ACDS V10.0 - Detailed Description of VII/175

ACDS V10.0 - Sat Jan 18 01:23:59 CET 2025

| # Detailed Description of VII/175 : Edinburgh-Durham Southern Galaxy Cat. - Cluster Cat. (Lumsden+ 1992) |

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.

    VII/175  Edinburgh-Durham Southern Galaxy Cat. - Cluster Cat. (Lumsden+ 1992)
    ================================================================================
    The Edinburgh-Durham southern galaxy catalogue -
    IV. The cluster catalog
         Lumsden S.L., Nichol R.C., Collins C.A., Guzzo L.
        <Mon. Not. R. Astron. Soc. 258, 1 (1992)>
        =1992MNRAS.258....1L
    ================================================================================
    ADC_Keywords: Clusters, galaxy

    Keywords: catalogues-galaxies: clustering

    Abstract:
       We present the Edinburgh-Durham Cluster Catalogue (EDCC). This is the
       first machine-based, objectively selected sample of clusters of
       galaxies. It consists of 737 clusters or groups of all richnesses,
       over 0.5 sr of sky, centred on the South Galactic Pole (SGP). The
       primary galaAy data set for the cluster survey is the
       Edinburgh-Durham Southern Galaxy Catalogue (EDSGC). The EDCC was
       constructed using an automatic peak-finding algorithm and is complete
       to m10(bj) = 18.75. In a comparison with the Abell clusters in
       the same region, we detect 80 per cent of their rich clusters
       nominally brighter than our completion limit in addition to many new
       systems. This suggests that the EDCC is 90 per cent complete for
       Abell-type clusters. We also conclude that the Abell magnitude system
       is biased towards bright magnitudes for most of their clusters, and
       that their richness estimates are prone to a larger uncertainty than
       they suggest. The EDCC therefore supersedes the Abell catalogue as a
       data base for statistical studies of cluster properties.

    See also:
        J/MNRAS/274/1071 : Edinburgh-Milano cluster redshift survey (Collins+ 1995)

    File Summary:

           FileName      Lrecl  Records   Explanations

    ×                   80        .   This file
    × ReadMe            80        .   this file
    × table3            92      737   the Edinburgh-Durham cluster catalogue

    Byte-by-byte Description of file:  table3

       Bytes Format  Units    Label    Explanations

       1-  5  I5     ---      EDCC     [1,769]+ sequential EDCC cluster
                                        identification number
           6  A1     ---      u_EDCC   [?] uncertainty flag on EDCC, indicating
                                        that such clusters could not be
                                        distinguished from the surrounding field
                                        (see paper, p6R)
       8-  9  I2     h        RAh      right ascension (hours)   (B1950)
      11- 12  I2     min      RAm      right ascension (minutes)
      14- 17  F4.1   s        RAs      right ascension (seconds)
          21  A1     ---      DE-      [-]! declination sign
      22- 23  I2     deg      DEd      declination (degrees)     (B1950)
      25- 26  I2     arcmin   DEm      declination (minutes)
      28- 31  F4.1   arcsec   DEs      declination (seconds)
      34- 38  F5.2   mag      M1       magnitude of first brightest member
      41- 45  F5.2   mag      M3       magnitude of third brightest member
      48- 52  F5.2   mag      M10      magnitude of tenth brightest member
          53  A1     ---      u_M10    [*] uncertainty flag of M10 where the visual
                                        inspection gave a clearly different result
                                        (see paper, p6R)
      55- 57  I3     ct       Nclus    [0,] number of galaxies within the Abell
                                        radius between M3 and M3+2 "after" the
                                        background galaxies have been removed
          58  A1     ---      u_Nclus  [*] uncertainty flag of Nclus (see u_M10)
      60- 62  I3     ct       Nback    [0,] number of background galaxies within
                                        the same radius to the same magnitude
                                        limit (see Nclus, and paper p6R)
      66- 70  F5.3   deg      THA      [0,] Abell radius
          74  A1     ---      F        [F]! character 'F' for field number
      75- 77  I3     ---      FIELD    [0,] Schmidt J survey field number
          80  I1     ct       RUN1     number of times the cluster was located in
                                        run 1 (see paper p2)
          81  I1     ct       RUN2     the above in run 2
          82  I1     ct       RUN3     the above in run 3
          85  A1     ---      DEB      [d] 'd'= the cluster was deblended, ' '= not
      87- 91  A5     ---      ACO      [0-9S ] Abell identification number (see
                                        paper p6R) (1)
          92  A1     ---      u_ACO    [:] only the clusters' Abell radii overlap (1)

    Note (1): ACO-identifications in the last column were aligned and
        brackets converted to a ':' sign AFTER the cluster number.
          --  H.A. 22-Oct-1992

    Historical notes:
       The catalogue was provided by courtesy of R.C.Nichol to H. Andernach;
       it was numbered A144 in H. Andernach's "List of Astronomical Catalogues
       and Documents kindly provided on request by various authors"
    References:

    References:
        The papers of this series are as follows:
          Paper I:    MNRAS 236, 7p (1988) "First results on the galaxy angular
                                            correlation function"
          Paper II:   MNRAS 238, 379 (1989) "Image classification and galaxy
                                            number counts"
          Paper III:  MNRAS 254, 295 (1992) "w(theta) from the full survey"
          Paper V:    MNRAS 255, 21p (1992) "The cluster correlation function"
          Paper VI:   MNRAS 265, 867 (1993) "The stability of w(theta)"
        The EDSGC is not yet published in these papers.
    ================================================================================
    (End)                                        Koichi Nakajima [CDS]   11-Mar-1994