In an old stellar population, most of the mass is either in the form of main-sequence stars, with masses ≲ ≲ 1–2 Solar masses, or in black hole remnants, with masses ~ 10–20 Solar masses. It is likely that the main-sequence stars dominate the total density; so their density should follow the Bahcall–Wolf form whereas the black holes should have the steeper, ρ ~ r profile. On the other hand, it has been suggested that the distribution of stellar masses at the Galactic Center is "top-heavy", with a much larger fraction of black holes. If this is the case, the observed stars would be expected to attain the shallower density profile, ρ ~ r. The number and distribution of black hole remnants at the Galactic Center is very poorly constrained.