Velocity dispersion of the PBH DM. The solid curves show our estimate from the Jeans equation. Three cases are shown: the Galaxy consisting only of (i) NFW DM halo, (ii) NFW DM halo + baryonic bulge, and (iii) Einasto DM halo + baryonic bulge. The triangles and squares denote the DM velocity dispersions taken from Ferrer & Hunter (2013). Neglecting the baryonic disk leads to a ∼25% underestimation of the DM velocity dispersion, i.e. a factor of ∼3 overestimation of the accreting PBH luminosity. Replacing NFW with the Einasto density profile leads to a factor of ∼1.5 increase in the velocity dispersion in the very central parts. The light gray shaded region shows an approximate extent of the CMZ.