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J/AJ/110/463       Kinematics of the Shapley supercluster (Quintana+ 1995)
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The Shapley supercluster. I. Spectroscopic observations in the central region
     Quintana H., Ramirez A., Melnick J., Raychaudhury S., Slezak E.
    <Astron. J. 110, 463 (1995)>
    =1995AJ....110..463Q
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ADC_Keywords: Clusters, galaxy ; Radial velocities

Abstract:
    We present a new analysis of the kinematics of the Shapley
    supercluster based on radial velocities for 1087 galaxies in the
    clusters A3558 (Shapley 8), A3528 (Klemola 21), A3532 (Klemola 22),
    A3530, A3556 (SC 1321-314), A3559 (CE 1327-292), A3560, A3562,
    SC 1329-314 and in the intercluster region of the core of the
    supercluster, of which 367 are new measurements. We also present
    accurate positions from APM and MAMA scans of the ESO/SERC Southern
    Sky Survey photographic plates. We obtain new velocity dispersions and
    estimate the masses of the member clusters, evaluating dynamical
    models of the supercluster. The supercluster is found to be
    significantly flattened. We find that for Omega_0=0.3, H_0=75km/s/Mpc,
    the gravitational pull of the supercluster may account for up to 25%
    of the peculiar velocity of the Local Group required to explain the
    dipole anisotropy of the Cosmic Microwave Background radiation, in
    which case the mass of the supercluster would be dominated by
    intercluster dark matter. This fractional contribution would be
    considerably higher for combinations of significantly lower values of
    Omega_0 and higher values of H_0.

File Summary:
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 FileName    Lrecl    Records   Explanations
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ReadMe          80          .   This file
table2.dat      80        497   Galaxy velocities
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Byte-by-byte Description of file: table2.dat
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   Bytes Format  Units      Label      Explanations
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   1-  7  A7     ---       Region    ACO <VII/110> cluster name or
                                      cluster area code (1)
  10- 13  A4     ---       ID        Observing identifications
  16- 18  I3     ---       ESO       ? ESO field
  21- 26  A6     ---       Coord     APM, MAMA cat. numbers or other codes (2)
  29- 30  I2     h         RAh       Right ascension (1950)
  32- 33  I2     min       RAm       Right ascension (1950)
  35- 38  F4.1   s         RAs       Right ascension (1950)
      40  A1     ---       DE-       Declination sign
  41- 42  I2     deg       DEd       Declination (1950)
  44- 45  I2     arcmin    DEm       Declination (1950)
  47- 48  I2     arcsec    DEs       Declination (1950)
      49  A1     ---     u_RAh       Equatorial coordinate uncertainty flag
      51  A1     ---       Code      [R:<( ] Codes for following fields (3)
  53- 56  F4.1   mag       Jmag      ? Ptg. J mag, measured from APM survey
  58- 63  I6     km/s      RV        Heliocentric velocities
  65- 67  I3     km/s    e_RV        Heliocentric velocities error
  69- 73  A5     ---       R         R value or number of lines (4)
  76- 80  A5     ---       Ref       Code for observer or velocity reference (5)
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Note (1): Gives either the ACO <VII/110> cluster name, ordered by ascending
           number, or a code for the area where the cluster is located. These
           areas denote (1degree x 5min) regions (approx 1 square degree) in
           which we divided the field to program the observations, and are
           named by the coordinates of the NW corner.
Note (2): The APM, MAMA catalogue numbers or other codes used as source for
           coordinates. Most coordinates are either from digital scans of the
           SERC IIIa-J atlas, using the APM facility in Cambridge, England or
           from scans of ESO/SRC R fields done with the MAMA machine at
           Paris. For galaxies not found in the APM and MAMA scans, positions
           are quoted from the ESO/Uppsala catalog (Lauberts 1982, <VII/34>).
           Coordinates for galaxies in A3558 were measured with the Optronics
           machine at ESO, Garching.
Note (3): the code has the following ,eaning:
     R  = m_J is R magnitude from the MAMA survey.
     :  = m_J is uncertain (saturated image on plate or estimated by eye)
     <  = m_J is an upper limit (the magnitude quoted being the total
          magnitude of a merged image of which the galaxy is a part)
     (  = velocities are not used in the mean values of redshifts.
Note (4): The R value of the cross-correlation, or the number of lines
           measured in each spectra, if the line position method was used.
           The R value is a real value and the number of lines is an integer
           value.
Note (5): The code of observer/telescope/date or a reference code if the
           galaxy also has a velocity reported in the literature.
   Q1-Q7,M1-M3: observing sessions as in Table 1 of the printed paper.
   MGS87   Metcalfe et al. (1987MNRAS.225..581M)
   TCG90   Teague et al. (1990ApJS...72..715T)
   Da86    da Costa et al. (1986AJ.....91....6D)
   Da87    da Costa et al. (1987AJ.....93.1338D)
   DS88    Dressler and Shectman (1988AJ.....95..284D)
   D091    Dressler 1991 <J/ApJS/75/241>
   Cr87    Cristiani et al. (1987A&A...179..108C)
   R087    Richter, O.-G. (1987A&AS...67..261R)
   Ve90    Vettolani et al. (1990AJ.....99.1709V)
   Mo88    Monk et al. (1988MNRAS.234..193M)
   Mo89    Mould et al. (1989ApJ...338..654A)
   PGC     Paturel et al. Catalogue of Principal Galaxies, Monographies 
           de la Base de Donnees Extragalactiques, No 1, Lyon: Obs. de Lyon;
           (Catalog <VII/119>)
   1737    ZCAT Catalog, Huchra et al. 1993 <VII/164>
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Origin: AAS CD-ROM series, Volume 5, 1995         Lee Brotzman [ADS] 06-Oct-1995
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(End)                                                         [CDS]  10-Jan-1996

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