1999/03/18 by Stéphane Courteau, Stephane Courteau, Sidney van den Bergh · 8 citations
Physics and Astronomy · #Astrophysics and Star Formation Studies #Galaxies: Formation, Evolution, Phenomena #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/300942
To appear in the Astronomical Journal, July 1999 -- 23 pages, 1 table (landscape format), and 6 figures
arxiv created 1999/03/18 · openalex publication_date 1999/07/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/31
New data on the membership of the Local Group (LG) are used, in conjunction with new and improved radial velocity data, to refine the derivation of the motion of the Sun relative to the LG. The Sun is found to be moving with a velocity of V = 306 ± 18 km s -1 toward an apex at l = 99° ± 5° and b = -4° ± 4°. This finding agrees very well with previous analyses, but we discuss the possibility of a bias if the phase-space distribution of LG galaxies is bimodal. The LG radial velocity dispersion is 61 ± 8 km s -1 . We use various mass estimators to compute the mass of the LG and the Andromeda subgroup. We find M LG = (2.3 ± 0.6) × 10 12 M ⊙ , from which M / L V = 44 ± 12 (in solar units). For an assumed LG age of 14 ± 2 Gyr, the radius of an idealized LG zero-velocity surface is r 0 = 1.18 ± 0.15 Mpc. The LG is found to have 35 likely members. Only three of these have (uncertain) distances ≳1.0 Mpc from the LG barycenter. Barring new discoveries of low surface brightness dwarfs, this suggests that the LG is more compact and more isolated from its surroundings than previously believed.