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Context. Absorbing galaxies are selected via the detection of characteristicabsorption lines which their gas-rich media imprint in the spectra of distantlight-beacons. The proximity of the typically faint foreground absorbinggalaxies to bright background sources makes it challenging to robustly identifythese in emission, and hence to characterise their relation to the generalgalaxy population. Aims. We search for emission to confirm and characterise tengalaxies hosting damped, metal-rich quasar absorbers at redshift z < 1.Methods. We identify the absorbing galaxies by matching spectroscopicabsorption -and emission redshifts and from projected separations. Combiningemission-line diagnostics with existing absorption spectroscopy and photometryof quasar-fields hosting metal-rich, damped absorbers, we compare our newdetections with reference samples and place them on scaling relations. Results.We spectroscopically confirm seven galaxies harbouring damped absorbers (a 70%success-rate). Our results conform to the emerging picture that neutral gas onscales of tens of kpc in galaxies is what causes the characteristic Hiabsorption. Our key results are: (I) Absorbing galaxies with $\log _{10}[M_\star ~(M_\odot)] \gtrsim 10$ have star formation rates that are lower thanpredicted for the main sequence of star formation. (II) The distribution ofimpact parameter with Hi column density and with absorption-metallicity forabsorbing galaxies at $z\sim 2-3$ extends to $z\sim 0.7$ and to lower Hi columndensities. (III) A robust mean metallicity gradient of $\langle \Gamma \rangle= 0.022 \pm 0.001~[dex~kpc^{-1}]$. (IV) By correcting absorption metallicitiesfor $\langle \Gamma \rangle$ and imposing a truncation-radius at$12~\mathrm{kpc}$, absorbing galaxies fall on top of predicted mass-metallicityrelations, with a statistically significant decrease in scatter.

Stellar masses, metallicity gradients and suppressed star formation revealed in a new sample of absorption selected galaxies