The Hubble flow around the Local Group |
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Authors: | I. D. Karachentsev O. G. Kashibadze D. I. Makarov R. B. Tully |
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Affiliation: | Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhnij Arkhyz, KChR, 369167, Russia;Institute for Astronomy of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA |
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Abstract: | We use updated data on distances and velocities of galaxies in the proximity of the Local Group (LG) in order to establish properties of the local Hubble flow. For 30 neighbouring galaxies with distances 0.7 < D LG < 3.0 Mpc, the local flow is characterized by the Hubble parameter H loc= (78 ± 2) km s−1 Mpc−1 , the mean-square peculiar velocity σv= 25 km s−1 , corrected for errors of radial velocity measurements (∼4 km s−1) and distance measurements (∼10 km s−1) , as well as the radius of the zero-velocity surface R 0= (0.96 ± 0.03) Mpc. The minimum value for σv is achieved when the barycentre of the LG is located at the distance Dc = (0.55 ± 0.05) D M31 towards Andromeda galaxy (M31) corresponding to the Milky Way (MW)-to-M31 mass ratio M MW/ M M31≃ 4/5 . In the reference frame of the 30 galaxies at 0.7–3.0 Mpc, the LG barycentre has a small peculiar velocity ∼(24 ± 4) km s−1 towards the Sculptor constellation. The derived value of R 0 corresponds to the total mass M T(LG) = (1.9 ± 0.2) 1012 M⊙ with Ωm= 0.24 and a topologically flat universe, a value in good agreement with the sum of virial mass estimates for the MW and M31. |
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Keywords: | Local Group dark matter |
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