The ERO host galaxy of GRB 020127: Implications for the metallicity of GRB progenitors

We present optical and near-IR observations of the host galaxy of GRB 020127, for which we measure R - K-s = 6.2 mag. This is only the second GRB host to date classified as an ERO. The spectral energy distribution (SED) is typical of a dusty starburst galaxy, with a redshift z approximate to 1: 9, a luminosity L approximate to 5L(*), and an inferred stellar mass of M-* similar to 10(11)-10(12) M-circle dot, two orders of magnitude more massive than typical GRB hosts. A comparison to the z similar to 2 mass metallicity (MZ) relation suggests that the host metallicity is about 0.5-1Z(circle dot). This result shows that at least some GRBs occur in massive, metal-enriched galaxies, and that the proposed low-metallicity bias of GRB progenitors is not as severe as previously claimed. Instead, we propose that the blue colors and sub-L luminosities of most GRB hosts reflect their young starburst populations. This explanation also accounts for the prevalence of low-redshift GRBs in low-mass galaxies, since star formation activity shifts from high-to low-mass galaxies as a function of decreasing redshift ("downsizing''). Thus, the low-metallicity bias claimed for P 0.2 GRB hosts is likely a secondary effect, which reflects the M-Z relation, and consequently GRBs and their hosts may serve as a reliable tracer of cosmic star formation activity.