2005/09/08 by И. Д. Караченцев, I. D. Karachentsev, Karachentsev, I. D. +2
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics (astro-ph) #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0509207
18 pages, 5 figures, accepted for publication in Astrofizica
openalex publication_date 2005/09/08 · arxiv created 2005/09/09 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
Based on accurate measurements of distances to nearby galaxies made with Hubble Space Telescope, we determined the radii of the zero-velocity surface: R0 = 0.96+-0.03 Mpc for the Local Group and R0 = 0.89+-0.05 Mpc for the group of galaxies around M81/M82. This yields the total masses of the groups to be MT = (1.29+-0.14) 1012 Msun and MT = (1.03+-0.17) 1012 Msun, respectively. The R0-method allowed us to determine the mass ratio of the brightest two members in the considered groups. Based on the minimum scatter of galaxies with respect to the Hubble regression, we derived a mass ratio of 0.8 : 1.0 for the Milky Way and Andromeda, and 0.54 : 1.00 for M82 and M81, which is quite close to the ratio of luminosities of these galaxies.