We calculate the stellar mass\u2013metallicity relation at five epochs ranging to z<\/i> \u223c 2.3. We quantify evolution in the shape of the mass\u2013metallicity relation as a function of redshift; the mass\u2013metallicity relation flattens at late times. There is an empirical upper limit to the gas-phase oxygen abundance in star-forming galaxies that is independent of redshift. From examination of the mass\u2013metallicity relation and its observed scatter, we show that the flattening at late times is a consequence of evolution in the stellar mass where galaxies enrich to this empirical upper metallicity limit; there is also evolution in the fraction of galaxies at a fixed stellar mass that enrich to this limit. The stellar mass where metallicities begin to saturate is \u223c0.7\u00a0dex smaller in the local universe than it is at z<\/i> \u223c 0.8.<\/p>\n","protected":false},"excerpt":{"rendered":"
We calculate the stellar mass\u2013metallicity relation at five epochs ranging to z \u223c 2.3. We quantify evolution in the shape of the mass\u2013metallicity relation as a function of redshift; the mass\u2013metallicity relation flattens at late times. There is an empirical upper limit to the gas-phase oxygen abundance in star-forming galaxies that is independent of redshift. 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