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Date and Time of the Query: 2019-06-25 T00:39:22 PDT
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For refcode 2002A&A...383..125K:
Retrieve 61 NED objects in this reference.
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Copyright by European Southern Observatory (ESO). Reproduced by permission
2002A&A...383..125K The M 81 group of galaxies: New distances, kinematics and structure I. D. Karachentsev, A. E. Dolphin, D. Geisler, E. K. Grebel, P. Guhathakurta, P. W. Hodge, V. E. Karachentseva, A. Sarajedini, P. Seitzer and M. E. Sharina Special Astrophysical Observatory, Russian Academy of Sciences, N. Arkhyz, KChR, 369167, Russia Kitt Peak National Observatory, National Optical Astronomy Observatories, PO Box 26732, Tucson, AZ 85726, USA Departamento de Fisica, Grupo de Astronomia, Universidad de Concepcion, Casilla 160-C, Concepcion, Chile Max-Planck-Institut fur Astronomie, Konigstuhl 17, 69117 Heidelberg, Germany UCO/Lick Observatory, University of California at Santa Cruz, Santa Cruz, CA 95064, USA Department of Astronomy, University of Washington, Box 351580, Seattle, WA, USA Astronomical Observatory of Kiev University, 04053, Observatorna 3, Kiev, Ukraine Department of Astronomy, University of Florida, Gainesville, FL 32611, USA Department of Astronomy, University of Michigan, 830 Dennison Building, Ann Arbor, MI 48109, USA 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 27.52^m^ (NGC 2366) to 28.30^m^ (DDO 165), with a median of 27.91^m^, 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+/-0.07) Mpc, which yields a total mass M(R_0_) = (1.6+/-0.3) x 10^12^ M_sun_ and a total mass-to-luminosity ratio M(R_0_)/L_B_ = (38+/-7) M_sun_/L_sun_. The total mass within R_0_ agrees well with the sum of masses estimated via the virial theorem (1.2 x 10^12^ M_sun_) and from orbital motions (2.0 x 10^12^ M_sun_) 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_pec_ < 35 km s^-1^). Key words: galaxies: dwarf - galaxies: distances and redshifts - galaxies: structure - galaxies: kinematics and dynamics
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