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We use a new set of cold dark matter simulations of the local universe toinvestigate the distribution of fossils of primordial dwarf galaxies within,and around the Milky Way. Throughout, we build upon previous results showingagreement between the observed stellar properties of a subset of theultra-faint dwarfs and our simulated fossils. Here, we show that fossils of thefirst galaxies have galactocentric distributions and cumulative luminosityfunctions consistent with observations. In our model there are ~ 300 luminoussatellites orbiting the Milky Way, ~50-70% of which are well preserved fossils,with this fraction decreasing with galactocentric distance. Within the MilkyWay virial radius, the majority of these fossils have luminosities L_V<10^5L_solar. This work produces an overabundance of bright dwarf satellites (L_V >10^4 L_solar) with respect to observations where observations are nearlycomplete. The "bright satellite problem" is most evident in the outer parts ofthe Milky Way. We estimate that, although relatively bright, the primordialstellar populations are very diffuse, producing a population with surfacebrightnesses below surveys` detection limits and are easily stripped by tidalforces. Although we cannot yet present unmistakable evidence for the existenceof the fossils of first galaxies in the Local Group, the results of our studiessuggest observational strategies that may demonstrate their existence.Primarily, the detection of "ghost halos" of primordial stars around isolateddwarfs would prove that stars formed in minihalos (M<10^8 M_solar) beforereionization, and strongly suggest that at least a fraction of the ultra-faintdwarfs are fossils of the first galaxies.

Where are the Fossils of the First Galaxies? II. True Fossils, Ghost Halos, and the Missing Bright Satellites