Investigations of the Local Supercluster Velocity Field III. Tracing the backside infall with distance moduli from the direct Tully-Fisher relation

Details Investigations of the Local Supercluster Velocity Field III. Tracing the backside infall with distance moduli from the direct Tully-Fisher relation Investigations of the Local Supercluster Velocity Field III. Tracing the backside infall with distance moduli from the direct Tully-Fisher relation

2000-01-27

arxiv.org/abs/astro-ph/0001475v1

Astronomy and Astrophysics

Astrophysics

13 pages, 9 figures. Accepted to A&A. Typeset with the A&A Latex package

Scientific paper

We have extended the discussion of Paper II (Ekholm et al. 1999) to cover also the backside of the Local Supercluster (LSC) by using 96 galaxies within Theta<30 deg from the adopted centre of LSC and with distance moduli from the direct B-band Tully-Fisher relation. In order to minimize the influence of the Malmquist bias we required log V_max>2.1 and sigma_{B_T}<0.2 mag. We found out that if R_Virgo<20 Mpc this sample fails to follow the expected dynamical pattern from the Tolman-Bondi (TB) model. When we compared our results with the Virgo core galaxies given by Federspiel et al. (1998) we were able to constrain the distance to Virgo: R_Virgo=20-24 Mpc. When analyzing the TB-behaviour of the sample as seen from the origin of the metric as well as that with distances from the extragalactic Cepheid PL-relation we found additional support to the estimate R_Virgo=21 Mpc given in Paper II. Using a two-component mass-model we found a Virgo mass estimate M_Virgo= (1.5-2)M_virial, where M_virial=9.375.10^14M_sun for R_Virgo=21 Mpc. This estimate agrees with the conclusion in Paper I (Teerikorpi et al. 1992). Our results indicate that the density distribution of luminous matter is shallower than that of the total gravitating matter when q_0<=0.5. The preferred exponent in the density power law, alpha\approx2.5, agrees with recent theoretical work on the universal density profile of dark matter clustering in an Einstein-deSitter universe (Tittley & Couchman 1999).

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