Dark matter subhalos and the dwarf satellites of the Milky Way.
MADAU P., DIEMAND J. and KUHLEN M.
Abstract (from CDS):
The Via Lactea simulation of the cold dark matter halo of the Milky Way predicts the existence of many thousands of bound subhalos with masses above 106M☉, distributed approximately with equal mass per decade of mass. Here we show that (1) a similar steeply rising subhalo mass function is also present at redshift z=0.5 in an elliptical-sized halo simulated with comparable resolution in a different cosmology. Compared to Via Lactea, this run produces nearly a factor of 2 more subhalos with large circular velocities; (2) the fraction of Via Lactea mass brought in by subhalos that have a surviving bound remnant today reaches 45%. Most of the Via Lactea mass is acquired in resolved discrete clumps, with no evidence for a significant smooth infall; (3) because of tidal mass loss, the number of subhalos surviving today that reached a peak circular velocity of >10 km/s throughout their lifetime exceeds half a thousand, 5 times larger than their present-day abundance; (4) unless the circular velocity profiles of Galactic satellites peak at values significantly higher that expected from the stellar line-of-sight velocity dispersion, only about one in five subhalos with Vmax>20 km/s today must be housing a luminous dwarf; (5) nearly 600 halos with masses greater than 107M☉ are found today in the ``field'' between r200 and 1.5r200, i.e. small dark matter clumps appear to be relatively inefficient at forming stars even well beyond the virial radius; 6) the observed Milky Way satellites appear to follow the overall dark matter distribution of Via Lactea, while the largest simulated subhalos today are found preferentially at larger radii; (7) subhalos have central densities that increase with Vmax and reach ρDM=0.1-0.3 M☉/pc3, comparable to the central densities inferred in dwarf spheroidals with core radii >250 pc.
Cosmology: Theory - Cosmology: Dark Matter - Galaxies: Dwarf - Galaxies: Formation - Galaxies: Halos - Methods: Numerical