Properties of Galactic Dark Matter: Constraints from Astronomical
  Observations
  The distributions of normal matter and of dark matter in the Galaxy are
coupled to each other as they both move in the common gravitational potential.
In order to fully exploit this interplay and to derive the various properties
of dark matter relevant to their direct and indirect detection, we have
comprehensively reviewed the astronomical observations of the spatial and
velocity distributions of the components of normal matter. We then postulate
that the phase-space distribution of dark matter follows a lowered-isothermal
form and self-consistently solve Poisson's equation to construct several models
for the spatial and velocity distributions of dark matter. In this paper, we
compute the total gravitational potential of the normal and dark matter
components and investigate their consistency with current observations of the
rotation curve of the Galaxy and of the spatial and velocity distributions of
blue horizontal-branch and blue straggler stars. Even with this demand of
consistency, a large number of models with a range of parameters characterizing
the dark matter distribution remain. We find the best choice of parameters,
within the range of allowed values, for the surface density of the disk 55
M$_\odot$ pc$^{-2}$, are the following: the dark matter density at the Galactic
center $\rho_{DM,c}\approx 100-250$ GeV cm$^{-3}$, the local dark matter
density $\rho_{DM}(R_0) \approx 0.56-0.72$ GeV cm$^{-3}$, and the
root-mean-speed of dark matter particles $< v_{DM}^{2}(R_0)>
^{1/2}\approx490-550$ km s$^{-1}$. We also discuss possible astronomical
observations that may further limit the range of the allowed models.
