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Absorption spectroscopy of gravitationally lensed quasars (GLQs) enablesstudy of spatial variations in the interstellar and/or circumgalactic medium offoreground galaxies. We report observations of 4 GLQs, each with two imagesseparated by 0.8-3.0", that show strong absorbers at redshifts0.4$<$$z_{abs}$$<$1.3 in their spectra, including some at the lens redshiftwith impact parameters 1.5-6.9 kpc. We measure H I Lyman lines along two sightlines each in five absorbers (10 sight lines in total) using HST STIS, andmetal lines using Magellan Echellette or Sloan Digital Sky Survey. Our datahave doubled the lens galaxy sample with measurements of H I column densities($N_{\rm H I}$) and metal abundances along multiple sight lines. Our data,combined with the literature, show no strong correlation between absolutevalues of differences in $N_{\rm H I}$, $N_{\rm Fe II}$, or [Fe/H] and thesight line separations at the absorber redshifts for separations of 0-8 kpc.The estimated abundance gradients show a tentative anti-correlation withabundances at galaxy centers. Some lens galaxies show inverted gradients,possibly suggesting central dilution by mergers or infall of metal-poor gas.[Fe/H] measurements and masses estimated from GLQ astrometry suggest the lensgalaxies lie below the total mass-metallicity relation for early-type galaxiesas well as measurements for quasar-galaxy pairs and gravitationally lensedgalaxies at comparable redshifts. This difference may arise in part from thedust depletion of Fe. Higher resolution measurements of H and metals(especially undepleted elements) for more GLQ absorbers and accurate lensredshifts are needed to confirm these trends.

Probing Structure in Cold Gas at $z \lesssim 1$ with Gravitationally Lensed Quasar Sight Lines