Abstract X-ray polarimetric missions planned for this decade will significantly enhance our knowledge of compact accreting sources. Observations of the X-ray polarisation signal from Active Galactic Nuclei (AGN) or X-ray binary systems (XRBs) will bring new means to study inner accretion flow in these objects that, together with currently used spectroscopic and timing techniques, will help us to determine better their properties, such as their inclination, orientation, shape and size of their corona as well as the black hole spin. In this work we present a yet missing piece in the global polarisation models of black hole accretion discs. We compute the reflected X-ray emission from the disc in a local co-moving frame using 1) the radiative transfer code TITAN to obtain the ionization structure of the disc and 2) the Monte Carlo code STOKES that incorporates the physics of absorption, re-emission and Compton scattering to produce a complete spectro-polarimetric output. We present the final Stokes parameters I, Q and U for a set of photon-indices of the incident primary power-law radiation, the disc ionization parameters, incident and emission angles, for three independent polarisation states of the incident coronal X-ray photons with a sufficient resolution in energy to allow for sharp discussion of spectral and polarisation properties. We show that the spectral component matches well literature predictions. The polarisation degree and angle are in agreement with analytical approximations previously appearing in reflection models and we demonstrate that the polarized reflected X-ray emission can be, locally, quite large in the 2 − 12 keV band.