The Stellar Halo in the Inner Milky Way: Predicted Shape and Kinematics
  We have used N-body simulations for the Milky Way to investigate the
kinematic and structural properties of the old metal-poor stellar halo in the
barred inner region of the Galaxy. We find that the extrapolation of the
density distribution for bulge RR Lyrae stars, $\rho\sim r^{-3}$, approximately
matches the number density of RR Lyrae in the nearby stellar halo. We follow
the evolution of such a tracer population through the formation and evolution
of the bar and box/peanut bulge in the N-body model. We find that its density
distribution changes from oblate to triaxial, and that it acquires slow
rotation in agreement with recent measurements. The maximum radial velocity is
$\sim15-25$ km/s at $| l|\!=10^\circ-30^\circ$, and the velocity dispersion is
$\sim120$ km/s. Even though the simulated metal-poor halo in the bulge has a
barred shape, just $12\%$ of the orbits follow the bar, and it does not trace
the peanut/X structure. With these properties, the RR Lyrae population in the
Galactic bulge is consistent with being the inward extension of the Galactic
metal-poor stellar halo.
