- ID:
- ivo://nasa.heasarc/gingamode
- Title:
- Ginga LAC Mode Catalog
- Short Name:
- GINGAMODE
- Date:
- 25 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The GINGAMODE database table contains selected information from the Large Area Counter (LAC) aboard the third Japanese X-ray astronomy satellite Ginga. The Ginga experiment began on day 36, 5 February 1987 and ended in November 1991. Ginga consisted of the LAC, the all-sky monitor (ASM) and the gamma-ray burst detector (GBD). The satellite was in a circular orbit at 31 degree inclination with apogee 670 km and perigee 510 km, and with a period of 96 minutes. A Ginga observation consisted of varying numbers of major frames which had lengths of 4, 32, or 128 seconds, depending on the setting of the bitrate. Each GINGAMODE database entry consists of data from the first record of a series of observations having the same values of the following: "BITRATE", "LACMODE", "DISCRIMINATOR", or "ACS MONITOR". When any of these changed, a new entry was written into GINGAMODE. The other Ginga catalog database, GINGALOG is also a subset of the same LAC dump file used to create GINGAMODE. GINGALOG contains a listing only whenever the "ACS monitor" (Attitude Control System) changes. Thus, GINGAMODE monitors changes in four parameters and GINGALOG is a basic log database mapping the individual FITS files. Ginga FITS files may have more than one entries in the GINGAMODE database. Both databases point to the same archived Flexible Image Transport System (FITS) files created from the LAC dump files. The user is invited to browse though the observations available from Ginga using GINGALOG or GINGAMODE, then extract the FITS files for more detailed analysis. The Ginga LAC Mode Catalog was prepared from data sent to NASA/GSFC from the Institute of Space and Astronautical Science (ISAS) in Japan. <p> Duplicate entries were removed from the HEASARC implementation of this catalog in June 2019. This is a service provided by NASA HEASARC .
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352. Ginga LAC Raw Data
- ID:
- ivo://nasa.heasarc/gingaraw
- Title:
- Ginga LAC Raw Data
- Short Name:
- GINGARAW
- Date:
- 25 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The GINGARAW database table provides access to the raw GINGA files in FITS format for the LAC experiment. Ginga was the third Japanese X-ray astronomy satellite. It was launched into low Earth orbit on 5th February 1987 and re-entered the atmosphere on 1st November 1991. The scientific payload consisted of the Large Area Counter (LAC; Turner et al. 1989), the All-Sky Monitor (ASM; Tsunemi et al. 1989) and the Gamma-ray Burst Detector (GBD; Murakami et al. 1989). A full description of the satellite is given in Makino et al. (1987). During its lifetime Ginga performed over 1000 pointed observations of approximately 350 different targets, covering all then known classes of cosmic X-ray sources. The LAC experiment, sensitive to X-rays with energy 1.5-37 keV, was the main scientific instrument aboard Ginga. It was designed and built under a Japan-UK collaboration (ISAS, U. Tokyo, Nagoya U., U. Leicester, Rutherford Appleton Lab). It consisted of an array of eight collimated co-aligned proportional counters with a total effective area of approximately 4000 cm<sup>2</sup>. Steel collimators restricted the field of view to 1.1 x 2.0 degrees (FWHM). This database table was last updated by the HEASARC in August 2005. Galactic coordinates were added and some parameters were renamed to adhere to the HEASARC's current parameter naming conventions. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/gingalac
- Title:
- GingaSourceLightcurves&Spectra
- Short Name:
- GINGALAC
- Date:
- 25 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The GINGALAC database table contains a summary of the contents of the Ginga pointed observations. This table has been produced from the raw Ginga LAC First Reduction Files (FRFs) and contains information of the individual pointings in addition to FITS spectra and light curves, HDS and FITS data cubes and the plots produced during the pipeline processing. These products can be used with either the Ginga data analysis software or the <a href="/docs/xanadu/xanadu.html">XANADU software suite</a>. This archive (database and all the associated products) is a copy of the GINGA LAC data products held at the Leicester Data Archive Service (<a href="http://ledas-www.star.le.ac.uk">http://ledas-www.star.le.ac.uk</a>). It was delivered to the HEASARC in 1999 as part of an archive exchange between the data centers. The original version was updated in October 2008, when the positions (which had been created assuming the wrong equinox) were corrected; in addition, the values of the nh parameter were corrected. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/cns3
- Title:
- Gliese Catalog of Nearby Stars, 3rd Edition
- Short Name:
- CNS3
- Date:
- 25 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The CNS3 catalog contains all known stars as of 1991 that are within 25 parsecs of the Sun. It depends mainly on a preliminary version (Spring 1989) of the new General Catalogue of Trigonometric Parallaxes (YPC) prepared by Dr. William F. van Altena (Yale University). The catalog contains every then-known star with a trigonometric parallax greater than or equal to 0.0390 arcsec, even though it may be evident from photometry or for other reasons that the star has a larger distance. For red dwarf stars, new color-magnitude calibrations for broad-band colors were carried out and applied. For white dwarfs, the recipes of McCook and Sion in ApJS, 65, 603 (1987) were applied. Stroemgren photometry was used (not yet systematically) for early-type stars and for late dwarfs, the latter supplied by E. H. Olsen from Copenhagen Observatory (private communication). In contrast to the CNS2 (Gliese 1969) catalog, trigonometric parallaxes and photometric or spectroscopic parallaxes were not combined in this version. The resulting parallax in the present version is the trigonometric parallax if the relative error of the trigonometric parallax is smaller than 14 percent. The parallax may be the photometric or spectroscopic parallax only if no trigonometric parallax is available or if the standard error of the trigonometric parallax is considerably larger. The original catalog and the notes describing it were prepared by Wilhelm Gliese and Hartmut Jahreiss, Astronomisches Rechen-Institut, Moenchhofstrasse 12-14, D-6900 Heidelberg 1, Germany, in 1991. The CDS has made a number of formatting and documentation changes in the period 1994-1997, e.g., in December 1997 it added a running number to the name for 1388 stars which had all been given the same name of "NN" in the original version, starting with "NN 3001" (for the first "NN" star in order of 1950 RA), and ending with "NN 4388" (for the last "NN" star in order of 1950 RA). This revised version of the catalog (CDS/ADC Catalog V/70A) was used by the HEASARC to create this database in February 2001. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/gliese2mas
- Title:
- Gliese Catalog Stars with Accurate Coordinates and 2MASS Cross-Identifications
- Short Name:
- GLIESE2MAS
- Date:
- 25 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains precise epoch 2000 coordinates and cross-identifications to sources in the 2MASS Point Source Catalog for nearly all stars in the Gliese, Gliese-Jahreiss, and Woolley catalogs of nearby stars. The only Gliese objects where the authors were not successful are two Gliese sources that are actually QSOs; two proposed companions to brighter stars, which they believe do not exist; four stars included in one of the catalogs but identified there as only optical companions; one probable plate flaw; and two stars that simply remain unrecovered. For the 4251 recovered stars, 2693 have coordinates based on Hipparcos positions, 1549 have coordinates based on 2MASS data, and 9 have positions from other astrometric sources. All positions have been calculated at epoch 2000 using proper motions from the literature, which are also given here. This table was created by the HEASARC in May 2011 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/PASP/122/885">CDS Catalog J/PASP/122/885</a> file table1.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/gcscat
- Title:
- Globular Cluster Systems of Galaxies Catalog
- Short Name:
- GCSCAT
- Date:
- 25 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains a catalog of 422 galaxies with published measurements of their globular cluster (GC) populations. Of these, 248 are E galaxies, 93 are S0 galaxies, and 81 are spirals or irregulars. Among various correlations of the total number of GCs with other global galaxy properties, the authors find that the number of globular clusters N<sub>GC</sub> correlates well though nonlinearly with the dynamical mass of the galaxy bulge M<sub>dyn</sub> = 4 sigma _e_<sup>2</sup> R<sub>e</sub>/G, where sigma<sub>e</sub> is the central velocity dispersion and R<sub>e</sub> the effective radius of the galaxy light profile. In their paper, the authors also present updated versions of the GC specific frequency S<sub>N</sub> and specific mass S<sub>M</sub> versus host galaxy luminosity and baryonic mass. These graphs exhibit the previously known U-shape: highest S<sub>N</sub> or S<sub>M</sub> values occur for either dwarfs or supergiants, but in the mid-range of galaxy size (10<sup>9</sup> - 10<sup>10</sup> L<sub>sun</sub>) the GC numbers fall along a well-defined baseline value of S<sub>N</sub> ~= 1 or S<sub>M</sub> = 0.1, similar among all galaxy types. Along with other recent discussions, the authors suggest that this trend may represent the effects of feedback, which systematically inhibited early star formation at either very low or very high galaxy mass, but which had its minimum effect for intermediate masses. Their results strongly reinforce recent proposals that GC formation efficiency appears to be most nearly proportional to the galaxy halo mass M<sub>halo</sub>. The mean "absolute" efficiency ratio for GC formation that the authors derive from the catalog data is M<sub>GCS</sub>/M<sub>halo</sub> = 6 x 10<sup>-5</sup>. They suggest that the galaxy-to-galaxy scatter around this mean value may arise in part because of differences in the relative timing of GC formation versus field-star formation. Finally, they find that an excellent empirical predictor of total GC population for galaxies of all luminosities is N<sub>GC</sub> ~ (R<sub>e</sub> sigma<sub>e</sub>)<sup>1.3</sup>, a result consistent with fundamental plane scaling relations. This table was created by the HEASARC in February 2014 based on an electronic version of Table 1 from the reference paper which was obtained from the ApJ web site. A duplicate entry for NGC 4417 was removed in June 2019. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/gusbad
- Title:
- GRBs Uniformly Selected from BATSE Archival Data (Version 2.1)
- Short Name:
- BATSE/GUSBAD
- Date:
- 25 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The GUSBAD (Gamma-ray bursts Uniformly Selected from BATSE Archival Data) Catalog is based on BATSE DISCLA data at a time resolution of 1.024 seconds for the full 9.1 years of the Compton Gamma-Ray Observatory (CGRO) mission from April 19, 1991 until May 26, 2000 (corresponding to Truncated Julian Dates from 8365 to 11690). This catalog lists over 2200 gamma-ray bursts (GRBs). Selection of GRBs for the GUSBAD Catalog requires a 5-sigma excess over the background in two of the BATSE detectors over the energy range 50-300 keV. The search covers the entire mission except when CGRO was over particular geographic regions or during one of 199,964 time windows when DISCLA data were missing or contaminated. The classification as GRB or non-GRB of the 6236 events that were produced by the software trigger was aided by correlating the times and positions of the events against the Current BATSE Burst Catalog. There are 589 GRBs in the GUSBAD Catalog that are not included in the Current BATSE Burst Catalog. The GUSBAD catalog is uniform in the sense that the detection criterion is the same throughout and that the properties given in the catalog are available for every burst. The detection and the derivation of the properties listed in the catalog were carried out automatically, except for some rare instances. This makes the catalog especially suitable for statistical work and simulations, such as used in the evaluation of V/Vmax. The procedure used to detect and classify the bursts has been described in Schmidt (2004). This database table was last updated by the HEASARC in April 2005 using the file GUSBADcat.dat containing version 2.1 of the catalog, which was obtained from the catalog author's web site at <a href="http://www.astro.caltech.edu/~mxs/grb/GUSBAD/">http://www.astro.caltech.edu/~mxs/grb/GUSBAD/</a> <p> Comments or questions about the contents of the GUSBAD Catalog are welcomed by the author who can be contacted at mxs@astro.caltech.edu. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/gb6
- Title:
- Green Bank 6-cm (GB6) Radio Source Catalog
- Short Name:
- GB6
- Date:
- 25 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the Green Bank 6-cm (GB6) Radio Source Catalog. The Green Bank 4.85 GHz (6-cm wavelength) survey (Condon J.J., Broderick J.J., Seielstad G.A., Douglas K., & Gregory P.C. in 1994AJ....107.1829C) was made with the NRAO seven-beam receiver on the (former) 91m telescope during 1986 November and 1987 October. The final set of sky maps covering the declination band 0 deg < Dec. < +75 deg was constructed with data from both epochs. Its noise and position errors are nearly a factor of 2^(1/2) smaller than in the epoch 1987 maps, from which the 87GB Catalog (<a href="https://cdsarc.cds.unistra.fr/ftp/cats/VIII/14">CDS Catalog <VIII/14></a>) of 54,579 sources stronger than S ~ 25mJy was extracted. Therefore, the new maps were used to make the GB6 catalog of 75,162 discrete sources with angular sizes phi <= 10.5 arcmin and flux densities S >= 18mJy. The GB6 weighted differential source counts S^(5/2)n(S) between 18 mJy and 7 Jy agree well with evolutionary models based on independent data. This table was created by the HEASARC in July 2003 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VIII/40">CDS Catalog <VIII/40></a>. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/gbt31ghz
- Title:
- Green Bank Telescope 100-m 31-GHZ Radio Source Catalog
- Short Name:
- GBT31GHZ
- Date:
- 25 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The 100m Robert C. Byrd Green Bank Telescope (GBT) and the 40m Owens Valley Radio Observatory (OVRO) telescope have been used to conduct a 31-GHz survey of 3165 known extragalactic radio sources over 143 deg<sup>2</sup> of the sky. Target sources were selected from the NRAO VLA Sky Survey (NVSS) in fields observed by the Cosmic Background Imager (CBI); most are extragalactic active galactic nuclei (AGNs) with 1.4-GHz flux densities of 3-10 mJy. Using a maximum-likelihood analysis to obtain an unbiased estimate of the distribution of the 1.4 - 31 GHz spectral indices of these sources, the authors find a mean 31 - 1.4 GHz flux ratio of 0.110 +/- 0.003 corresponding to a spectral index alpha = -0.71+/-0.01 (S<sub>nu</sub> ~ nu<sup>alpha</sup>); 9.0% +/- 0.8% of the sources have alpha > -0.5 and 1.2% +/- 0.2% have alpha > 0. By combining this spectral-index distribution with 1.4GHz source counts, the authors predict 31-GHz source counts in the range 1 mJy <S<sub>31</sub> < 4 mJy, N(>S<sub>31</sub>) = (16.7+/-1.7)deg<sup>-2</sup>(S<sub>31</sub>/1mJy)<sup>(-0.80+/-0.07)</sup>. In this study, the authors present a detailed characterization of the impact of the discrete source foreground on arcminute-scale 31-GHz anisotropy measurements based upon two observational campaigns. The first campaign (the results of which are given in the OVRO31GHZ table) was carried out with the OVRO 40m telescope at 31 GHz from 2000 September through 2002 December. The second campaign (the results of which are given in the present table) used the GBT from 2006 February to May. A companion paper (Sievers et al. 2009arXiv0901.4540S) presents the five-year CBI total intensity power spectrum incorporating the results of the point-source measurements discussed here. Reported error bars include a 10% and 5% rms gain uncertainty for GBT and OVRO measurements, respectively. Sources detected at greater than 4 sigma at 31 GHz are flagged (detection_flag = 'Y'); for this calculation, the random gain uncertainty was excluded. In all 3165 sources were observed. The GBT catalog (this table) contains 1490 sources. Of the 2315 useful OVRO observations many of the non-detections (and a few detections) were superceded by more sensitive GBT observations; the OVRO catalog contained in the HEASARC's OVRO31GHZ table therefore contains data on 1675 sources. The detection rate of the OVRO measurements was 11%, and that of the GBT measurements 25%. In all, 18% of the sources were detected at 31 GHz. This table was created by the HEASARC in June 2012 based on CDS Catalpog J/ApJ/704/1433 file table3.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/snrgreen
- Title:
- Green Catalog of Galactic SNRs (June 2017 Version)
- Short Name:
- SNR(Green)
- Date:
- 25 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This catalog of known Galactic supernova remnants (SNRs) is an updated version of the catalogs of Galactic SNRs presented in detail in Green (1984, 1988), in summary form in Green (1991, 1996, 2004, 2009), and on the Web (versions of 1995-July, 1996-August, 1998-September, 2000-August, 2001-December, 2004-January, 2006-April, 2009-March, and 2014-May). [Note that the version published in Green (1996) was produced in 1993.] This June 2017 version of the catalog contains 295 SNRs, and is based on results published in the literature up to the end of 2016. The basic summary data included in this catalog for each SNR are its designation, position, angular size (in arcminutes), type, flux density at 1 GHz, spectral index, and any other names by which it is known. Notes on these parameters, on possible remnants not included, and on questionable SNRs that are listed in this catalog, are given in the full version of the catalog on the Web at <a href="http://www.mrao.cam.ac.uk/surveys/snrs/snrs.info.html">http://www.mrao.cam.ac.uk/surveys/snrs/snrs.info.html</a> It should be noted that there are serious selection effects which apply to the identification of Galactic SNRs (e.g., Green 1991, 2004, 2005, 2009, 2014), so that care should be taken if these data are used in any statistical studies. This version of the Green Catalog of Galactic Supernova Remnants was ingested at the HEASARC in July 2017. It is based on the Catalogue of Galactic Supernova Remnants, 2017 June version, <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VII/278">CDS Catalog VII/278</a>, file snrs.dat, obtained from the CDS at <a href="http://cdsarc.u-strasbg.fr/ftp/cats/VII/278/">http://cdsarc.u-strasbg.fr/ftp/cats/VII/278/</a>. This is a service provided by NASA HEASARC .
