J/A+AS/74/315 J/A+AS/74/315 327 MHz Survey of the A262 cluster region G Righetti G Giovannini L Feretti Astron. Astrophys. Suppl. Ser. 74 315 1988 1988A&AS...74..315R Clusters, galaxy Galaxies, radio radio continuum: general radio sources: general surveys This catalog contains a survey at 327 MHz of the A262 cluster region. The survey was performed with the WSRT Telescope in the redundancy mode, and covers a circular region of 21 square degrees towards A262 (RA = 01h49m50s, decl = 35d54'20" -- B1950). The synthesized beam width is 56" x 93" (RA x DEC). 309 sources were detected, with a detection limit of 7 mJy (~5 sigma) at the field center. Nine of these galaxies have been identified with galaxies of the A262 cluster.

Name Name of source number=1 This column contains the name of the source, consisting of the Westerbork survey number (73W) followed by a sequence number in order of right ascension. Source '73W076' is a double and both components are listed separately; '73W076a' and '73W076b'. --- RAh Right Ascension (B1950) (hour) number=2 These columns contain the B1950 source position. The positional accuracy depends on the source strength and size; it is estimated to be ~4" in right ascension and ~7" in declination for the weakest point sources, and becomes 2.4" and 4" respectively, for the sources with flux density > 14 mJy. h RAm Right Ascension (B1950) (min) min RAs Right Ascension (B1950) (sec) s DE- Declination sign (B1950) number=2 These columns contain the B1950 source position. The positional accuracy depends on the source strength and size; it is estimated to be ~4" in right ascension and ~7" in declination for the weakest point sources, and becomes 2.4" and 4" respectively, for the sources with flux density > 14 mJy. --- DEd Declination (B1950) (deg) deg DEm Declination (B1950) (arcmin) arcmin DEs Declination (B1950) (arcsec) arcsec r Distance from pointing center number=3 This column contains the distance from the pointing center, in degrees. This value is used to obtain the correction for primary beam attenuation. deg Smap Flux density measured on map number=4 The Smap column contains the source flux density, as measured on the map (in mJy). The Ssky column contains the source flux density corrected for the primary beam attenuation. The attenuation factor is calculated as f(r) = cos^-6^ * (21.154 * r) (ref. Oort, 1987), where 'r' is the distance from the pointing center, given above. mJy Ssky Flux density corrected for attenuation number=4 The Smap column contains the source flux density, as measured on the map (in mJy). The Ssky column contains the source flux density corrected for the primary beam attenuation. The attenuation factor is calculated as f(r) = cos^-6^ * (21.154 * r) (ref. Oort, 1987), where 'r' is the distance from the pointing center, given above. mJy tt Angular (DECONVOLVED or SKY) extent number=5 These columns give the angular extent, in arcsec (deconvolved), and the position angle, N to E, in degrees of the major axis of the radio brightness. arcsec pa Position angle N to E of major axis number=5 These columns give the angular extent, in arcsec (deconvolved), and the position angle, N to E, in degrees of the major axis of the radio brightness. deg ID Optical identification number=6 This column gives the optical identification of the source as follows: BO: Blue stellar object QSO: Quasar R: Red stellar object GAL: Galaxy EF: Empty field There are 227 empty fields, corresponding to 74% of the sample. The identification rate is independent of the flux density. Identifications are accepted when the positions agree to within 3 sigma (see text (1988A&AS...74..315R) for definition of sigma). --- oRA RA difference radio minus optical position number=7 These columns give the 'radio minus optical' positional difference between the radio and optical positions (RA and Dec, respectively), in arcsec. arcsec oDE Dec Difference radio minus optical position number=7 These columns give the 'radio minus optical' positional difference between the radio and optical positions (RA and Dec, respectively), in arcsec. arcsec Notes Notes number=8 This column marks notes on the optical identification. Due to the large uncertainty on the radio positions, a high contamination from chance coincidences is expected. For this reason, identifications with coincidence less than 2 sigma are differentiated from those between 2 and 3 sigma. The latter, which should be considered less reliable, are marked with an asterisk in this column. Where available, the name of the cluster galaxies is also given. --- Patricio Ortiz CDS 1999Mar30 UNKNOWN UNKNOWN "The catalogue was originally archived as A006 by H. Andernach (heinz@astro.ugto.mx) and the ADS documentation prepared in collaboration with Carolyn Stern Grant (stern@cfa.harvard.edu)." J_A+AS_74_315.xml