified detector; used with 128-energy channel counts data to generate burst photon spectra.

    mer_drm_YYYY.fits

    detector response matrix for 16-energy channel burst data triggered detectors only; used with 16-energy channel data to generate burst photon spectra.

    cont_TJD_fits

    8 batse detectors, 2.048s resolution/16 energy channels.

    discla_TJD.fits

    8 batse detectors, 1.024 s resolution/4 energy channels.

    XXX_TJD1_TJD2_his.fits

    Occultation histories.

    XXX_TJD1_TJD2_nhis.fits

    Data for one or more BATSE detectors for available energy channels as source count rate (counts/sec) from which the background has been subtracted - used for light curves

    XXX_TJD_lad_p11.fits

    Pulsar low level data

    XXX_TJD1_TJD2_lad_olc

    Light curve file for a given pulsar

    YYYY = trigger number, XXXX = source name, TJD = Truncated Julian Day, X = detector number

    4.2   EGRET data holdings

    EGRET data can be obtained via ftp://cossc.gsfc.nasa.gov/pub/data/egret/. The high level data products are indexed in W3Browse and also available on CD-ROM (through the beginning of Cycle 6; see http://cossc.gsfc.nasa.gov/cossc/egret/egret_cd.html). The EGRET data area is divided into high level and low level products; the high level products are the most useful for analysis. Within the high_level and low_level directory trees, the data products are stored in subdirectories by observatory operating phase (phase1, phase2, etc.) and viewing period (e.g., pnt_3370 for viewing period 337.0).

    The high level data products include maps of photon counts, instrument exposure, and gamma-ray intensity (counts divided by exposure) binned in 0.5 deg pixels as well as time-ordered lists of photons including arrival times, energies, directions, and a great deal of additional information. Also included is an 'exposure history' file, used by the INTMAP program (see below) to construct exposure and intensity maps. The standard counts, exposure, and intensity maps are in Galactic coordinates except when the viewing direction was close to the Galactic pole; in these cases, the maps are in celestial coordinates. Maps are available for four standard sets of energy ranges as shown below:

    Table 4.2-1 EGRET High-Level Data Available For Each Viewing Period (#####)

    Filename

    Description

    qvp_vp####s.fits

    Time-ordered list of photons with well-determined energies and directions(within 30oof axis, EGRET - full FOV mode)

    wvp_vp####s.fits

    Time-order list of photons further off axis

    counts_vp####_g00#.fits

    Maps of photon counts

    exposr_vp####_g00#.fits

    Maps of instrumental exposure

    intens_vp####_g00#.fits

    Maps of gamma-ray intensity

    exphst.v01p####.fits

    Exposure history file for INTMAP

    rdf####.fits

    Composite file containing qvp and exphst files

    Energy Ranges of the Standard Maps

    Extension

    Energy ranges of maps in file (MeV)

    g001

    30-50, 50-70, 70-100, 100-150, 150-300, 300-500, 500-1000, 1000-2000, 2000-4000, and 4000-10000

    g002

    30-100 and 100-10000

    g003

    30-300 and 300-1000

    g004

    30-1000 and 1000-10000

    Also available under the high_level directory tree is a set of composite counts, exposure, and intensity maps covering the entire sky derived from all viewing periods in Phase 1, Phase 2, etc. as well as the tables from the Second EGRET Source Catalog (Thompson et al.1995).

    The low_level directory contains EGRET Primary Database files, organized by observatory operating phase (phase1, phase2, etc.) and viewing period (e.g., pnt_3370 for viewing period 337.0). The Primary Database files contain records for each trigger of the EGRET spark chamber, regardless of subsequent rejection. They contain records of background spectra every ~30 sec in the TASC, instrument housekeeping, and the rare gamma-ray events that satisfy the Microsecond Burst trigger requirement, used to record events that appear to result from multiple, nearly simultaneous arrivals of gamma rays.

    4.3   OSSE's data holdings

    OSSE's archive is undergoing the final stages of a major reorganization and is being gradually rebuilt with the new data products described below. Some are already on line and the archive will grow gradually. Completion is scheduled for Fall, 1998.

    Raw OSSE data are stored in VAX/VMS indexed files called SDB (for Spectral Data Base) format. This format is designed for efficient processing by the IGORE (Integrated GRO/OSSE Reduction Environment) analysis package which is currently the only software which can perform in-depth analysis of OSSE data. OSSE data are archived as follows:

    Table 4.3-1 OSSE data products available

    Data type

    Name

    Contents

    Low Level

    pYDOY0000_spm.fits

    Spectral files of pointed or designated sources

     

    pYDOY0000_burst.fits

    Shield spectra (from active shielding)

     

    pYDOY0000_c60.fits

    60Co calibration data

     

    pYDOY0000_c60sm.fits

    60Co calibration data - summary

     

    pYDOY0000_pdf.fits

    Contains event and/or binned rate data

    High Level

    TTT_VVV_xspec.tar

    XSPEC PHA and RMF files for each detector of the observation

     

    TTT_VVV_bln.ps

    PostScript output of 'bottom line' spectra (2)

     

    TTT_VVV_state.ps

    PostScript output of the detector pointing strategy

     

    TTT_VVV.log

    Log file of the analysis run - examine this before analyzing data

     

    vpVV_notes.doc

    Information about viewing period analysis - check before use

     

    TT_VV.tot.fits

    Totaled spectrum for observation by detector with DRM (1)

     

    TT_VV.gsm.fits

    Good-summed spectra of daily-averaged background-subtracted count spectra by detector (1)

     

    TT_VV.bln.fits

    Bottom-line spectra containing observation averaged, background subtracted, deconvolved photon spectra. (2)

     

    pYDOY0000_xxxx.fits

    Daily difference spectra of two-minute accumulations of background subtracted spectra (1)

     

    TT_VV_phot.dat

    Averaged Photon Spectrum: The observation-averaged photon spectrum (already deconvolved )in text format for plotting (2)

     

    TT_VV_eband.ps

    PostScript plot of count time series over several energy bands

     

    TT_VV_counts.ps

    Count spectra over several accumulation intervals

    (1) Products are best used with IGORE; (2) deconvolution performed with E-2 deconvolution model;

    TT = a form of the target name e.g. GX 1+4 ; VV = Viewing period; xxxx = target designator (primary, secondary etc.); YDOY = 2-digit year and day-of-year (Jan 1 = DOY 1)

    Low-level products must be reconverted to their original format to be used with existing analysis tools and converter software is available for this purpose. COSSC staff can assist with the installation of IGORE on VAX platforms only.

    The OSSE SDB and PDF files are converted to FITS format at the COSSC. High-level data products and more detailed description of their contents are available through the Web: http://cossc.gsfc.nasa.gov/cossc/osse/hilev/hilev.html. Other products are available via anonymous FTP (ftp://cossc.gsfc.nasa.gov/compton/data/osse/) and can be searched for with W3Browse (capability will grow as archive is replenished during 1998).

    Figure 4:
    Map of the 511 keV emission from the galactic center region constructed from OSSE data. The image was constructed by the OSSE team at the Naval Research Laboratory and Northwestern University. It suggests the existence of an 'annihilation fountain' of positrons from the Galactic Center.

    4.4 COMPTEL data holdings

    The COMPTEL archive contains both native and FITS data. The FITS data is the native binary data product (which, in its pre-FITS form is intended solely for use by COMPASS - COMPTEL's Oracle-based data analysis system) with ancillary information extracted from the COMPASS database used to create the FITS header and properly describe the data. Only recently have these files been made available to the public via WWW and FTP. W3Browse access should be available by 1998 October 1. The FTP archive is organized by observing cycles (phase 1, phase 2, etc.) and by viewing period (e.g. pnt_3370 for viewing period 337.0).

    Table 4.4-1 COMPTEL data by type and name

    Type of data

    Name

    Contents

    Low Level Data

    EVP

    processed event

     

    TIM

    Exposures

     

    HKD

    housekeeping (daily)

     

    OAD

    orbit and attitude (daily)

     

    BVC

    barycentric velocity correction

    High Level Data

    DRE

    binned event (one per energy range)

     

    DRX

    binned exposure (one per energy range)

     

    DRG

    binned geometry (one per energy range)

     

    MLM

    maximum likelihood map (one per energy range)

     

    PBS

    processed burst spectra (daily)

    Except as otherwise noted, each file is available on a per viewing period basis. Typically, the standard high level MLM data in four energy bands is useful for quick look purposes as it contains simple FITS skymap images which overlay counts, intensity, and statistical significance for integrated COMPTEL data.

  5. TOOLS AVAILABLE FOR ANALYSIS AND DISPLAY OF CGRO DATA

    The major FTOOL package at http://heasarc.gsfc.nasa.gov/docs/software/ftools/gro.html contains a wide variety of tools many of which offer capabilities for the CGRO data - which is also accessible to other analysis systems like XSPEC. For specific assistance in using any CGRO product, staff scientists at the CGRO Science Support Center can be contacted via cossc@cossc.gsfc.nasa.gov or grohelp@cossc.

    5.1 BATSE FTOOLS AND OTHER ANALYSIS TOOLS

    There are several FTOOLS designed specifically for BATSE data, and the data are also convertible for use in other analysis/display systems like XSPEC. In addition several non FTOOL capabilities are available (see table in Appendix A for locations):

    FTOOL name

    Available

    Function

    fbbft2pha

    Now

    Converts BATSE BFITS file to spectral PHA file

    fbdrm2rmf

    Now

    Converts BATSE DRM file to RMF format

    bod2pha

    Now

    Converts BATSE NHIS data to spectral PHA file

    bodgetvp

    Now

    Gets the viewing period of the BATSE earth occultation file

    5.2 EGRET FTOOLS

    Standard analysis programs provided by the EGRET instrument team are being converted to FTOOLs. ADDMAP - already converted - is used to combine counts, exposure, and intensity maps. MAPGEN is used to generate counts maps for arbitrary coordinate grids and energy ranges and INTMAP is used to derive corresponding exposure and intensity maps. Other programs, such as SPECTRAL for deriving source spectra, and PULSAR for phase binning of photons from gamma-ray pulsars, may also be converted.

    FTOOL name

    Available

    Function

    econvpha

    Now

    Converts EGRET .spec files to XSPEC .pha files

    econvrmf

    Now

    Converts EGRET .resp files to XSPEC .rmf files

    addmap

    Now

    Coadds two different sky maps

    intmap

    Aug 98

    Takes counts maps to create intensity maps

    mapgen

    Aug 98

    Makes raw data into counts maps

    fesdb2rdf

    Now

    (used in pipeline)

    Reads i/p QVP and EXP (optional) data files and writes an o/p FITS data file in OGIP standard format

     

    5.3 OSSE FTOOLS

    The OSSEDRM FTOOL (under development) will generate an OSSE response matrix, for use with XSPEC, for any source in the OSSE field-of-view. This is useful for source-confused regions. We plan no capability outside IGORE (an IDL-based tool for analysis and display of OSSE data available for use on VAX/VMS systems only) for performing a rigorous deconvolution of the spectra of multiple sources in a single field-of-view. The OSSE Guest Investigator Guide is available through the high-level archive Web pages and is filled with examples of OSSE spectral analysis. High-level PHA & RMF products can be analyzed with XSPEC (available from the HEASARC) and IGORE can also be obtained for analysis and display.

    5.4   COMPTEL FTOOLS

    No FTOOLS are planned for COMPTEL and access to the COMPASS environment is therefore necessary (contact COSSC). Availability of the data in FITS format may stimulate the development of further analysis capability using FITS based methods.

    Appendix A - Ancillary information

    Principal Investigators:

    OSSE

    Dr. James D. Kurfess at the Naval Research Laboratory

    EGRET

    Dr. David Bertsch at Goddard Space Flight Center, Dr. Klaus Pinkau, Max Planck Institute for Extraterrestrial Physics

    BATSE

    Dr. Gerald Fishman, Marshall Space Flight Center

    COMPTEL

    Dr. V. Schönfelder of Max-Planck Institute for Extraterrestrial Physics

    WEB and FTP site information

     

    URL

    Contents

    http://cossc.gsfc.nasa.gov/cossc/nra/appendix_g.html

    Technical appendix describing instruments

    http://cossc.gsfc.nasa.gov/

    Compton GRO home page - contains many useful links and references plus how to get in touch with COSSC personnel

    ftp://cossc.gsfc.nasa.gov/compton/data

    Directory for GRO FTP data access

    http://osse-www.nrl.navy.mil/osselib.html

    Preprints for OSSE

    ftp://cossc.gsfc.nasa.gov/pub/software/batse/ (no longer works)

    BATSE software products including

    • burst_ibdb_structures: the Fortran structures which define the data formats in which the BATSE ibdb data is stored
    • quick_look_util: a utility to take a quick look at batse discsc and erb data
    • ibdb_v10:to/from FITS conversions for BATSE ibdb/cont data

    http://heasarc.gsfc.nasa.gov/docs/software/ftools/gro.html

    Information on FTOOLS for GRO

    http://cossc.gsfc.nasa.gov/cossc/egret/egret_cd.html

    Egret CD information

    http://www.batse.msfc.nasa.gov/tools/

    Code and documentation for WINGSPAN BATSE analysis software package

    http://cossc.gsfc.nasa.gov/cossc/batse/hilev/occul_tools.html

    BATSE occultation analysis tools limb.pro & src_plot.pro

    http://wwwgro.unh.edu/comptel/comptel_main.html

    COMPTEL collaboration home page

    http://cossc.gsfc.nasa.gov/cossc/batse/4Bcatalog/4b_catalog.html

    BATSE CD image


    Email addresses: cossc@cossc.gsfc.nasa.gov or grohelp@cossc.gsfc.nasa.gov

    Appendix B - Reference Bibliography

    BATSE references

    Fishman, G.J., et al. 1991, in Proc. The Compton Observatory Science Workshop, (NASA CP-3137)
    Wilson, R.B. et al. 1991, in Proc. The Compton Observatory Science Workshop
    Harmon, B.A. et al. 1994, in 2nd Compton Symposium, AIP Conf. Proc. 304, 210
    Briggs, M.S., et al. 1996, ApJ 459, 40
    Meegan, C.A., et al. 1996, ApJ supplement, 106,65
    Finger, M.H., et al. 1997, in 4th Compton Symposium, AIP Conf. Proc 410, 57
    Wilson, C.A. et al. 1998, to appear in ApJ, 499
    Bildsten, L. et al. 1997, APJ Supplement, 113,367

    EGRET references

    Bertsch, D.L., et al. 1989, in Proc. Gamma-Ray Observatory Science
    Workshop, ed. W.N. Johnson (Greenbelt:NASA),2-52
    Hughes, E.B., et al. 1980, IEEE, Trans. Nucl. Sci., NS-27, 364
    Kanbach, G., et al. 1988, Space Sci. Rev., 49, 69
    Kanbach, G., et al. 1989, in Proc. Gamma-Ray Observatory Science
    Workshop, ed. W.N. Johnson (Greenbelt:NASA),2-1
    Thompson, D.J., et al. 1993, ApJS, 86, 629
    Thompson, D.J., et al. 1993, ApJ, 415, L13
    Thompson, D.J., et al. 1995, ApJS, 101, 259
    Thompson, D.J., et al. 1996, ApJS, 107, 227

    OSSE References

    Cameron, R.A. et al., NASA Conf. Publication 3137, p3 (1991)
    Johnson, W.N. et al. in Proc. Gamma-Ray Observatory Science Workshop, ed W.N. Johnson (Greenbelt, NASA), 2-22 (1989)
    Johnson, W.N. et al., 1992 Astron. & Astrophys. Suppl. 97, p21 Copyright 1992, European Southern Observatory (ESO
    Kurfess, J.D. et al. in Proc. Gamma-Ray Observatory Science Workshop, ed W.N. Johnson (Greenbelt, NASA), 3-35 (1989)
    Kurfess, J.D. Annuals of the New York Academy of Sciences, V759, p236 (1995)
    Kurfess, J.D. 3rd Compton Symposium, Astronomy and Astrophysics Supplement Series, 120, p5 (1996)
    Purcell, W.R. et al., NASA Conf. Publication 3137, p15 (1991)

    COMPTEL references

    van Dijk, Rob, 1996, "Gamma-Ray Observations of X-Ray Binaries with COMPTEL", Ph.D. thesis.
    Dermer, C.D., Strickman, M.S., & Kurfess, J.D. 1997, "Fourth Compton Symposium", AIP Conf. Proc. 410.
    Grewing, M., Kanbach, G., & Schoenfelder, V. 1996, "Third Compton Symposium", A&A Supp, 120.
    Schönfelder, V. et al., 1993, ApJS,86, 657

     


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