Dwarf galaxy annihilation and decay emission profiles for dark matter
  experiments
  Gamma-ray searches for dark matter annihilation and decay in dwarf galaxies
rely on an understanding of the dark matter density profiles of these systems.
Conversely, uncertainties in these density profiles propagate into the derived
particle physics limits as systematic errors. In this paper we quantify the
expected dark matter signal from 20 Milky Way dwarfs using a uniform analysis
of the most recent stellar-kinematic data available. Assuming that the observed
stellar populations are equilibrium tracers of spherically-symmetric
gravitational potentials that are dominated by dark matter, we find that
current stellar-kinematic data can predict the amplitudes of annihilation
signals to within a factor of a few for the ultra-faint dwarfs of greatest
interest. On the other hand, the expected signal from several classical dwarfs
(with high-quality observations of large numbers of member stars) can be
localized to the ~20% level. These results are important for designing
maximally sensitive searches in current and future experiments using space and
ground-based instruments.
