The Giant Metrewave Radio Telescope (GMRT) was used to survey the radio sky at 150 MHz between 2010 and 2012. To date, the data collected by the TIFR GMRT Sky Survey (TGSS) project team remained largely unpublished within the scope of that project. We independently reprocessed the TGSS data using the SPAM pipeline, which includes corrections for direction-dependent ionospheric phase effects. Our first alternative data release (ADR1) includes continuum stokes I images of 99.5 percent of the radio sky north of -53° DEC (3.6π sr, or 90 percent of the full sky) at a resolution of 25“ x 25” north of 19° DEC and 25“ x 25” / cos(DEC-19°) south of 19°, and a median noise of 3.5 mJy/beam. The extracted radio source catalog contains positions, flux densities, sizes and more for 0.62 Million sources down to a 7-sigma peak-to-noise threshold. The data processing and products are described in detail in Intema et al. (2017).
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The TGSS ADR survey products are hosted by the ASTRON virtual observatory (VO) system. This system complies with the VO standard and can be accessed directly by tools like TOPCAT. The VO system provides three services, for which web-based interfaces are available:
The VO service links are given here:
The 5×5 square degree mosaic images that form the basis of TGSS ADR1 are available for direct download here (5336 FITS images; 32 MB each). Note that there is a factor 3.6(!) redundancy in the sky coverage, mainly to guarantee up to 1×1 square degree cutouts anywhere in the survey area.
A conversion table between pointing/mosaic names (RxxDxx) and center RA,DEC (deg) is provided here (Starbase format)
The TGSS ADR1 source catalog is available for direct download in various formats (right click link for download):
A description of the table columns is given in the TGSS ADR survey paper. Not all table formats have the units stored in the header. The units are (epoch J2000):
A NOTE OF CAUTION: The source extraction and catalog merging is a very complex operation. Certain choices were made that have an impact on the characteristics of the final catalog. A source catalog can be used to quickly make selections based on the average properties of sources, but may not give the desired answer for individual sources. Especially for (strongly) resolved sources, it is advised to inspect the image(s). The interactive tools presented below are a convenient way to do that, but there are also other options (DS9, TOPCAT, etc.).
EXPERIMENTAL: VO access is also possible through python PyVO (although we have little experience with this, so comments are welcome!):
import pyvo as vo url = 'http://vo.astron.nl/tgssadr/q/cone/scs.xml' t = vo.conesearch( url, pos = vo.object2pos( 'NGC 5939' ), radius = 30.0 ) print t.votable
The TGSS ADR survey images and catalog are available as a Hierarchical Progressive Survey (HiPS), which allows you to efficiently inspect the whole survey area interactively. With powerful tools such as Aladin you can quickly search for your favorite object(s), and combine TGSS ADR images with many other astronomy (survey) images and catalogs, either available online through CDS and other resources or from your local disk. Here are three ways to use Aladin to access the TGSS ADR HiPS.
For options 2 and 3, make sure you have java installed and enabled.
For option 3, use menu File→Open URL and enter the following links:
Note: When using the Aladin Desktop tool, it keeps a local cache (under $HOME/.aladin/Cache). Ocaisionally we will make changes to the HiPS images or catalog, which we will announce in the news section and on Facebook. For this to work, the local Aladin cache needs to be cleared (deleted). As far as we know, this can only be done by deleting the contents of the cache directory.
Created by Alex Mechev and Josh Albert (Leiden).
You can use the TGSS ADR source catalog for generating a BBS-compatible Global Sky Model to calibrate your LOFAR data. Either fill out the form below, or run something like
wget -O GSM.txt 'http://tgssadr.strw.leidenuniv.nl/cgi-bin/gsmv3.cgi?coord=3c323&radius=3&unit=deg&deconv=y&cutoff=0.3'
This figure is a Mollweide projection in equatorial coordinates showing the sky coverage and the distribution of the background RMS noise for the TGSS ADR1. The median RMS noise is 3.5 mJy/beam. The noise is higher in the Galactic plane, at low declinations (due to lower elevation angles of the telescopes), and around bright radio sources at this frequency such as Cas A, Cen A, and Cyg A.
This plot shows the superiority of TGSS ADR in terms of the angular resolution and RMS sensitivity with respect to other wide-field surveys at similar frequencies. Wide-field centimeter wavelength surveys are also shown for comparison. Red symbols indicate meter wavelength surveys (<300 MHz), while blue and green symbols are existing and planned centimeter surveys (>300 MHz), respectively. Lines of constant surface brightness are shown in gray for a surface brightness sensitivity calculated as a function of resolution for 3 x RMS noise.
We are very interested in receiving feedback from users of the TGSS ADR survey products. We aim to improve the quality of the survey products where needed, but will need your help with that. So please report any problems that you find. We're also interested to hear about positive experiences and cool science that was enabled by using the TGSS ADR survey products.
If you are using the TGSS ADR survey products for your research, that's great! Please acknowledge our service to the astronomical community by adding this reference (Intema et al. 2017, A&A, 598, A78) in your publication.
Please also add the standard GMRT acknowledgement: We thank the staff of the GMRT that made these observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research.
If you use one of the Aladin tools to access TGSS ADR for your research, please refer to these papers (2000A&AS..143...33B and 2014ASPC..485..277B) and add this acknowledgement: This research has made use of “Aladin sky atlas” developed at CDS, Strasbourg Observatory, France.
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