J/A+AS/74/315 327 MHz Survey of the A262 cluster region (Righetti+, 1988)
Survey at 327 MHz of the A 262 cluster region. Righetti G., Giovannini G., Feretti L. <Astron. Astrophys. Suppl. Ser. 74, 315 (1988)> =1988A&AS...74..315R (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Galaxies, radio Keywords: radio sources: general - radio continnum - surveys Description: 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. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file rad_a262.dat 89 309 327 MHz Survey of Abell 262
See also: Byte-by-byte Description of file: rad_a262.dat Byte-by-byte Description of file: rad_a262.dat
Bytes Format Units Label Explanations
1- 7 A7 --- Name Name of source (1) 8- 9 I2 h RAh Right Ascension (B1950) (hour) (2) 10- 11 I2 min RAm Right Ascension (B1950) (min) 12- 15 F4.1 s RAs Right Ascension (B1950) (sec) 16 A1 --- DE- Declination sign (B1950) (2) 17- 18 I2 deg DEd Declination (B1950) (deg) 19- 20 I2 arcmin DEm Declination (B1950) (arcmin) 21- 22 I2 arcsec DEs Declination (B1950) (arcsec) 25- 28 F4.2 deg r Distance from pointing center (3) 31- 34 I4 mJy Smap Flux density measured on map (4) 37- 40 I4 mJy Ssky Flux density corrected for attenuation (4) 44- 46 I3 arcsec tt ? Angular (DECONVOLVED or SKY) extent (5) 50- 52 I3 deg pa ? Position angle N to E of major axis (5) 54- 56 A3 --- ID Optical identification (6) 59- 62 F4.1 arcsec oRA ? RA difference radio minus optical position (7) 64- 68 F5.1 arcsec oDE ? Dec Difference radio minus optical position (7) 70- 89 A20 --- Notes Notes (8)
Note (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'. Note (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. Note (3): This column contains the distance from the pointing center, in degrees. This value is used to obtain the correction for primary beam attenuation. Note (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. Note (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. Note (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). Note (7): These columns give the 'radio minus optical' positional difference between the radio and optical positions (RA and Dec, respectively), in arcsec. Note (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.
References: Oort, M. J. A. 1987, Phd Thesis, Leiden. History: "The catalogue was originally archived as A006 by H. Andernach () and the ADS documentation prepared in collaboration with Carolyn Stern Grant ()."
(End) Patricio Ortiz [CDS] 30-Mar-1999
(End) Patricio Ortiz [CDS] 30-Mar-1999
|The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line|