to within sub-pixel precision. We then assume that the PSF profile does not vary with wavelength and that the quasar continuum emission can be modelled as a pure power-law across the covered wavelength range. This is used to scale the strength of the modelled quasar PSF in each wavelength, which can then be subtracted from the 2D-spectrum.

In eight out of ten targeted systems we identify the absorbing galaxy from emission lines at the expected wavelengths (see Table \[tab:line-fluxes\]). In six of these systems the detection of emission lines is possible in the science frames without performing SPSF subtraction. This allows us to measure line-fluxes directly without the addition of noise. In passing, we note that the SPSF-subtracted spectrum of Q1209+107 PA2 does not reveal hidden emission lines from an object at small impact parameter. Instead, we confirm the detection of emission lines at $z=0.3922$ in the object first reported by [@Cristiani87] which then remains the best candidate in that field. Two additional objects are identified as the absorbing galaxies after performing SPSF subtraction (Q1323-0021 and Q2328+0022, see Figure \[fig:SPSFsub\]). For these two systems, we vary the size and limits of the wavelength windows to see if the residual flux 