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
Burkert, A. 1995, Astrophys. J., 447, L25
Carignan, C. and Freeman, K.C. 1988, Astrophys. J., 332, L33
Flores, R.A. and Primack, J.R. 1994, Astrophys. J., 427, L1
Moore, B. 1994, Nature, 370, 629
Navarro, J.F., Frenk, C.S. and White, S.D.M. 1995, MNRAS, 275, 56
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© 1996 Springer Science+Business Media Dordrecht
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Burkert, A. (1996). The Structure of Dark Matter Halos in Dwarf Galaxies. In: Bender, R., Davies, R.L. (eds) New Light on Galaxy Evolution. International Astronomical Union / Union Astronomique Internationale, vol 171. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-0229-9_25
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DOI: https://doi.org/10.1007/978-94-009-0229-9_25
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