Elliptical Galaxy Halo Masses from Internal Kinematics
Abstract
The halo masses of nearby individual elliptical galaxies can be estimated by using the kinematics of their stars, planetary nebulae, and globular clusters -- ideally in combination. With currently improving coverage of galaxies of ordinary luminosities and morphologies, systematic trends may be identified. Bright, boxy ellipticals show strong signatures of dark matter, while faint, disky ones typically do not. The former result is problematic for the MOND theory of gravity, and the latter is a challenge to explain in the LCDM paradigm of galaxy formation.
Cite
@article{arxiv.astro-ph/0510183,
title = {Elliptical Galaxy Halo Masses from Internal Kinematics},
author = {Aaron J. Romanowsky},
journal= {arXiv preprint arXiv:astro-ph/0510183},
year = {2009}
}
Comments
8 pages, 8 figs. Invited review contribution in Proceedings of XXIst IAP Colloquium, "Mass Profiles & Shapes of Cosmological Structures" (Paris, 4-9 July 2005), eds G. A. Mamon, F. Combes, C. Deffayet, B. Fort (Paris: EDP Sciences). Color figs may print better as ps than pdf. v2: refs updated and Fig 2b corrected