ACDS V10.0 - Tue Apr 23 01:12:34 CEST 2019
 |
Detailed Description of J/MNRAS/301/881 : The ROSAT brightest cluster sample - I. (Ebeling+, 1998)
|
 |
Note : this is the description file of the original catalog.
This HTML page corresponds well to the original description, but some minor
changes in the format may have been introduced in the FITS output
files in order to allow for arithmetic operations on quantities
such as coordinates and times. h:m:s and d:m:s units are normally
converted into degrees, and YYYY-MM-DD into julian days.
Similarly, some slight changes may have been introduced in the
units; the value given in the HTML files supersedes the value indicated in the ReadMe
file for this catalogue.
J/MNRAS/301/881 The ROSAT brightest cluster sample - I. (Ebeling+, 1998)
================================================================================
The ROSAT brightest cluster sample - I.
The compilation of the sample and the cluster log N-log S distribution.
Ebeling H., Edge A.C., Boehringer H., Allen S.W., Crawford C.S.,
Fabian A.C., Voges W., Huchra J.P.
<Mon. Not. R. Astron. Soc. 301, 881 (1998)>
=1998MNRAS.301..881E
================================================================================
ADC_Keywords: Clusters, galaxy ; X-ray sources ; Surveys
Mission_Name: ROSAT
Keywords: catalogues - surveys - galaxies: clusters: general -
cosmology: observations - large-scale structure of Universe -
X-rays: galaxies
Abstract:
We present a 90 per cent flux-complete sample of the 201
X-ray-brightest clusters of galaxies in the northern hemisphere
({delta}>=0°), at high Galactic latitudes (|b|>= 20°), with
measured redshifts z<=0.3 and fluxes higher than
4.4x10-12erg/cm2/s in the 0.112.4 keV band. The sample, called the
ROSAT Brightest Cluster Sample (BCS), is selected from ROSAT All-Sky
Survey data and is the largest X-ray-selected cluster sample compiled
to date. In addition to Abell clusters, which form the bulk of the
sample, the BCS also contains the X-ray-brightest Zwicky clusters and
other clusters selected from their X-ray properties alone. Effort has
been made to ensure the highest possible completeness of the sample
and the smallest possible contamination by non-cluster X-ray sources.
X-ray fluxes are computed using an algorithm tailored for the
detection and characterization of X-ray emission from galaxy clusters.
These fluxes are accurate to better than 15 per cent (mean 1{sigma}
error).
File Summary:
FileName Lrecl Records Explanations
× 80 . This file
× ReadMe 80 . This file
× table3.dat 119 206 The ROSAT Brightest Cluster Sample
× refs.dat 73 47 References
See also:
IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1999)
J/ApJ/502/558 : Catalog of ROSAT galaxy clusters (Vikhlinin+ 1998)
J/ApJ/514/148 : ROSAT survey of bright galaxies clusters (De Grandi+, 1999)
J/MNRAS/306/857 : ROSAT Brightest Cluster Sample. III. (Crawford+, 1999)
J/MNRAS/318/333 : Extended ROSAT Bright Cluster Sample (Ebeling+ 2000)
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 4 A4 --- n_Name Note on Name (1)
6- 20 A15 --- Name Cluster name (2)
22- 23 I2 h RAh Right ascension (B1950)
25- 26 I2 min RAm Right ascension (B1950)
28- 31 F4.1 s RAs Right ascension (B1950)
33 A1 --- DE- Declination sign (B1950)
34- 35 I2 deg DEd Declination (B1950)
37- 38 I2 arcmin DEm Declination (B1950)
40- 41 I2 arcsec DEs Declination (B1950)
43- 49 F7.3 deg RAdeg X-ray right ascension (J2000)
51- 57 F7.3 deg DEdeg X-ray declination (J2000)
59- 62 F4.1 10+20cm-2 NH Hydrogen column density from
Stark et al. (1992, Cat. J/ApJS/79/77)
64- 67 I4 s Texp RASS exposition time
69- 73 F5.2 ct/s CR(VTP) PSPC count rate in PHA (Pulse Height Analyser)
channels 11 to 235 originally detected by VTP
(Voronoi tesselation and percolation)
75- 78 F4.1 arcmin R(VTP) Equivalent radius of the source detected by
VTP (Voronoi tesselation and percolation)
80- 85 F6.2 ct/s CR Final PSCP count rate (3)
87- 91 F5.2 ct/s e_CR rms uncertainty on CR (4)
93- 96 F4.1 keV kT Intra-cluster medium gas temperature used in
conversion from count rates to energy fluxes
97 A1 --- n_kT [e] e: temperature estimated
99-103 F5.4 --- z Redshift
105-109 F5.1 10-15W/m2 FX Unabsorbed X-ray energy flux in the
0.1-2.4keV band (10-12erg/cm2/s)
111-116 F6.2 10+37W LX Intrinsic X-ray luminosity in 0.1-2.4keV band
118-119 I2 --- r_z Redshift reference in refs.dat file
Note (1): Flags:
V = extended according to VTP, Voronoi tesselation and percolation
S = extended according to SASS, Standard Analysis Sofware System
(Vosges et al., 1992, Proc. Satellite Symp. 3, ESA ISY-3, p. 223)
c = likely contamination from point sources
+ = serendipitous VTP detection
* = redshift z>0.3
Note (2): Where clusters appear to consist of two components,
two entries ('a' and 'b') are listed.
Note (3): Final PSC count rate in PHA channels 11 to 235 based on the original
VTP count rate. Statistical corrections for low-surface brightness
emission that has not been detected directly and for contamination
from point sources have been applied.
Note (4): Error in the final PSPC count rate according to equation
{Delta}CR/CR=2.29(CR*Texp)-0.48.
The fractional uncertainty in the energy flux and the X-ray luminosity
can be assumed to be the same as the fractional count rate error.
Byte-by-byte Description of file: refs.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Ref Reference number
4- 22 A19 --- BibCode BibCode
24- 49 A26 --- Aut Author's name
51- 73 A23 --- Com Comments
History:
Provided by H. Andernach, A489 in his list
================================================================================
(End) Francois Ochsenbein [CDS] 28-Jun-2000