ROS400GCLS - ROSAT PSPC 400 Square Degree Galaxy Cluster Catalog
This is a catalog of galaxy clusters detected in a new ROSAT PSPC
survey. The survey is optimized to sample, at high redshifts, the mass range
corresponding to T > 5 keV clusters at z = 0. Technically, our survey is the
extension of the 160 square degree survey (160d, the HEASARC Browse table
called ROSGALCLUS). The authors use the same detection algorithm, thus
preserving the high quality of the resulting sample; the main difference is
a significant increase in sky coverage. The new survey covers 397 square
degrees and is based on 1610 high Galactic latitude ROSAT PSPC pointings,
virtually all of the pointed ROSAT data that were suitable for the detection
of distant clusters. The search volume for X-ray luminous clusters within
z < 1 exceeds that of the entire local universe (z < 0.1). The authors
detected 287 extended X-ray sources with fluxes f_x > 1.4 x 10^-13 erg
s^-1 cm^-2 in the 0.5 - 2 keV energy band, of which 266 (93%) are optically
confirmed as galaxy clusters, groups or individual elliptical galaxies. The
paper from which this table is extracted provides a description of the input
data, the statistical calibration of the survey via Monte Carlo simulations,
and the catalog of detected clusters. The authors also therein compare the
basic results with those from previous, smaller area surveys and find good
agreement for the logN - log S distribution and the local X-ray luminosity
function. This sample clearly shows a decrease in the number density for
the most luminous clusters at z > 0.3. The comparison of these ROSAT-derived
fluxes with the accurate Chandra measurements for a subset of high-redshift
clusters demonstrates the validity of the 400 square degree survey's
This Browse table contains the main cluster catalog (Table 4 of the reference
paper) which comprises 242 serendipitously detected clusters of galaxies.
It does not include 24 clusters within a redshift of 0.01 of the redshift
of the target of the ROSAT observation (given in Table 5 of the reference
paper), as these latter are not entirely serendipitous, 5 noncluster extended
sources (given in Table 6 of the reference paper), nor 16 likely false X-ray
detections (given in Table 7 of the reference paper).
The 400 square degrees ROSAT PSPC galaxy cluster survey: Catalog and
Burenin R.A., Vikhlinin A., Hornstrup A., Ebeling H., Quintana H.,
<Astrophys. J. Suppl. 172, 561 (2007)>
This table was created by the HEASARC in December 2007 based on
the machine-readable version of Table 4 (the 'Cluster Catalog') obtained from
the electronic ApJ website.
A running X-ray source number in order of increasing J2000
The name of the X-ray source using the naming convention recommended
by the CDS Dictionary of Nomenclature of Celestial Objects for objects from
Table 4 of the reference paper, viz. '[BVH2007] NNN', in
which BVH2007 refers to Burenin, Vikhlinin, Hornstrup 2007, and NNN is the
X-ray source number.
The Right Ascension of the X-ray source centroid, in the selected
equinox. This was given in J2000.0 coordinates to a precision of 0.1 seconds
of time in the original reference. The typical positional uncertainty is
10 - 30 arcseconds.
The Declination of the X-ray source centroid, in the selected equinox.
This was given in J2000.0 coordinates to a precision of 1 arcsecond in the
original reference. The typical positional uncertainty is 10 - 30 arcseconds.
The Galactic Longitude of the X-ray source centroid.
The Galactic Latitude of the X-ray source centroid.
The total unabsorbed X-ray flux in the 0.5 - 2.0 keV band, in
The uncertainty in the total unabsorbed X-ray flux in the
0.5 - 2.0 keV band, in erg/s/cm^2.
The redshift of the cluster.
The reference code for the source of the cluster redshift.
If the redshift reference code is blank, the source for the redshift is
the authors' own measurement (A. Hornstrup 2007, in preparation). The key
to the reference codes is as follows:
1 = Vikhlinin et al. (1998a), Mullis et al. (2003);
2 = Cappi et al. (1998);
3 = Struble & Rood (1999);
4 = Mahdavi & Geller (2004);
5 = Rines et al. (2003);
6 = Simien & Prugniel (2000);
7 = Huchra et al..(1999);
8 = Perlman et al. (2002);
9 = Romer et al. (2000);
10 = Nesci & Altamore (1990);
11 = Abazajian et al. (2005);
12 = da Costa et al. (1998);
13 = Abell et al. (1989);
14 = de Vaucouleurs et al. (1991);
15 = Colless et al. (2001);
16 = Batuski et al. (1999);
17 = Stocke et al. (1991);
18 = Wegner et al. (2003);
19 = Mason et al. (2000);
20 = Peterson (1978);
21 = Molthagen et al. (1997);
22 = Bohringer et al. (2000);
23 = Miller et al. (2002);
24 = Appenzeller et al. (1998);
25 = Smith et al. (2000);
26 = Denicolo et al. (2005);
27 = Binggeli et al. (1985);
28 = Ebeling et al. (2001b);
29 = Burke et al. (2003);
30 = Bernardi et al. (2002);
31 = Binggeli et al. (1993);
32 = Falco et al. (1999);
33 = Hewitt & Burbidge (1991);
34 = Keel (1996);
35 = Huchra et al. (1990);
36 = Wegner et al. (1999);
37 = Miller et al. (2004);
38 = Owen et al. (1995);
39 = Kochanek et al. (2001);
40 = Gioia et al. (2003);
41 = da Costa et al. (1991);
42 Katgert et al. (1998).
The total X-ray luminosity in the 0.5 - 2.0 keV band, in erg/s. The
X-ray luminosity was computed as described in Appendix B of the reference
This field contains some additional notes on the optical
identifications of the clusters of galaxies, where VMF refers to a.
160d cluster (Vikhlinin et al. 1998a; Mullis et al. 2003),
A to an Abell cluster (Abell et al. 1989), and MS to the EMSS
(Stocke et al. 1991). A note of 'Section 4.1' means that there is
a discussion of the cluster in that section of the reference paper
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