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 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 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 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:
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FileName Lrecl Records Explanations
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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
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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 1989AuJPh..42..633S). Tables on structural details of multiple
sources as published in papers II and III are available upon request
to the authors.
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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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)
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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 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 1979PASAu...3..332S
Note (3):
The centroid position (B1950) of the optical cluster, mainly from
Abell (1958) (=1958ApJS....3..211A 1958ApJS....3..211A), but data for three clusters come
from Abell et al. (1989) (=1989ApJS...70....1A 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 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 1991ApJS...77..363S
2 From the m10-z relation =1994AuJPh..47..145S 1994AuJPh..47..145S
(Slee, Roy & Savage SRS94, Paper II)
3 Melnick & Quintana =1981A&AS...44...87M 1981A&AS...44...87M
4 Abell et al. =1989ApJS...70....1A 1989ApJS...70....1A
5 Beers et al. =1991AJ....102.1581B 1991AJ....102.1581B
6 Slee & Reynolds =1984PASAu...5..516S 1984PASAu...5..516S
7 Reynolds 1986 =1986USydn.T00J....R 1986USydn.T00J....R
8 Postman et al. =1992ApJ...384..404P 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).
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Byte-by-byte Description of file: catalog.dat
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Bytes Format Units Label Explanations
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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)
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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.
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(End) Heinz Andernach [IUE Vilspa] 23-Oct-1996