Dark matter inner slope and concentration in galaxies: from the Fornax
  dwarf to M87
  We apply two new state-of-the-art methods that model the distribution of
observed tracers in projected phase space to lift the mass / velocity
anisotropy (VA) degeneracy and deduce constraints on the mass profiles of
galaxies, as well as their VA. We first show how a distribution function based
method applied to the satellite kinematics of otherwise isolated SDSS galaxies
shows convincing observational evidence of age matching: red galaxies have more
concentrated dark matter (DM) halos than blue galaxies of the same stellar or
halo mass. Then, applying the MAMPOSSt technique to M87 (traced by its red and
blue globular clusters) we find that very cuspy DM is favored, unless we
release priors on DM concentration or stellar mass (leading to unconstrained
slope). For the Fornax dwarf spheroidal (traced by its metal-rich and
metal-poor stars), the inner DM slope is unconstrained, with weak evidence for
a core if the stellar mass is fixed. This highlights how priors are crucial for
DM modeling. Finally, we find that blue GCs around M87 and metal-rich stars in
Fornax have tangential outer VA.
