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The Structure of Dark Matter Halos in Dwarf Galaxies

  • A. Burkert
Conference paper
Part of the International Astronomical Union / Union Astronomique Internationale book series (IAUS, volume 171)

Abstract

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.

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References

  1. Burkert, A. 1995, Astrophys. J., 447, L25ADSCrossRefGoogle Scholar
  2. Carignan, C. and Freeman, K.C. 1988, Astrophys. J., 332, L33ADSCrossRefGoogle Scholar
  3. Flores, R.A. and Primack, J.R. 1994, Astrophys. J., 427, L1ADSCrossRefGoogle Scholar
  4. Moore, B. 1994, Nature, 370, 629ADSCrossRefGoogle Scholar
  5. Navarro, J.F., Frenk, C.S. and White, S.D.M. 1995, MNRAS, 275, 56ADSGoogle Scholar

Copyright information

© Springer Science+Business Media Dordrecht 1996

Authors and Affiliations

  • A. Burkert
    • 1
  1. 1.Max-Planck-Institut für AstronomieHeidelbergGermany

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