Free access article

A&A 476, L1-L4 (2007)
DOI: 10.1051/0004-6361:20078569

Letter

Velocity dispersion around ellipticals in MOND

O. Tiret¹, F. Combes¹, G. W. Angus², B. Famaey³, and H. S. Zhao<sup>2

1</sup>  Observatoire de Paris, LERMA, 61 Av. de l'Observatoire, 75014 Paris, France
    e-mail: olivier.tiret@obspm.fr
²  SUPA, School of Physics and Astronomy, Univ. of St. Andrews, Scotland KY169SS, UK
³  Institut d'Astronomie et d'Astrophysique, Univ. Libre de Bruxelles, CP 226, Bvd du Triomphe, 1050 Bruxelles, Belgium

(Received 29 August 2007 / Accepted 15 October 2007 )

Abstract
We investigate how different models that have been proposed for solving the dark matter problem can fit the velocity dispersion observed around elliptical galaxies, on either a small scale (~20 kpc) with stellar tracers, such as planetary nebulae, or large scale (~200 kpc) with satellite galaxies as tracers. Predictions of Newtonian gravity, either containing pure baryonic matter, or embedded in massive cold dark matter (CDM) haloes, are compared with predictions of the modified gravity of MOND. The standard CDM model has problems on a small scale, and the Newtonian pure baryonic model has difficulties on a large scale, while a fit with MOND is possible on both scales.

Key words: galaxies: elliptical and lenticular, cD -- galaxies: kinematics and dynamics -- cosmology: dark matter

© ESO 2007

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