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J/A+A/327/952       Centaurus cluster velocities (Stein+ 1997)
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Velocity structure of the dwarf galaxy population in the Centaurus cluster
       Stein P., Jerjen H., Federspiel M.
      <Astron. Astrophys. 327, 952 (1997)>
      =1997A&A...327..952S      (SIMBAD/NED BibCode)
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ADC_Keywords: Clusters, galaxy ; Radial velocities
Keywords: clusters of galaxies: general: Centaurus cluster - evolution of -
          galaxies: redshifts; evolution; NGC 4696

Abstract:
    Based on the photometric survey of the inner region of the Centaurus
    cluster (Jerjen & Dressler, 1997, Cat. <J/A+AS/124/1>) we measured
    redshifts for a deep, surface brightness limited sample of galaxies
    using the MEFOS multifibre spectrograph at the ESO 3.6m telescope.
    With the new data set radial velocities for 120 centrally located
    cluster members become available which is equivalent to 78% of all
    known cluster galaxies in the region brighter than B_T_=18.5. The
    relevant aspect of this investigation is that new redshifts for 32
    dwarf galaxies have been measured, rising the total number to 48. We
    investigate the prominent bimodal velocity distribution of Centaurus
    in more detail, discussing the very different characteristics of the
    velocity distributions for the main Hubble types E&S0, spirals,
    Im&BCD, and dE&dS0. The nucleated, bright dwarf ellipticals are the
    only galaxies with a Gaussian-like distribution centred at
    3148+/-98km/s. The remarkable coincidence of this velocity with the
    mean velocity of Cen 30 and the redshift of NGC 4696 in particular
    strongly suggests a connection of the dE&dS0s to the gravitational
    centre of the Centaurus cluster and/or to the cluster dominant E
    galaxy. The application of statistical tests reveals the existence of
    a population dwarf galaxies bound to NGC 4696. The dynamical
    parameters for the two velocity components suggest that Cen 30 is the
    real Centaurus cluster whereas Cen 45 can only be a loosely bound
    group of galaxies. This conclusion is followed up with a type-mixture
    analysis. All results are fully consistent with the cluster-group
    scenario. Whether Cen 45 is merging with the cluster or is located in
    the close background remains unclear. We show that the poorness of Cen
    45 represents an intrinsic problem which makes it difficult to
    approach this question.

File Summary:
--------------------------------------------------------------------------------
  FileName   Lrecl  Records   Explanations
--------------------------------------------------------------------------------
ReadMe          80        .   This file
table5a.dat     81       36   New redshifts for Centaurus cluster members
table5b.dat     81       14   New redshifts of background galaxies
table5c.dat     81       65   Reobserved redshifts for Centaurus cluster members
table5.tex      97      283   LaTeX version of table5
table5.ps       83      931   PostScript version of table5
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See also:
   J/A+AS/124/1 : The Centaurus Cluster Catalogue (Jerjen+ 1997)

Byte-by-byte Description of file: table5a.dat, table5b.dat, table5c.dat
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   Bytes Format    Units    Label Explanations
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   1-  3  I3       ---      Seq   Sequential number
   5-  6  I2       h        RAh   Right ascension (1950.0)
   8-  9  I2       min      RAm   Right ascension (1950.0)
  11- 15  F5.2     s        RAs   Right ascension (1950.0)
      17  A1       ---      DE-   Declination sign
  18- 19  I2       deg      DEd   Declination (1950.0)
  21- 22  I2       arcmin   DEm   Declination (1950.0)
  24- 27  F4.1     arcsec   DEs   Declination (1950.0)
  29- 31  I3       ---      CCC   Centaurus Cluster Catalogue (Jerjen & Dressler
                                   1996, Cat. <J/A+AS/124/1>) reference number
  33- 38  A6       ---      Mtype Morphological type
  40- 44  F5.2     mag      BT    Total blue magnitude
  46- 49  F4.1 mag/arcsec+2 SBeff ? Effective surface brightness
  51- 54  F4.2     %        Prob  ? Cen 45 cluster member probability (1)
  56- 60  I5       km/s     Vcc   ? Cross-correlation redshift
  62- 63  I2       km/s   e_Vcc   ? rms uncertainty on Vcc
  65- 69  I5       km/s     Vem   ? Emission line redshift
  71- 72  I2       km/s   e_Vem   ? rms uncertainty on Vem
  74- 78  I5       km/s     cz    ? Heliocentric radial velocity (2)
  80- 81  I2       km/s   e_cz    ? rms uncertainty on cz
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Note (1): If prob=0.00, this automatically implies that the galaxy is
           a 100% Cen 30 member.
Note (2): Weighted average of Vccf and Vemi.
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Acknowledgements: Martin Federspiel <martin@astro.unibas.ch>
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(End)                                          Patricia Bauer [CDS]  26-Jan-1998