in the reduced spectra are listed in Table \[tab:obslog\]. The observations were taken with a 1.31$''$ slit-width, the slit aligned to cover both the quasar and the candidate host with relative coordinates based on archival imaging. The observations were carried out with the 600RI and the 600z grisms, covering wavelength-ranges of $\lambda \lambda 5120-8450~\AA$ and $\lambda \lambda 7370-10700~\AA$ at a nominal spectral resolution $\mathcal{R}_\text{600RI} = 1000$ and $\mathcal{R}_\text{600z} = 1390$ assuming 1.0$''$ slit-widths, respectively [@Boffin2015]. For all the observations, we use a 2$\times$2 binning configuration along spatial and spectral directions.

We perform a cosmic-ray removal on the raw data frames with `P3D` [@Sandin2010], an adaptation of the `L.A.Cosmic` algorithm [@vanDokkum2001]. Each frame is subsequently reduced in a standard manner by passing it through the ESO/Reflex pipeline version 5.1.4 [@Freudling2013]. Individual exposures are combined into 2D spectra for each object using the average pixel value and a sigma-clipping rejection. In three cases (Q0153+0009, Q1209+107 PA1, and Q1436-0051), the pipeline did an unsatisfactory sky-subtraction, and we post-processed the intermediate Reflex products of those observations with standard `IRAF` tasks.

For each science-frame, the host-galaxy is flux-calibrated by extracting 1D-spectra of the quasar and target, scaling the quasar spectrum to its Sloan Digital Sky 