Hostname: page-component-77c89778f8-cnmwb Total loading time: 0 Render date: 2024-07-19T07:39:21.831Z Has data issue: false hasContentIssue false
  • English
  • Français

Formation of dwarf galaxies and small-scale problems of CDM

Published online by Cambridge University Press:  01 August 2006

Oleg Y. Gnedin
Oleg Y. Gnedin*
Affiliation:
University of Michigan, Department of Astronomy, Ann Arbor, MI 48109-1042, USAognedin@umich.edu
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The concordance cosmological model based on cold dark matter makes definitive predictions for the growth of galaxies in the Universe, which are being actively studied using numerical simulations. These predictions appear to contradict the observations of dwarf galaxies. Dwarf dark matter halos are more numerous and have steeper central density profiles than the observed galaxies. The first of these small-scale problems, the “missing satellites problem”, can be resolved by accounting for the low efficiency of gas cooling and star formation in dwarf halos. A newly-discovered class of HyperVelocity Stars will soon allow us to test another generic prediction of CDM models, the triaxial shapes of dark matter halos. Measuring the proper motions of HVS will probe the gravitational potential out to 100 kpc and will constrain the axis ratios and the orientation of the Galactic halo.

Keywords

dark matter — Galaxy: halo — galaxies: dwarf — galaxies: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S235: Galaxy Evolution Across the Hubble Time , August 2006 , pp. 385 - 388
Copyright
Copyright © International Astronomical Union 2007

References

Belokurov, V. 2006, ApJ submitted, astro-ph/0608448Google Scholar
Brown, W. R., Geller, M. J., Kenyon, S. J. & Kurtz, M. J. 2005, ApJ 622, L33; 2006a, ApJ 640, L35; 2006b, ApJ 647, 303CrossRefGoogle Scholar
Edelmann, H. 2005, ApJ 634, L181CrossRefGoogle Scholar
Gnedin, N. Y. & Kravtsov, A. V. 2006, ApJ 645, 1054CrossRefGoogle Scholar
Gnedin, O. Y., Gould, A., Miralda-Escude, J. & Zentner, A. R. 2005, ApJ 634, 344CrossRefGoogle Scholar
Helmi, A. 2004, MNRAS 351, 643CrossRefGoogle Scholar
Hills, J. G. 1988, Nature 331, 687CrossRefGoogle Scholar
Hirsch, H. A., Heber, U., O'Toole, S. J. & Bresolin, F. 2005, A&A 444, L61Google Scholar
Johnston, K. V., Law, D. R. & Majewski, S. R. 2005, ApJ 619, 800CrossRefGoogle Scholar
Kazantzidis, S., Kravtsov, A. V., Zentner, A. R., Allgood, B., Nagai, D. & Moore, B. 2004, ApJ 611, L73CrossRefGoogle Scholar
Klypin, A., Kravtsov, A. V., Valenzuela, O. & Prada, F. 1999, ApJ 522, 82–92CrossRefGoogle Scholar
Kravtsov, A. V., Gnedin, O. Y. & Klypin, A. A. 2004, ApJ 609, 482CrossRefGoogle Scholar
Moore, B. 1999, ApJ 524, L19CrossRefGoogle Scholar