  The Besan\c{c}on Galaxy model was used to compare the infrared colour
distribution of synthetic stars with those from 2MASS observations taking the
selection function of the data into account, in order to study the shape of the
stellar halo of the Milky Way, with complemetary spectroscopic data from
SDSS-III/APOGEE survey. Furthermore, we compared the generated mock metallicity
distribution of the Besan\c{c}on Galaxy model, to the intrinsic metallicity
distribution with reliable stellar parameters from the APOGEE Stellar
Parameters and Chemical Abundances Pipeline (ASPCAP). The comparison was
carried accross a large volume of the inner part of the Galaxy, revealing that
a metal-poor population, [M/H]$<-1.2$ dex, could fill an extended component of
the inner galactic halo. With this data set, we are able to model a more
realistic mass density distribution of the stellar halo component of the Milky
Way, assuming a six-parameters double power-law model, and reconstruct the
behaviour of the rotation curve in the inner part of the Galaxy.
