Abstract
ABSTRACT We explore the evolution of the Stellar Mass–Star Formation Rate (SFR)–Metallicity relation using a set of 256 COSMOS and GOODS galaxies in the redshift range 1.90 < z < 2.35. We present the galaxies’ rest-frame optical emission-line fluxes derived from IR-grism spectroscopy with the Hubble Space Telescope and combine these data with SFRs and stellar masses obtained from deep, multi-wavelength (rest-frame UV to IR) photometry. We then compare these measurements to those for a local sample of galaxies carefully matched in stellar mass ( 7.5 ≲ log ( M * / M ⊙ ) ≲ 10.5 ?> ) and SFR ( − 0.5 ≲ log ( SFR ) ≲ 2.5 ?> in M ⊙ yr−1). We find that the distribution of z ∼ 2.1 galaxies in stellar mass–SFR–metallicity space is clearly different from that derived for our sample of similarly bright ( L H β > 3 × 10 40 ?> erg s−1) local galaxies, and this offset cannot be explained by simple systematic offsets in the derived quantities. At stellar masses above ∼ 10 9 M ⊙ ?> and SFRs above ∼ 10 M ⊙ ?> yr−1, the z ∼ 2.1 galaxies have higher oxygen abundances than their local counterparts, while the opposite is true for lower-mass, lower-SFR systems.
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