  We analyse the positions of RR Lyrae stars in the central region of the Milky
Way. In addition to the overall bar shape detected previously, we find evidence
for a peanut shaped structure, in form of overdensities near $\ell=-2$ deg and
$1$ deg at $b\sim-3.5$ deg. The corresponding physical distance between the two
peaks of the peanut is $\sim0.7$ kpc, significantly shorter than that found
from near-IR images (3.3 kpc) and red-clump stars. Qualitatively this is
expected from `fractionation' of bar orbits, which we demonstrate to be matched
in a simulation of an inside-out growing disc subsequently forming a bar.
