  Using the STOKES Monte Carlo radiative transfer code we revisit the
predictions of the spectropolarimetric signal from a disc-like Broad Emission
Line Region (BLR) in Type I AGN due to equatorial scattering. We reproduce the
findings of previous works, but only for a scatterer which is much more
optically and geometrically thick than previously proposed. We also find that
when taking into account the polarized emission from all regions of the
scatterer, the swing of the Polarizarion Angle (PA) is in the opposite
direction to that originally proposed. Furthermore, we find that the presence
of outflows in the scattering media can significantly change the observed line
profiles, with the PA of the scattering signal being enhanced in the presence
of radially outflowing winds. Finally, a characteristically different PA
profile, shaped like an `M', is seen when the scatterer is cospatial with the
BLR and radially outflowing.
