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Globular Cluster Systems and the Missing Satellite Problem: Implications for Cold Dark Matter Models

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© 2002. The American Astronomical Society. All rights reserved. Printed in U.S.A.
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Author e-mails

pcote@physics.rutgers.edu

west@bohr.uhh.hawaii.edu

marzke@quark.sfsu.edu

Author affiliations

1 Department of Physics and Astronomy, Rutgers University, New Brunswick, NJ 08854

2 Department of Physics and Astronomy, University of Hawaii, Hilo, HI 96720

3 Department of Physics and Astronomy, San Francisco State University, 1600 Holloway Avenue, San Francisco, CA 94132

Dates

Received 2001 October 2
Accepted 2001 November 23

Citation

Patrick Côté et al 2002 ApJ 567 853

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DOI

https://doi.org/10.1086/338670

Keywords

cosmology: observations; dark matter; galaxies: elliptical and lenticular, cD; galaxies: formation; galaxies: star clusters

Journal RSS feed

0004-637X/567/2/853

Abstract

We analyze the metallicity distributions of globular clusters belonging to 28 early-type galaxies in the survey of Kundu & Whitmore. A Monte Carlo algorithm that simulates the chemical evolution of galaxies that grow hierarchically via dissipationless mergers is used to determine the most probable protogalactic mass function for each galaxy. Contrary to the claims of Kundu & Whitmore, we find that the observed metallicity distributions are in close agreement with the predictions of such hierarchical formation models. The mass spectrum of protogalactic fragments for the galaxies in our sample has a power-law behavior, n(M) ∝ Mα, with an index of α sime -2. This spectrum is indistinguishable from the mass spectrum of dark matter halos predicted by cold dark matter models for structure formation. We argue that these protogalactic fragments—the likely sites of globular cluster formation in the early universe—are the disrupted remains of the "missing" satellite galaxies predicted by cold dark matter models. Our findings suggest that the solution to the missing satellite problem is through the suppression of gas accretion in low-mass halos after reionization, or via self-interacting dark matter, and argue against models with suppressed small-scale power or warm dark matter.

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