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The conjecture that the ancient globular clusters (GCs) formed at the centerof their own dark matter halos was first proposed by Peebles (1984), and hasrecently been revived to explain the puzzling abundance patterns observedwithin many GCs. In this paper we demonstrate that the outer stellar densityprofile of isolated GCs is very sensitive to the presence of an extended darkhalo. The GCs NGC 2419, located at 90 kpc from the center of our Galaxy, andMGC1, located at ~200 kpc from the center of M31, are ideal laboratories fortesting the scenario that GCs formed at the centers of massive dark halos.Comparing analytic models to observations of these GCs, we conclude that theseGCs cannot be embedded within dark halos with a virial mass greater than 10^6Msun, or, equivalently, the dark matter halo mass-to-stellar mass ratio must beMdm/M_*<1. If these GCs have indeed orbited within weak tidal fields throughouttheir lifetimes, then these limits imply that these GCs did not form withintheir own dark halos. Recent observations of an extended stellar halo in the GCNGC 1851 are also interpreted in the context of our analytic models.Implications of these results for the formation of GCs are briefly discussed.

Evidence Against Dark Matter Halos Surrounding the Globular Clusters MGC1 and NGC 2419