REST-UV ABSORPTION LINES AS METALLICITY ESTIMATOR: THE METAL CONTENT OF STAR-FORMING GALAXIES AT z similar to 5
Résumé
We measure a relation between the depth of four prominent rest-UV absorption complexes and metallicity for local galaxies and verify it up to z similar to 3. We then apply this relation to a sample of 224 galaxies at 3.5 \textless z \textless 6.0 (\textless z \textgreater = 4.8) in the Cosmic Evolution Survey (COSMOS), for which unique UV spectra from the Deep Imaging Multi-object Spectrograph (DEIMOS) and accurate stellar masses from the Spitzer Large Area Survey with HyperSuprime-Cam (SPLASH) are available. The average galaxy population at z similar to 5 and log(M / M-circle dot) \textgreater 9 is characterized by 0.3-0.4 dex (in units of 12 + log(O / H)) lower metallicities than at z similar to 2, but comparable to z similar to 3.5. We find galaxies with weak or no Ly alpha emission to have metallicities comparable to z similar to 2 galaxies and therefore may represent an evolved subpopulation of z similar to 5 galaxies. We find a correlation between metallicity and dust in good agreement with local galaxies and an inverse trend between metallicity and star-formation rate consistent with observations at z similar to 2. The relation between stellar mass and metallicity (MZ relation) is similar to z similar to 3.5, but there are indications of it being slightly shallower, in particular for the young, Ly alpha-emitting galaxies. We show that, within a “bathtub” approach, a shallower MZ relation is expected in the case of a fast (exponential) build-up of stellar mass with an e-folding time of 100-200 Myr. Because of this fast evolution, the process of dust production and metal enrichment as a function of mass could be more stochastic in the first billion years of galaxy formation compared to later times.