The MOSDEF Survey: The Evolution of the Mass-Metallicity Relation from $z=0$ to $z\sim3.3$.
The MOSDEF Survey: The Evolution of the Mass-Metallicity Relation from $z=0$ to $z\sim3.3$.
复制标题
DOI：
10.3847/1538-4357/abf4c1
复制
发表时间：
2020-09
期刊：
影响因子：
--
通讯作者：
R. Sanders;A. Shapley;Tucker Jones;N. Reddy;M. Kriek;B. Siana;A. Coil;B. Mobasher;I. Shivaei;Romeel Dave;Mojegan Azadi;S. Price;G. Leung;W. Freeman;T. Fetherolf;L. D. Groot;T. Zick;Guillermo Barro
中科院分区：
文献类型：
--
作者：
R. Sanders;A. Shapley;Tucker Jones;N. Reddy;M. Kriek;B. Siana;A. Coil;B. Mobasher;I. Shivaei;Romeel Dave;Mojegan Azadi;S. Price;G. Leung;W. Freeman;T. Fetherolf;L. D. Groot;T. Zick;Guillermo Barro
我们调查星系气相金属丰度（O/H）的演变范围为$z = 0 - 3.3 $使用的样本$\sim300 $星系在$z\sim2.3 $和$\sim150 $星系在$z\sim3.3 $从MOSDEF调查。该分析至关重要地利用在$z\sim0 $和$z> 1 $处的不同金属丰度校准来解释不断变化的ISM条件。我们发现O/H和恒星质量（$M_*$）在$z\sim2.3 $和$z\sim3.3 $处有显著的相关性。质量-金属丰度关系的低质量幂律斜率在z = 0 - 3.3 $范围内是显著不变的，使得在此范围内的所有红移处，$\textrm {O/H}\propto M_*^{0.30}$。在固定M * 时，O/H随红移的增加而减小：dlog（O/H）/d $z =-0.11\pm0.02$.我们没有发现M *$、O/H和恒星形成率（SFR）之间的基本金属丰度关系演化到z3.3的证据，其中z2.3 - 3.3的星系的O/H在M *$和SFR平均匹配的本星系的0.04倍之内。我们采用分析化学演化模型的银河系外流的质量和金属负载因子的限制。在固定的红移下，金属去除效率随着M *$的减小而增大;在固定的M *$下，金属去除效率随着M *$的增大而增大。这些模型表明，质量-金属丰度关系的斜率是由流出物的金属负载因子与M *$的比例关系决定的，而不是由气体分数随M *$的变化决定的。随着红移的增加，在固定的$M_*$下向较低的O/H的演化是由较高的气体分数（导致ISM金属的较强稀释）和较高的金属去除效率驱动的，模型表明这两种效应对所观察到的演化的贡献大致相等。这些结果表明，至少在过去的12~Gyr中，通过气体流动和星星形成控制星系的平稳重子生长的过程保持相同的形式。
We investigate the evolution of galaxy gas-phase metallicity (O/H) over the range $z=0-3.3$ using samples of $\sim300$ galaxies at $z\sim2.3$ and $\sim150$ galaxies at $z\sim3.3$ from the MOSDEF survey. This analysis crucially utilizes different metallicity calibrations at $z\sim0$ and $z>1$ to account for evolving ISM conditions. We find significant correlations between O/H and stellar mass ($M_*$) at $z\sim2.3$ and $z\sim3.3$. The low-mass power law slope of the mass-metallicity relation is remarkably invariant over $z=0-3.3$, such that $\textrm{O/H}\propto M_*^{0.30}$ at all redshifts in this range. At fixed $M_*$, O/H decreases with increasing redshift as dlog(O/H)/d$z=-0.11\pm0.02$. We find no evidence that the fundamental metallicity relation between $M_*$, O/H, and star-formation rate (SFR) evolves out to $z\sim3.3$, with galaxies at $z\sim2.3-3.3$ having O/H within 0.04~dex of local galaxies matched in $M_*$ and SFR on average. We employ analytic chemical evolution models to place constraints on the mass and metal loading factors of galactic outflows. The efficiency of metal removal increases toward lower $M_*$ at fixed redshift, and toward higher redshift at fixed $M_*$. These models suggest that the slope of the mass-metallicity relation is set by the scaling of the metal loading factor of outflows with $M_*$, not by the change in gas fraction as a function of $M_*$. The evolution toward lower O/H at fixed $M_*$ with increasing redshift is driven by both higher gas fraction (leading to stronger dilution of ISM metals) and higher metal removal efficiency, with models suggesting that both effects contribute approximately equally to the observed evolution. These results suggest that the processes governing the smooth baryonic growth of galaxies via gas flows and star formation hold in the same form over at least the past 12~Gyr.