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

2000/01/27 by T. Ekholm, Ekholm, T., P. Lanoix +8
Economics, Econometrics and Finance · Physics and Astronomy · #Astrophysics (astro-ph) #Cosmology and Gravitation Theories #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #High-Energy Particle Collisions Research #Scientific Research and Discoveries #Stochastic processes and financial applications #Theoretical and Computational Physics #astro-ph

paper · pdf · doi:10.48550/arxiv.astro-ph/0001475

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

arxiv created 2000/01/27 · openalex publication_date 2000/01/27 · arxiv updated 2009/12/01 · openalex created_date 2020/07/16 · openalex updated_date 2026/07/28

Abstract

We have extended the discussion of Paper II (Ekholm et al. 1999) to cover\nalso the backside of the Local Supercluster (LSC) by using 96 galaxies within\nTheta<30 deg from the adopted centre of LSC and with distance moduli from the\ndirect B-band Tully-Fisher relation. In order to minimize the influence of the\nMalmquist bias we required log V_max>2.1 and sigma_BT<0.2 mag.\n We found out that if R_Virgo<20 Mpc this sample fails to follow the expected\ndynamical pattern from the Tolman-Bondi (TB) model. When we compared our\nresults with the Virgo core galaxies given by Federspiel et al. (1998) we were\nable to constrain the distance to Virgo: R_Virgo=20-24 Mpc.\n When analyzing the TB-behaviour of the sample as seen from the origin of the\nmetric as well as that with distances from the extragalactic Cepheid\nPL-relation we found additional support to the estimate R_Virgo=21 Mpc given in\nPaper II. Using a two-component mass-model we found a Virgo mass estimate\nM_Virgo= (1.5-2)M_virial, where M_virial=9.375.10¹4M_sun for R_Virgo=21 Mpc.\nThis estimate agrees with the conclusion in Paper I (Teerikorpi et al. 1992).\n Our results indicate that the density distribution of luminous matter is\nshallower than that of the total gravitating matter when q₀<=0.5. The\npreferred exponent in the density power law, alpha\≈2.5, agrees with\nrecent theoretical work on the universal density profile of dark matter\nclustering in an Einstein-deSitter universe (Tittley & Couchman 1999).\n

Related

• Investigations of the Local Supercluster Velocity Field II. A study using Tolman-Bondi solution and galaxies with accurate distances from the Cepheid PL-relation
• A Re-Examination of the Origins of the Peculiar Velocity Field Within the Local Supercluster
• Focussing in on H₀
• Bias Properties of Extragalactic Distance Indicators XII: Bias Effects of Slope Differences and Intrinsic Dispersion on Tully-Fisher Distances to Galaxy Clusters with Application to the Virgo Cluster
• The Distance to the Virgo Cluster from a Recalibrated Tully-Fisher Relation Based on HST Cepheids and a Demonstrated Teerikorpi Cluster Incompleteness Bias