%0 Generic %1 ly2016metal %A Ly, Chun %A Malkan, Matthew A. %A Rigby, Jane %A Nagao, Tohru %D 2016 %K evolution mass metallicity relation %T The Metal Abundance across Cosmic Time ($MACT$) Survey II: Evolution of the Mass-Metallicity Relation over 8 Billion Years, using OIII$łambda$4363\AA-based Metallicities %U http://arxiv.org/abs/1602.01098 %X Abridged We present the results of MMT and Keck spectroscopy for a large sample of $0.1złeq1$ emission-line galaxies selected from our narrow-band imaging in the Subaru Deep Field. In total, we have measured the weak OIII$łambda$4363 line for 164 galaxies (66 with at least 3$\sigma$ detections, and 98 with significant upper limits). The strength of this nebular emission line is set by the electron temperature ($T_e$) for the ionized gas in these galaxies. Since the gas temperature is regulated by the metal content, an inverse relationship exists between gas-phase oxygen abundance and OIII$łambda$4363 line strength. Our $T_e$-based metallicity study is the first to span $\approx$8 Gyr of cosmic time and $\approx$3 dex in stellar mass for low-mass galaxies, $(M_star/M_sun)\approx6.0-9.0$. Combined with extensive multi-wavelength photometry, we investigate the evolution of the stellar mass--gas metallicity relation, and its dependence on dust-corrected star formation rate. The latter is obtained from high signal-to-noise Balmer emission-line measurements. Our mass-metallicity relation is consistent with Andrews & Martini at $złeq0.3$, and evolves toward lower abundances at a given stellar mass, $\propto(1+z)^-2.32^+0.53_-0.35$. We find that galaxies with lower metallicities have higher star formation rates at a given stellar mass and redshift, although the scatter is large ($\approx$0.3 dex) and the trend is weaker than seen in local studies. We also compare our mass--metallicity relation against predictions from high-resolution galaxy formation simulations and find good agreement with models that adopt energy and momentum stellar feedback. In addition, we have identified 16 extremely metal-poor galaxies with abundances less than a tenth of solar; our most metal-poor galaxy at $z\approx0.85$ has an oxygen abundance that is similar to I Zw 18.

@misc{ly2016metal, abstract = {[Abridged] We present the results of MMT and Keck spectroscopy for a large sample of $0.1\leq z\leq1$ emission-line galaxies selected from our narrow-band imaging in the Subaru Deep Field. In total, we have measured the weak [OIII]$\lambda$4363 line for 164 galaxies (66 with at least 3$\sigma$ detections, and 98 with significant upper limits). The strength of this nebular emission line is set by the electron temperature ($T_e$) for the ionized gas in these galaxies. Since the gas temperature is regulated by the metal content, an inverse relationship exists between gas-phase oxygen abundance and [OIII]$\lambda$4363 line strength. Our $T_e$-based metallicity study is the first to span $\approx$8 Gyr of cosmic time and $\approx$3 dex in stellar mass for low-mass galaxies, $\log{(M_{star}/M_{sun})}\approx6.0-9.0$. Combined with extensive multi-wavelength photometry, we investigate the evolution of the stellar mass--gas metallicity relation, and its dependence on dust-corrected star formation rate. The latter is obtained from high signal-to-noise Balmer emission-line measurements. Our mass-metallicity relation is consistent with Andrews & Martini at $z\leq0.3$, and evolves toward lower abundances at a given stellar mass, $\propto(1+z)^{-2.32^{+0.53}_{-0.35}}$. We find that galaxies with lower metallicities have higher star formation rates at a given stellar mass and redshift, although the scatter is large ($\approx$0.3 dex) and the trend is weaker than seen in local studies. We also compare our mass--metallicity relation against predictions from high-resolution galaxy formation simulations and find good agreement with models that adopt energy and momentum stellar feedback. In addition, we have identified 16 extremely metal-poor galaxies with abundances less than a tenth of solar; our most metal-poor galaxy at $z\approx0.85$ has an oxygen abundance that is similar to I Zw 18.}, added-at = {2016-02-04T09:54:07.000+0100}, author = {Ly, Chun and Malkan, Matthew A. and Rigby, Jane and Nagao, Tohru}, biburl = {https://www.bibsonomy.org/bibtex/213dec9e335329e21ce055d4c08a0c728/miki}, description = {[1602.01098] The Metal Abundance across Cosmic Time ($\mathcal{MACT}$) Survey II: Evolution of the Mass-Metallicity Relation over 8 Billion Years, using [OIII]$\lambda$4363\AA-based Metallicities}, interhash = {b03922a5f82de88397857784e2553f53}, intrahash = {13dec9e335329e21ce055d4c08a0c728}, keywords = {evolution mass metallicity relation}, note = {cite arxiv:1602.01098Comment: 17 pages, 11 figures, 2 tables. Submitted to ApJ on Feb 1, 2016. Paper presents first results on the evolution of the stellar mass--gas metallicity relation. The description of the survey and dataset is available in Paper I (Ly et al. ApJS, submitted). Key figures are # 4 & 5 (M-Z evolution), 7-9 (M-Z-SFR relation), and 11 (comparison with theory). Comments welcome}, timestamp = {2016-02-04T09:54:07.000+0100}, title = {The Metal Abundance across Cosmic Time ($\mathcal{MACT}$) Survey II: Evolution of the Mass-Metallicity Relation over 8 Billion Years, using [OIII]$\lambda$4363\AA-based Metallicities}, url = {http://arxiv.org/abs/1602.01098}, year = 2016 }