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We present a statistically robust mass-metallicity (M-Z) relation forlong-duration gamma-ray burst (LGRB) host galaxies at z < 1. By comparing theLGRB host M-Z relation to samples representative of the general star-forminggalaxy population, we conclude that LGRBs occur in host galaxies with lowermetallicities than the general population, and that this trend extends to z ~1, with an average offset of -0.42 +/- 0.18 from the M-Z relation forstar-forming galaxies. Our sample in this work includes new spectroscopic datafor 6 LGRB host galaxies obtained at the Keck and Magellan telescopes, as wellas 2 new host galaxies from the literature. Combined with data from ourprevious work, this yields a total sample of 6 LGRB host galaxies at z < 0.3and 10 host galaxies at 0.3 < z < 1. We have determined a number ofinterstellar medium properties for our host galaxies using opticalemission-line diagnostics, including metallicity, ionization parameter, youngstellar population age, and star formation rate. Across our full sample of 16LGRB hosts we find an average metallicity of log(O/H) + 12 = 8.4 +/- 0.3.Notably, we also measure a comparatively high metallicity of log(O/H) + 12 =8.83 +/- 0.1 for the z = 0.296 host galaxy of GRB 050826. We also determinestellar masses (M*) for our LGRB host galaxy sample, finding a mean stellarmass of log(M*/Msun) = 9.25 (+0.19,-0.23).

The Host Galaxies of Gamma-Ray Bursts II: A Mass-Metallicity Relation for Long-Duration Gamma-Ray Burst Host Galaxies