The M 81 group of galaxies: New distances, kinematics and structure

Free access article

Issue		A&A Volume 383, Number 1, February III 2002


Page(s)		125 - 136
Section		Extragalactic astronomy
DOI		http://dx.doi.org/10.1051/0004-6361:20011741

A&A 383, 125-136 (2002)
DOI: 10.1051/0004-6361:20011741

The M 81 group of galaxies: New distances, kinematics and structure

I. D. Karachentsev¹, A. E. Dolphin², D. Geisler³, E. K. Grebel⁴, P. Guhathakurta⁵, P. W. Hodge⁶, V. E. Karachentseva⁷, A. Sarajedini⁸, P. Seitzer⁹ and M. E. Sharina^{1, 10}

¹ Special Astrophysical Observatory, Russian Academy of Sciences, N. Arkhyz, KChR, 369167, Russia
² Kitt Peak National Observatory, National Optical Astronomy Observatories, PO Box 26732, Tucson, AZ 85726, USA
³ Departamento de Física, Grupo de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, Chile
⁴ Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
⁵ UCO/Lick Observatory, University of California at Santa Cruz, Santa Cruz, CA 95064, USA
⁶ Department of Astronomy, University of Washington, Box 351580, Seattle, WA, USA
⁷ Astronomical Observatory of Kiev University, 04053, Observatorna 3, Kiev, Ukraine
⁸ Department of Astronomy, University of Florida, Gainesville, FL 32611, USA
⁹ Department of Astronomy, University of Michigan, 830 Dennison Building, Ann Arbor, MI 48109, USA
¹⁰ Isaac Newton Institute, Chile, SAO Branch

(Received 25 September 2001 / Accepted 5 December 2001 )

Abstract
We present Hubble Space Telescope/WFPC2 images of the galaxies NGC 2366, NGC 2976, NGC 4236, IC 2574, DDO 53, DDO 82, DDO 165, Holmberg I, Holmberg II, Holmberg IX, K52, K73, BK3N, Garland, and A0952+69 in the M 81 complex. Their true distance moduli, derived from the brightness of the tip of the red giant branch, lie in the range of 27 $\fm$ 52 (NGC 2366) to 28 $\fm$ 30 (DDO 165), with a median of 27 $\fm$ 91, which is typical for other known M 81 group members. Using distances and radial velocities of about 50 galaxies in and around the M 81/NGC 2403 complex, we find the radius of the zero-velocity surface of the M 81 group to be $R_0 = (1.05\pm0.07$ ) Mpc, which yields a total mass $M(R_0) = (1.6\pm0.3)\times 10^{12}~M_{\odot}$ and a total mass-to-luminosity ratio $M(R_0)/L_B = (38\pm7)~M_{\odot}/L_{\odot}$ . The total mass within R₀ agrees well with the sum of masses estimated via the virial theorem ( $1.2\times 10^{12}~M_{\odot})$ and from orbital motions $(2.0\times 10^{12}~M_{\odot})$ of companions around M 81 and NGC 2403. We suggest that most of the dark matter in the group is concentrated around the luminous matter, allowing us to explain the observed asymmetry of the peculiar motions of the M 81 companions. M 81 itself has a peculiar velocity of about 130 km s ^-1 with respect to the local Hubble flow, but the centroid of the M 81/NGC 2403 complex is almost at rest with respect to Hubble flow $(v_{\rm pec} < 35$ km s ^-1).

Key words: galaxies: dwarf -- galaxies: distances and redshifts -- galaxies: structure -- galaxies: kinematics and dynamics

Offprint request: I. D. Karachentsev, ikar@luna.sao.ru

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