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We present a new method for generating initial conditions for LCDM N-bodysimulations which provides the dynamical range necessary to follow theevolution and distribution of the fossils of the first galaxies on LocalVolume, 5-10 Mpc, scales. The initial distribution of particles represents theposition, velocity and mass distribution of the dark and luminous halosextracted from pre-reionization simulations. We confirm previous results thatultra-faint dwarfs have properties compatible with being well preserved fossilsof the first galaxies. However, because the brightest pre-reionization dwarfsform preferentially in biased regions, they most likely merge into non-fossilhalos with circular velocities >20-30 km/s. Hence, we find that the maximumluminosity of true-fossils in the Milky Way is L_V<10^5 L_solar, casting doubtson the interpretation that some classical dSphs are true-fossils. In addition,we argue that most ultra-faints at small galactocentric distance, R<50 kpc, hadtheir stellar properties modified by tides, while a large population of fossilsis still undetected due to their extremely low surface brightness log(Sigma_V)< -1.4. We estimate that the region outside R_50 (~ 400 kpc) up to 1 Mpc fromthe Milky Way contains about a hundred true fossils of the first galaxies withV-band luminosities 10^3 - 10^5 L_solar and half-light radii, r_hl ~ 100-1000pc.

Where are the Fossils of the First Galaxies? I. Local Volume Maps and Properties of the Undetected Dwarfs