Velocity dispersion around ellipticals in MOND

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 (~ 20kpc) with stellar tracers, such as planetary nebulae, or large scale (~ 200kpc) 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.

4 pages, 3 figures, accepted in A&A Letters

References in corpus (3)

• On the Proof of Dark Matter, the Law of Gravity and the Mass of Neutrinos
• Escaping from MOND
• Loss of mass and stability of galaxies in MOND

Cited by in corpus (7)

• The PN.S Elliptical Galaxy Survey: the dark matter in NGC 4494
• X-ray Group and cluster mass profiles in MOND: Unexplained mass on the group scale
• Milky Way potentials in CDM and MOND. Is the Large Magellanic Cloud on a bound orbit?
• Reconciling MOND and dark matter?
• The velocity distribution of SDSS satellites in MOND
• An Uneven Vacuum Energy Fluid as $\Lambda$, Dark Matter, MOND and Lens
• Galaxy Bulges As Tests of CDM vs MOND in Strong Gravity