Hostname: page-component-cd9895bd7-mkpzs Total loading time: 0 Render date: 2024-12-24T16:13:59.607Z Has data issue: false hasContentIssue false
  • English
  • Français

The Structure of Dark Matter Halos in Dwarf Galaxies

Published online by Cambridge University Press:  25 May 2016

A. Burkert
A. Burkert*
Affiliation:
Max-Planck-Institut für Astronomie Königstuhl 17, 69117 Heidelberg, Germany

Extract

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.

Some dwarf galaxies have HI rotation curves that are completely dominated by a surrounding dark matter (DM) halo (e.g. Carignan & Freeman 1988). These objects represent ideal candidates for an investigation of the density structure of low-mass DM halos as the uncertainties resulting from the subtraction of the visible component are small, even in the innermost regions. Flores & Primack (1994) and Moore (1994) compared the observed DM rotation curves with the profiles, predicted from cosmological cold dark matter (CDM) calculations. They found an interesting discrepancy: whereas the calculations lead to a DM density distribution which diverges as ρ ∼ r−1 in the inner parts, the observed rotation curves indicate shallow DM cores which can be described by an isothermal density profile with finite central density.

Type
Dark Matter Halos around Galaxies
Information
Symposium - International Astronomical Union , Volume 171: New Light on Galaxy Evolution , 1996 , pp. 175 - 178
Copyright
Copyright © Kluwer 1996 

References

Burkert, A. 1995, Astrophys. J., 447, L25 Google Scholar
Carignan, C. and Freeman, K.C. 1988, Astrophys. J., 332, L33 Google Scholar
Flores, R.A. and Primack, J.R. 1994, Astrophys. J., 427, L1 CrossRefGoogle Scholar
Moore, B. 1994, Nature, 370, 629 Google Scholar
Navarro, J.F., Frenk, C.S. and White, S.D.M. 1995, MNRAS, 275, 56 Google Scholar