Access to Astronomical Catalogues

J/MNRAS/366/645     LARCS. 11 X-ray luminous clusters     (Pimbblet+, 2006)
The Las Campanas/Anglo-Australian Telescope Rich Cluster Survey -
III. Spectroscopic studies of X-ray bright galaxy clusters at z∼0.1.
    Pimbblet K.A., Smail I., Edge A.C., O'hely E., Couch W.J., Zabludoff A.I.
   <Mon. Not. R. Astron. Soc., 366, 645-666 (2006)>
   =2006MNRAS.366..645P    (SIMBAD/NED BibCode)
ADC_Keywords: Surveys ; Clusters, galaxy ; X-ray sources ; Photometry, CCD

Keywords: catalogues - surveys - galaxies: clusters: general -
          galaxies: evolution - cosmology: observations

Abstract:
    We present the analysis of the spectroscopic and photometric
    catalogues of 11 X-ray luminous clusters at 0.07<z<0.16 from the Las
    Campanas/Anglo-Australian Telescope Rich Cluster Survey. Our
    spectroscopic data set consists of over 1600 galaxy cluster members,
    of which two-thirds are outside r200. These spectra allow us to assign
    cluster membership using a detailed mass model and expand on our
    previous work on the cluster colourmagnitude relation (CMR) where
    membership was inferred statistically.

Description:
    High-quality broad-band B- and R-band CCD images of our clusters have
    been secured at LCO using the 1-m Swope Telescope. More details of the
    observations, reduction and analysis of these data are given in
    Pimbblet et al. (2001, Cat. J/MNRAS/327/588).
Objects:
    ----------------------------------------------------------
       RA   (2000)   DE      Cluster designation(s)
    ----------------------------------------------------------
    00 20 34.8   -25 41 51   a22   = ACO 22
    10 44 37.0   -07 04 48   a1084 = ACO 1084
    12 00 24.5   +03 19 52   a1437 = ACO 1437
    12 58 41.1   -01 45 25   a1650 = ACO 1650
    12 59 22.9   -04 11 10   a1651 = ACO 1651
    13 03 41.0   -24 13 06   a1664 = ACO 1664
    15 18 46.0   +06 12 06   a2055 = ACO 2055
    15 40 06.0   -03 17 42   a2104 = ACO 2104
    16 32 45.0   +05 34 42   a2204 = ACO 2204
    22 34 23.0   -37 43 29   a3888 = ACO 3888
    22 49 38.6   -64 23 15   a3921 = ACO 3921
    ----------------------------------------------------------

File Summary:

       FileName      Lrecl  Records   Explanations

ReadMe            80        .   This file
larcs3.dat        75     6427   LARCS spectroscopic cluster catalogues


See also:
   J/MNRAS/327/588 : Las Campanas/AAT Rich Cluster Survey - I (Pimbblet+, 2001)


Byte-by-byte Description of file: larcs3.dat

   Bytes Format Units   Label   Explanations

   1- 13  A13   ---     LARCS   LARCS identifier, aNNNN_NN:NNNN
  15- 16  I2    h       RAh     Right ascension (J2000)
  18- 19  I2    min     RAm     Right ascension (J2000)
  21- 25  F5.2  s       RAs     Right ascension (J2000)
      27  A1    ---     DE-     Declination sign (J2000)
  28- 29  I2    deg     DEd     Declination (J2000)
  31- 32  I2    arcmin  DEm     Declination (J2000)
  34- 37  F4.1  arcsec  DEs     Declination (J2000)
  39- 43  F5.2  mag     Rmag    R (0.6830um) magnitude
  45- 48  F4.2  mag     e_Rmag  rms uncertainty on Rmag
  50- 54  F5.2  mag     B-R     ?=- B-R colour index (1)
  56- 59  F4.2  mag     e_B-R   ?=- rms uncertainty on B-R (1)
  61- 66  I6    km/s    cz      Heliocentric redshift
  68- 70  I3    km/s    e_cz    rms uncertainty on cz
  72- 75  F4.1  ---     RTDR    Tonry & Davis (1979AJ.....84.1511T)
                                 quality value (2)

Note (1): Entries with "----" indicate that whilst the R band was observed, the
           B band was not (Pimbblet, 2001, Cat. J/MNRAS/327/588)
Note (2): RTDR is the ratio of the height of the fitted peak to the average
           height of peaks in the anti-symmetrical part of the cross-correlation
           function. The larger the value of RTDR, the better the fit of the
           template spectrum to the galaxy spectrum. Since each 2dF fibre is
           cross-correlated with many templates, it is necessary to determine
           which of the redshift estimates are correct. The redshift is usually
           taken to be the value with the highest RTDR.


Acknowledgements: Kevin Pimbblet, pimbblet(at)physics.uq.edu.au


References:
    O'Hely et al.,            1998PASA...15..273O
    Pimbblet et al, Paper I   2001MNRAS.327..588P, Cat. J/MNRAS/327/588
    Pimbblet et al, Paper II  2002MNRAS.331..333P
(End)                                      Patricia Vannier [CDS]    05-Jun-2006