VIII/50 VLA Survey of Rich Clusters of Galaxies (Slee+ 1996)
A VLA survey of rich clusters of galaxies. I. Whole-cluster maps, source list and statistics. Slee O.B., Perley R.A., Siegman B.C. <Aust. J. Phys. 42, 633 (1989)> =1989AuJPh..42..633S
A VLA Survey of Rich Clusters of Galaxies II. The Stronger Sources: Maps, Polarisations and Identifications Slee O.B., Roy A., Savage A. <Aust. J. Phys. 47, 145 (1994)> =1994AuJPh..47..145S A VLA Survey of Rich Clusters of Galaxies III. The Weaker Sources: Maps and Identifications Slee O.B., Roy A., Andernach H. <Aust. J. Phys. 49, 977 (1996)> =1996AuJPh..49..977S ADC_Keywords: Clusters, galaxy ; Radio sources Keywords: galaxies: clusters of - radio continuum: galaxies; surveys - radio sources: optical identification Description: We observed 60 fields towards 57 Abell and one Zwicky cluster of galaxies using the Very Large Array (VLA) with scaled arrays at 1.5 and 4.9 GHz. The source catalogue contains radio and optical parameters for 994 sources up to a lower flux limit of 1.0 mJy at 1.5 GHz and comprises a complete sample above 2.5 mJy. The combined sky area within the half-power circle on the maps is 3.5x10-3 sr, and the cluster fields are distributed between +35 deg and -30 deg declination. The source catalogue list positions, angular size, spectral index and optical identification, magnitude and morphology, if available. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file paper1.txt 62 937 Radio Sources Towards 58 Galaxy Clusters table1.dat 105 60 Properties of the observed clusters catalog.dat 108 1037 *Radio and optical parameters of sources
Note on catalog.dat: The source catalogues from papers II and III were merged, as well as the radio and the optical information joined into a single table. For each source only the most likely optical candidates (if any) were retained. This merged table replaces the one published in paper I (1989AuJPh..42..633S). Tables on structural details of multiple sources as published in papers II and III are available upon request to the authors.
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 7 A7 --- Field Name of observed field (1) 9 A1 --- n_Field [#*x ] Note on the field (2) 11- 12 I2 h RAh Right ascension (1950) of cluster centre (3) 14- 17 F4.1 min RAm Right ascension of cluster centre(1950) (3) 19 A1 --- DE- Declination sign 20- 21 I2 deg DEd Declination of cluster centre (1950) (3) 23- 24 I2 arcmin DEm Declination of cluster centre (1950) (3) 27- 30 F4.1 arcmin offRO Offset of radio field centre from optical cluster centre 33- 36 F4.2 --- offRcl Offset of radio field centre from optical cluster centre in units of cluster radii 38- 43 F6.1 deg offPA Position angle of vector from optical cluster centre to radio field centre (positive from N through E) 46- 48 I3 uJy rms_1.5 ? rms noise of radio map at 1.5 GHz (/beam) 50- 52 I3 uJy rms_4.9 ? rms noise of radio map at 4.9 GHz (/beam) 55 I1 --- Rclass Abell richness class of cluster 57 I1 --- Dclass Abell distance class of cluster 59- 62 F4.1 mag m10R red magnitude of 10th brightest galaxy 64- 69 A6 --- BMclass Bautz-Morgan (BM) class of cluster 70 A1 --- u_BMclass [ :] uncertainty flag on BM class 72- 73 A2 arcmin Rclu angular cluster radius (4) 76- 79 F4.2 Mpc Rclin linear cluster radius (H0=75km/s/Mpc) 82- 87 F6.4 --- zclu cluster redshift 90 A1 --- r_zclu reference for cluster redshift (5) 93- 97 F5.2 [10-7W] lgxein ? log of EINSTEIN X-ray luminosity (6) 99 A1 --- n_lgxein [ R] R= ROSAT measurement converted to EINSTEIN luminosity scale (see paper) 101-105 F5.2 [10-7W] lgxros ? log of ROSAT X-ray luminosity from Ebeling 1993 (PhD MPE Garching)
Note (1): 'A' stands for 'Abell cluster' and Z1518.8 stands for the Zwicky cluster Zw1518.8+0747. Two clusters (A 85 and A154) were observed with two different field centers. Note (2): *= The RA is from Abell et al. (1989). The incorrect RA of Abell (1958) was used for the radio field centre - hence the large offset. #= Data from Abell et al. (1989) =1989ApJS...70....1A x= Data from "Catalogue of Galaxies and of Clusters of Galaxies" (Zwicky et al. 1961) and Slee & Quinn (1979) =1979PASAu...3..332S Note (3): The centroid position (B1950) of the optical cluster, mainly from Abell (1958) (=1958ApJS....3..211A), but data for three clusters come from Abell et al. (1989) (=1989ApJS...70....1A) and Zwicky et al. (1961). Note (4): Rclu is the cluster radius from the Palomar Sky Survey (Struble & Rood 1987 =1987ApJS...63..555S) except that the Abell radius (approximately 1.72/z arcmin) is quoted for A3528, Zw1518.8, A4038. Note (5): Redshift references : 1 Struble & Rood =1991ApJS...77..363S 2 From the m10-z relation =1994AuJPh..47..145S (Slee, Roy & Savage SRS94, Paper II) 3 Melnick & Quintana =1981A&AS...44...87M 4 Abell et al. =1989ApJS...70....1A 5 Beers et al. =1991AJ....102.1581B 6 Slee & Reynolds =1984PASAu...5..516S 7 Reynolds 1986 =1986USydn.T00J....R 8 Postman et al. =1992ApJ...384..404P Note (6): The EINSTEIN X-ray luminosity in the energy range 0.5-4.5 keV and out to a radius of 1Mpc from the cluster centre. The data (scaled to Ho=75 km/s/Mpc) are from Jones & Forman (1995, unpublished).
Byte-by-byte Description of file: catalog.dat
Bytes Format Units Label Explanations
1- 14 A14 --- Name Name of cluster (A=Abell, Z=Zwicky) (1) 16 A1 --- multID [ #] # denotes one of several optical identifications for the same source 17 A1 --- IDnum Sequence number of optical ID 20- 21 I2 h RAh Right ascension of radio centroid (1950) 22- 23 I2 min RAm Right ascension of radio centroid (1950) 24- 28 F5.2 s RAs Right ascension of radio centroid (1950) 30 A1 --- DE- Declination sign 31- 32 I2 deg DEd Declination of radio centroid (1950) 33- 34 I2 arcmin DEm Declination of radio centroid (1950) 35- 38 F4.1 arcsec DEs Declination of radio centroid (1950) 40- 41 A2 --- paper [23 ] number of paper in which the source was published ('2 '=II; ' 3'=III; '23'=both) 43- 46 F4.2 --- offRcl projected distance of radio source from cluster center in units of Rc (see table1) 48- 53 F6.1 mJy F1.5 ? integrated 1.5GHz flux density 55- 59 F5.1 mJy F4.9 ? integrated 4.9GHz flux density 61- 64 F4.1 --- alpha ? spectral index between 1.5 and 4.9 GHz (2) 67- 69 I3 arcsec majax ? size of source major axis (deconvolved) (3) 71- 72 I2 arcsec minax ? size of source minor axis (deconvolved) (3) 74- 76 I3 deg PosAng ? position angle of major axis (N thru E) 78- 81 A4 --- omorph optical morphology of most likely ID (4) 82 A1 --- l_Rmag [ >] upper limit flag for Rmag (4) 83- 86 F4.1 mag Rmag ? red magnitude from POSS prints (4) 88- 91 F4.1 mag Jmag ? blue (B_j) magnitude from SERC plates (4) 94- 95 I2 arcsec offRO ? Positional offset of opt. ID with respect to radio centroid 97-100 I4 deg offPA ? Position angle of vector pointing from radio centroid to opt. ID (positive N through E) 103-108 F6.4 --- z ? heliocentric redshift of opt. ID, if available (references see paper)
Note (1): The source name is composed of the name of cluster (A=Abell, Z=Zwicky, in A5 format), an underscore symbol, the source running number within the observed field (optionally appended by a roman numeral), and an optional list of subcomponents (a, ab, abc...) which indicate the presence of more detailed structural data in tables 3 and 4 of both papers II and III. Note that Z1518 stands for the Zwicky cluster Zw1518.8+0747. The source running numbers are those of paper I. However, a few of the weak sources listed in Paper I (e.g. A0133_10) were omitted because subsequent analysis showed that they were probably spurious. To avoid later confusion, the additional sources are inserted in the Table at the correct right ascension but are given an extra lower case Roman numeral. For example, the source A0013_13 in table 2 of paper I is now A0013_13i, while the source A001313iiab of slightly later RA (as well as two components a and b) has been inserted in the present source list. In one case two sources (A1913_6 and A1913_8) were merged to a single source (A1913_6,8). Note (2): The spectrum is defined as F(freq)∼freqalpha. The spectral index is between 1.5 and 4.9 GHz. When no 4.9 GHz flux is listed in the table, the spectral index is between 1.5 GHz and another frequency taken from references quoted in the printed version of the papers. Note (3): An elliptical Gaussian was fitted to the source. The quoted values are the full widths at half power, deconvolved with the antenna beam, and corrected for bandwidth smearing. Note (4): The optical identifications were classified into the following categories: E = elliptical galaxy (ie. visibly extended, surrounded by a diffuse structureless halo with axial ratio ≲2 D = elliptical galaxy several times larger than all neighbouring galaxies if well away from cluster centre cD = same as D if close to the cluster centre DB = two barely resolved elliptical galaxies (dumb-bell galaxy) G = galaxy (diffuse image too faint to assign a galaxy class) Q = quasar known from literature S0 = as 'E' above but with an axial ratio ≳2 Sp = spiral galaxy (galaxy with considerable structure in the halo) St = image with a sharp circular boundary and sometimes showing diffraction spikes The symbol 'x2' is appended to double objects, for which the summed magnitude is quoted in the subsequent columns. Very faint images are difficult to assign to the G or St categories and often the choice is rather arbitrary. If an image was detected on the Bj plates, but not on the red POSS prints a conservative upper limit of ">19.5" is quoted for the red magnitude.
(End) Heinz Andernach [IUE Vilspa] 23-Oct-1996
|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|