  I review the properties of degenerate fermion balls and investigate the dark
matter distribution at galactic centers using NFW, Moore and isothermal density
profiles. I show that dark matter becomes degenerate for particles masses of a
few keV at distances less than a few parsec from the center of our galaxy. To
explain the galactic center black hole of mass of $\sim 3.5 \times
10^{6}M_{\odot}$ and a supermassive black hole of $\sim 3 \times
10^{9}M_{\odot}$ at a redshift of 6.41 in SDSS quasars, the mass of the fermion
ball is assumed to be between $3 \times 10^{3} M_{\odot}$ and $3.5 \times
10^{6}M_{\odot}$. This constrains the mass of the dark matter particle between
$0.6 {\rm keV}$ and $82 {\rm keV}$. The lower limit on the dark matter mass is
improved to about {\rm 6 keV} if exact solutions of Poisson's equation are used
in the isothermal power law case. The constrained dark matter particle could be
interpreted as a sterile neutrino.
