The GINGALOG 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 GINGALOG database entry is the first record of a series of observations having the same values of "ACS MONITOR" (Attitude Control System). When this value changes, a new FITS file was written. The other Ginga catalog database, GINGAMODE is also a subset of the same LAC dump file used to create GINGALOG. GINGAMODE contains a listing whenever any of the following changes: "BITRATE", "LACMODE", "DISCRIMINATOR", or "ACS MONITOR". Thus, GINGAMODE monitors changes in several parameters and GINGALOG is a basic log of all the FITS files. Both databases point to the corresponding archived Flexible Image Transport System (FITS) files, but GINGAMODE may have more than one entry for a given FILE_LCURVE in the database. 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 Log Catalog was prepared from data sent to NASA/GSFC from the Institute of Space and Astronautical Science (ISAS) in Japan. This is a service provided by NASA HEASARC .
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 .
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 .
GLEAM 72-103: GaLactic and Extragalactic Allsky MWA Survey
Short Name:
GLEAM1
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
GLEAM, the GaLactic and Extragalactic All-sky MWA survey, is a survey of
the entire radio sky south of declination 30 degrees at frequencies
between 72 and 231 MHz. It was made with the Murchison Widefield Array
(MWA) using a drift scan method that makes efficient use of the MWA's very
large field-of-view. The survey is described in Wayth et al. (2015) and
the <a href="https://www.mwatelescope.org/gleam">website</a> at https://www.mwatelescope.org/gleam.
<p>
The data presented here are from the first year of GLEAM observing, published in:
<ul>
<li> Hurley-Walker et al. (2017): 25,000 square degrees of extragalactic sky
<li> For et al. (2018): the Large and Small Magellanic Clouds
<li> Hurley-Walker et al. (2019c): 8,000 square degrees of the Galactic plane
</ul>
A region around Centaurus A, a few other small regions described by Hurley-Walker et al. (2017), and the Galactic plane between 180 < l < 345 degrees, are not available.
<p>
The most sensitive and highest-resolution image is the 170-231MHz image
which was used for all source-finding in generating the catalogue. It has
a resolution of approximately 2.2 x 2.2/cos (dec + 26.7) arcmin at this
frequency. However, due to ionospheric distortions, the final resolution
of the survey varies by ~10% over the sky, with a direction-dependent PSF.
<p>
The <i>SkyView</i> data for the GLEAM surveys was extracted using the team's
cutout server, into small (3 degree) raw cutouts over the region covered
by the GLEAM survey. These cutouts have somewhat variable size and resolution. The
default scale (i.e., pixel size) used for <i>SkyView</i> images is given in the table
below. Since the GLEAM cutout server will not create an appropriately sized tile for the Sourth Pole, a
larger tile offset from the pole is used.
<p>
<i>SkyView</i> resamples the cutouts retreived from the GLEAM website into the image
geometry requested by the user. Only four wide-band datasets are included.
The table below gives the frequency range, central frequency and a typical pixel
scale for each of these bands.
<table border>
<tr><th colspan=5> GLEAM Bands In <i>SkyView</i> </th></tr>
<tr><th>Band</th>
<th>f<sub>min</sub> (MHz)</th>
<th>f<sub>max</sub> (MHz)</th>
<th>f<sub>C</sub> (MHz)</tg>
<th>Pixel scale (") </th>
</tr>
<tr> <td> 1 </td><td> 72 </td><td>103 </td><td> 88 </td> <td> 56 </td></tr>
<tr> <td> 2 </td><td>103 </td><td>134 </td><td>118 </td> <td> 44 </td></tr>
<tr> <td> 3 </td><td>138 </td><td>170 </td><td>155 </td> <td> 34 </td></tr>
<tr> <td> 4 </td><td>170 </td><td>231 </td><td>200 </td> <td> 28 </td></tr>
</table>
These data and 20 narrower bands are available through the team website.
<p>
To minimize resampling artifacts, this survey defaults to the Lanczos third order resampler.
SkyView tracks the size and orientation of the beam as given in each of the tiles and includes
the averaged value (i.e., the average of the input images weighted by the output pixels sampled
from each input) in the BMAJ, BMIN, and BPA keywords of any result FITS file. Provenance: Source data extracted as cutouts from <a href="http://gleam-vo.icrar.org/gleam_postage/q/form">GLEAM cutout server</a> in March 2020 with updates in July 2020.. This is a service of NASA HEASARC.
GMRT 150 MHz All-sky Radio Survey: First Alternative Data Release
Short Name:
TGSS
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
The first full release of a survey of the 150 MHz radio sky observed with
the Giant Metrewave Radio Telescope between April 2010 and March 2012 as
part of the TGSS project.
Aimed at producing a reliable compact source survey, the automated data reduction
pipeline efficiently processed more than 2000 hours of observations with minimal
human interaction. Through application of innovative techniques such as image-based
flagging, direction-dependent calibration of ionospheric phase errors, correcting
for systematic offsets in antenna pointing, and improving the primary beam model,
good quality images were created for over 95 percent of the 5336 pointings.
This data release covers 36,900 square degrees (or 3.6 pi steradians) of the
sky between -53 deg and +90 deg DEC, which is 90 percent of the total sky.
The majority of pointing images have a background RMS noise below 5 mJy/beam
with an approximate resolution of 25" x 25" (or 25" x 25" / cos (DEC - 19 deg)
for pointings south of 19 deg DEC).
The associated catalog has 640 thousand radio sources derived from an initial,
high reliability source extraction at the 7 sigma level.
The measured overall astrometric accuracy is better than 2" in RA and DEC,
while the flux density accuracy is estimated at ~10 percent.
Data is stored as 5336 mosaic images (5 deg x 5 deg).
<p>
<i>SkyView</i> uses Lanczos resampling and Sqrt image scaling by default for this
survey. Provenance: TGS ADR Team. This is a service of NASA HEASARC.
This survey comprises the 2 Ms Chandra Deep Field North and 4 Ms Deep Field South ACIS observations.
All observations are co-added into two fields in the north and south. Data are provided in three bands,
the soft 0.5-2 keV band, the hard 2.0-8.0 keV and the full 0.5 to 8 keV band. Provenance: Taken from the Neil Brandt's PSU websites for the the
<a href="https://personal.psu.edu/wnb3/hdf/hdf-chandra.html">north</a>
and
<a href="https://personal.psu.edu/wnb3/cdfs/cdfs-chandra.html">south</a>.. This is a service of NASA HEASARC.
GOODS-Herschel is an open time key program of more than 360 hours of observation with the Hershel, SPIRE and PACS, from 100 um and 500.
<p>
North and South GOODS data is available for 100 and 160 microns (using PACS) but only the northern field is
available at 250, 350 and 500 microns (using SPIRE).
<p>
Note that the scale and resolution of the underlying pixels is different in each band. Provenance: Downloaded from the <a href="https://hedam.lam.fr/GOODS-Herschel/">Herschel Database in Marseille</a>. Release DR1.. This is a service of NASA HEASARC.
GOODS-Herschel is an open time key program of more than 360 hours of observation with the Hershel, SPIRE and PACS, from 100 um and 500.
<p>
North and South GOODS data is available for 100 and 160 microns (using PACS) but only the northern field is
available at 250, 350 and 500 microns (using SPIRE).
<p>
Note that the scale and resolution of the underlying pixels is different in each band. Provenance: Downloaded from the <a href="https://hedam.lam.fr/GOODS-Herschel/">Herschel Database in Marseille</a>. Release DR1.. This is a service of NASA HEASARC.
GOODS-Herschel is an open time key program of more than 360 hours of observation with the Hershel, SPIRE and PACS, from 100 um and 500.
<p>
North and South GOODS data is available for 100 and 160 microns (using PACS) but only the northern field is
available at 250, 350 and 500 microns (using SPIRE).
<p>
Note that the scale and resolution of the underlying pixels is different in each band. Provenance: Downloaded from the <a href="https://hedam.lam.fr/GOODS-Herschel/">Herschel Database in Marseille</a>. Release DR1.. This is a service of NASA HEASARC.
![the Fornax VST Survey is licensed under the `Creative Commons Attribution 4.0 License <http://creativecommons.org/licenses/by/4.0/>`_ .. image:: /static/img/ccby.png :alt: [CC-BY]](/registry-search/?f%5Brights_facet%5D%5B%5D=the+Fornax+VST+Survey+is+licensed+under+the+%60Creative+Commons+Attribution+4.0+License+%3Chttp%3A%2F%2Fcreativecommons.org%2Flicenses%2Fby%2F4.0%2F%3E%60_%0A%0A..+image%3A%3A+%2Fstatic%2Fimg%2Fccby.png%0A+++%3Aalt%3A+%5BCC-BY%5D%0A%0A&f%5Btype_facet%5D%5B%5D=Archive){kind=link}