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Detailed Description of J/MNRAS/289/263 :
Galaxy clusters from the APM galaxy survey (Dalton+ 1997)

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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/289/263     Galaxy clusters from the APM galaxy survey  (Dalton+ 1997)
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The APM galaxy survey - V. Catalogues of galaxy clusters.
       Dalton G.B., Maddox S.J., Sutherland W.J., Efstahiou G.
      <Mon. Not. R. Astron. Soc. 289, 263 (1997)>
      =1997MNRAS.289..263D      (SIMBAD/NED BibCode)
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ADC_Keywords: Clusters, galaxy

Keywords: catalogues - surveys - galaxies: clusters: general -
          large-scale structure of the Universe

Abstract:
    We describe the construction of catalogues of galaxy clusters from the
    APM Galaxy survey using an automated algorithm based on Abell-like
    selection criteria. We investigate the effects of varying several
    parameters in our selection algorithm, including the magnitude range
    and radius from the cluster centre used to estimate the cluster
    richnesses. We quantify the accuracy of the photometric distance
    estimates by comparing them with measured redshifts, and we
    investigate the stability and completeness of the resulting
    catalogues. We find that the angular correlation functions for
    different cluster catalogues are in good agreement with one another,
    and are also consistent with the observed amplitude of the spatial
    correlation function of rich clusters.

File Summary:

FileName Lrecl Records Explanations
× 80 . This file × ReadMe 80 . This file × catalog 57 957 The APM cluster catalogue
See also: J/MNRAS/278/1025 : The APM Bright Galaxy Catalogue (Loveday 1996) J/MNRAS/246/433 : APM galaxy survey. II. (Maddox+ 1990) J/MNRAS/269/151 : APM galaxy survey. IV. (Dalton+, 1994) J/MNRAS/274/1071 : Edinburgh-Milano cluster redshift survey (Collins+ 1995) VII/203 : Las Campanas Redshift Survey (Shectman+ 1996) Byte-by-byte Description of file: catalog
Bytes Format Units Label Explanations
1- 3 I3 --- Cluster Cluster number 5- 6 I2 h RAh Right ascension (1950) 7- 8 I2 min RAm Right ascension (1950) 9- 12 F4.1 s RAs Right ascension (1950) 14 A1 --- DE- Declination sign 15- 16 I2 deg DEd Declination (1950) 17- 18 I2 arcmin DEm Declination (1950) 19- 20 I2 arcsec DEs Declination (1950) 22- 26 F5.2 mag Xmag X magnitude (1) 28- 31 F4.1 arcmin rC Projected radius 33- 37 F5.3 --- z Estimated redshift determined from Xmag 39- 43 F5.1 --- R Cluster richness 44 A1 --- n_R [abc] Notes (2) 46- 50 F5.3 --- zabs ? Absorption redshift 52- 56 A5 --- n_zabs [12345+, ] Notes (3)
Note (1): We define Xmag to be the magnitude for which Ci=X, i.e. in the case of X=10 with no weighting then Xmag is exactly equivalent to Abell's m10. (Ci is the weighted sum of galaxies brighter than mi minus the expected background count brighter than mi.) Note (2): a: This cluster is close to a bright star which has been excised from the galaxy catalogue. A part of the cluster area is therefore missing from the survey data and so the richness may have been underestimated. b: The field of this cluster includes a 2-arcmin foreground galaxy 0.7rC from the centre which has been broken up into several small galaxian images by the APM software. These additional objects may have caused the richness to be slightly overestimated. c: This field is dominated by a 2-arcmin foreground galaxy which has been broken up into several small galaxian images by the APM software. The field does not appear to contain a true cluster. The cluster was below the richness threshold used by Dalton et al. (1994MNRAS.271L..47D) and was not visually inspected at the time of those observations. Note (3): 1: Redshift from Paper IV, Dalton et al., 1994, Cat. J/MNRAS/269/151 2: Redshift measured by Dalton et al. (1994MNRAS.271L..47D). Note that this survey was limited to Xmag <=19.2 3: Redshift measured as part of the deep extension to the APM cluster redshift survey (Croft et al., 1997, MNRAS, in press) 4: Cluster found in the Edinburgh-Milano Cluster Redshift Surcey (Collins et al., 1995, Cat. J/MNRAS/274/1071). If only one references is present then the redshift is adopted from this source, otherwise this entry indicates that the cluster is also found in that survey. 5: Cluster redshift has been drawn from Las Campanas Redshifdt Survey (LCRS: Schectman et al., 1996ApJ...470..172S. Cat. VII/203) +: For the cluster APM 100, we have adopted the value given by Collins et al. (1995, Cat. J/MNRAS/274/1071) as they point out this is in better agreement with the maximum likelihood redshift estimate quoted in Paper IV (Cat. J/MNRAS/269/151) than our single galaxy redshift.
Acknowledgements: Gavin Dalton g.dalton1@physics.ox.ac.uk References: Maddox et al., Paper I. 1990MNRAS.243..692M Maddox et al., Paper II. 1990MNRAS.246..433M, Cat. J/MNRAS/246/433 Maddox et al., Paper III. 1996MNRAS.283.1227M Dalton et al., Paper IV. 1994MNRAS.269..151D, Cat. J/MNRAS/269/151 ================================================================================ (End) Patricia Bauer [CDS] 10-Oct-1997