The conjecture that the ancient globular clusters ( GCs ) formed at the center of their own dark matter halos was first proposed by Peebles ( 39 ) , and has recently been revived to explain the puzzling abundance patterns observed within many GCs . In this paper we demonstrate that the outer stellar density profile of isolated GCs is very sensitive to the presence of an extended dark halo . The GCs NGC 2419 , located at 90 kpc from the center of our Galaxy , and MGC1 , located at \sim 200 kpc from the center of M31 , are ideal laboratories for testing the scenario that GCs formed at the centers of massive dark halos . Comparing analytic models to observations of these GCs , we conclude that these GCs can not be embedded within dark halos with a virial mass greater than 10 ^ { 6 } M _ { \sun } , or , equivalently , the dark matter halo mass-to-stellar mass ratio must be M _ { DM } / M _ { \ast } < 1 . If these GCs have indeed orbited within weak tidal fields throughout their lifetimes , then these limits imply that these GCs did not form within their own dark halos . Recent observations of an extended stellar halo in the GC NGC 1851 are also interpreted in the context of our analytic models . Implications of these results for the formation of GCs are briefly discussed .