Volume 393, Number 1, October I 2002
|Page(s)||57 - 68|
|Section||Cosmology (including clusters of galaxies)|
|Published online||18 September 2002|
Local velocity field from sosie galaxies*
I. The Peebles' model
CRAL-Observatoire de Lyon, UMR 5574, 69230 Saint-Genis Laval, France
Corresponding author: G. Paturel, email@example.com
Accepted: 20 June 2002
Pratton et al. (1997) showed that the velocity field around clusters could generate an apparent distortion that appears as tangential structures or radial filaments. In the present paper we determine the parameters of the Peebles' model (1976) describing infall of galaxies onto clusters with the aim of testing quantitatively the amplitude of this distortion. The distances are determined from the concept of sosie galaxies (Paturel 1984) using 21 calibrators for which the distances were recently calculated from two independent Cepheid calibrations. We use both B and I-band magnitudes. The Spaenhauer diagram method is used to correct for the Malmquist bias. We give the equations for the construction of this diagram. We analyze the apparent Hubble constant in different regions around Virgo and obtain simultaneously the Local Group infall and the unperturbed Hubble constant. We found: The front side and backside infalls can be seen around Virgo and Fornax. In the direction of Virgo the comparison is made with the Peebles' model. We obtain: with for Virgo and for Fornax, with the adopted units (km s-1 and Mpc). We obtain the following mean distance moduli: All these quantities form an accurate and coherent system.
Key words: galaxies: general / galaxies: distances and redshifts / cosmology: distance scale / methods: statistical
© ESO, 2002
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