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Dark Matter in Dwarf Galaxies

Published online by Cambridge University Press:  04 August 2017

John Kormendy
John Kormendy*
Affiliation:
Dominion Astrophysical Observatory, 5071 W. Saanich Road, Victoria, B. C. V8X 4M6 Canada

Abstract

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This paper reviews the observational evidence for dark matter (DM) in dwarf spiral (dS) and dwarf spheroidal (dE) galaxies. The most secure detection of DM in dwarf galaxies is given by HI rotation curves. They provide estimates of DM halo parameters, i. e., isothermal core radii r c , central densities ρ0 and one-dimensional velocity dispersions σ. The smallest DM halo measured so far is in DDO 127 (M B = −14.5 for H 0 = 75 km s−1 Mpc−1, r c ≃ 2.3 kpc, σ ≃ 27 km s−1). If this halo is made of neutrinos of mass m v , then phase-space constraints imply that m v > 110 eV. This is difficult to reconcile with cosmological upper limits giving Ω ≤ 1. Ultimately, dE galaxies will provide the strongest constraints on DM in dwarf galaxies; a detailed look at present results shows that they are not yet conclusive.

Information

Type
Review Paper
Information
Symposium - International Astronomical Union , Volume 117: Dark Matter in the Universe , 1987, pp. 139 - 152
Copyright
Copyright © Reidel 1987 

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