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The Structure of Dark Matter Halos in Dwarf Galaxies
Open accessAbstract
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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Kouvaris, C., & Tinyakov, P. (2010) · Physical Review D · doi:10.1103/physrevd.82.063531 · Cited by 270
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Cuoco, A., Krämer, M., & Korsmeier, M. (2017) · Physical Review Letters · doi:10.1103/physrevlett.118.191102 · Cited by 256
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Metadata
- Authors
- Burkert, A.
- Venue
- Symposium - International Astronomical Union
- Publisher
- Cambridge University Press (CUP)
- Published
- 1996
- Volume
- 171
- Pages
- 175-178
- ISSN
- 0074-1809 (ISSN-L)
- OpenAlex
- W3148503721
- Cited by
- 176
- References
- 0
- FWCI
- 0.00
- Type
- conference paper
- Language
- en
- Open access
- bronze
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