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 \sim 15 - 25 km/s at |l| = 10 ^ { \circ } -30 ^ { \circ } , and the velocity dispersion is \sim 120 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 .