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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

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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

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