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We have used N-body simulations for the Milky Way to investigate thekinematic and structural properties of the old metal-poor stellar halo in thebarred inner region of the Galaxy. We find that the extrapolation of thedensity distribution for bulge RR Lyrae stars, $\rho\sim r^{-3}$, approximatelymatches the number density of RR Lyrae in the nearby stellar halo. We followthe evolution of such a tracer population through the formation and evolutionof the bar and box/peanut bulge in the N-body model. We find that its densitydistribution changes from oblate to triaxial, and that it acquires slowrotation 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 abarred shape, just $12\%$ of the orbits follow the bar, and it does not tracethe peanut/X structure. With these properties, the RR Lyrae population in theGalactic bulge is consistent with being the inward extension of the Galacticmetal-poor stellar halo.

The Stellar Halo in the Inner Milky Way: Predicted Shape and Kinematics