/ftp/cats/vii/211



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VII/211   ==OBSOLETE version of Catalogue==
07-Mar-2002: (by Francois Ochsenbein) See VII/227
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=VII/211
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drwxr-xr-x 257 cats archive 8192 Feb 8 10:28 [Up] drwxr-xr-x 2 cats archive 242 May 26 2023 [TAR file] -rw-r--r-- 1 cats archive 394 Dec 19 2022 .message -rw-r--r-- 1 cats archive 50 Mar 7 2002 =obsolete= -r--r--r-- 1 cats archive 8050 Feb 11 2000 ReadMe -r--r--r-- 1 cats archive 4756 Feb 11 2000 snrs.dat.gz [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe : VII/211 A Catalogue of Galactic Supernova Remnants (Green 1998) ================================================================================ A Catalogue of Galactic Supernova Remnants, 1998 September version Green D.A. <Mullard Radio Astronomy Observatory, Cambridge, United Kingdom (1998)> ================================================================================ ADC_Keywords: Supernova remnants ; Milky Way ; Nonstellar objects Abstract: This catalogue of known Galactic supernova remnants (SNRs) is an updated version of the catalogues of Galactic SNRs presented in detail in Green (1984, 1988), in summary form in Green (1991, 1996), and on the World-Wide-Web (versions of July 1995 and August 1996). (Note that version published in Green (1996) was produced in 1993.) This September 1998 version of the catalogue contains 220 SNRs, which is 5 more than listed in the previous version. The basic summary data included in this catalogue for each SNR are its Galactic coordinates, RA and Dec (B1950.0), angular size (in arcmin), type, flux density at 1 GHz, spectral index, and any other names. Notes on these parameters, on possible remnants not included, and questionable SNRs listed in the catalogue are given in full version of the catalogue on the World-Wide-Web. It should be noted that there are serious selection effects which apply to the identification of Galactic SNRs (see Green 1991), so that great care should be taken if these data are used in statistical studies.