ACDS V10.0 - Detailed Description of J/MNRAS/301/881

ACDS V10.0 - Tue Dec 17 23:06:14 CET 2024

| # 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
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    (End)                                   Francois Ochsenbein [CDS]    28-Jun-2000