The Mass–Metallicity Relation at z ∼ 1–2 and Its Dependence on the Star Formation Rate-猫眼课题宝

DOI：

10.3847/1538-4357/ac1105

发表时间：

2021-07

期刊：

The Astrophysical Journal

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

A. Henry;M. Rafelski;B. Sunnquist;N. Pirzkal;C. Pacifici;H. Atek;M. Bagley;I. Baronchelli;G. Barro;A. Bunker;J. Colbert;Y. Dai;B. Elmegreen;D. Elmegreen;S. Finkelstein;D. Kocevski;A. Koekemoer;M. Malkan;C. Martin;V. Mehta;A. Pahl;C. Papovich;M. Rutkowski;J. Sánchez Almeida;C. Scarlata;G. Snyder;H. Teplitz

我们提出了一个新的测量气相质量金属丰度关系（MZR）和它的依赖于星星形成率（SFR）在1.3 < z < 2.3。我们的样本包括1056个星系，平均红移z = 1.9，从哈勃空间望远镜宽视场相机3（WFC 3）的棱镜光谱在宇宙大会近红外深河外巡天和WFC 3红外光谱平行调查。这个样本比以前在z 102的金属丰度调查大四倍，恒星质量（108 M）低一个数量级。使用堆叠的光谱，我们发现，MZR的发展由0.3 dex相对于z = 0.1。此外，我们确定了一个49个星系的子集，具有高信噪比（S/N）光谱和红移在1.3 < z < 1.5之间，其中Hα发射与[O iii]和[O ii]沿着观察。在这些对象中的SFR的精确测量，我们确认存在的质量金属丰度SFR（M-Z-SFR）的关系在高红移。这些星系表现出系统的差异，从本地的M-Z-SFR关系，这取决于所采用的本地关系的测量。然而，仍然很难确定这些差异是否可能是由于红移的演变，因为本地M-Z-SFR关系在我们的样品的质量和SFR的约束很差。最后，我们在IllustrisTNG流体动力学模拟中再现了我们的样本选择，表明我们的线通量限制将模拟MZR的归一化降低了0.2 dex。我们表明，M-Z-SFR关系在IllustrisTNG有一个SFR的依赖性，是太陡峭的约3倍。

We present a new measurement of the gas-phase mass–metallicity relation (MZR) and its dependence on star formation rates (SFRs) at 1.3 < z < 2.3. Our sample comprises 1056 galaxies with a mean redshift of z = 1.9, identified from the Hubble Space Telescope Wide Field Camera 3 (WFC3) grism spectroscopy in the Cosmic Assembly Near-infrared Deep Extragalactic Survey and the WFC3 Infrared Spectroscopic Parallel Survey. This sample is four times larger than previous metallicity surveys at z ∼ 2 and reaches an order of magnitude lower in stellar mass (108 M ⊙). Using stacked spectra, we find that the MZR evolves by 0.3 dex relative to z ∼ 0.1. Additionally, we identify a subset of 49 galaxies with high signal-to-noise (S/N) spectra and redshifts between 1.3 < z < 1.5, where Hα emission is observed along with [O iii] and [O ii]. With accurate measurements of SFR in these objects, we confirm the existence of a mass–metallicity–SFR (M–Z–SFR) relation at high redshifts. These galaxies show systematic differences from the local M–Z–SFR relation, which vary depending on the adopted measurement of the local relation. However, it remains difficult to ascertain whether these differences could be due to redshift evolution, as the local M–Z–SFR relation is poorly constrained at the masses and SFRs of our sample. Lastly, we reproduced our sample selection in the IllustrisTNG hydrodynamical simulation, demonstrating that our line flux limit lowers the normalization of the simulated MZR by 0.2 dex. We show that the M–Z–SFR relation in IllustrisTNG has an SFR dependence that is too steep by a factor of around 3.

The Mass–Metallicity Relation at z ∼ 1–2 and Its Dependence on the Star Formation Rate

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