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

被引：31

作者：

Henry, Alaina ^{[1
,2
]}

Rafelski, Marc ^{[1
,2
]}

Sunnquist, Ben ^{[1
]}

Pirzkal, Norbert ^{[1
]}

Pacifici, Camilla ^{[1
]}

Atek, Hakim ^{[3
]}

Bagley, Micaela ^{[4
]}

Baronchelli, Ivano ^{[5
]}

Barro, Guillermo ^{[6
]}

Bunker, Andrew J. ^{[7
,8
]}

Colbert, James ^{[9
]}

Dai, Y. Sophia ^{[10
]}

Elmegreen, Bruce G. ^{[11
]}

Elmegreen, Debra Meloy ^{[12
]}

Finkelstein, Steven ^{[4
]}

Kocevski, Dale ^{[13
]}

Koekemoer, Anton ^{[1
]}

Malkan, Matthew ^{[14
]}

Martin, Crystal L. ^{[15
]}

Mehta, Vihang ^{[16
]}

Pahl, Anthony ^{[14
]}

Papovich, Casey ^{[17
]}

Rutkowski, Michael ^{[18
]}

Sanchez Almeida, Jorge ^{[19
]}

Scarlata, Claudia ^{[16
]}

Snyder, Gregory ^{[1
]}

Teplitz, Harry ^{[9
]}

机构：

[1] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA

[2] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[3] Sorbonne Univ, CNRS, Inst Astrophys Paris, UMR7095, 98bis Blvd Arago, F-75014 Paris, France

[4] Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA

[5] Univ Padua, Dipartmento Fis & Astron, Vicolo Osservatorio 1-3, I-31522 Padua, Italy

[6] Univ Pacific, Dept Phys, 3601 Pacific Ave, Stockton, CA 95211 USA

[7] Univ Oxford, Dept Phys, Subdept Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England

[8] Univ Tokyo, Univ Tokyo Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan

[9] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA

[10] Chinese Acad Sci, South Amer Ctr Astron CASSACA, NAOC, 20A Datun Rd, Beijing 100101, Peoples R China

[11] TJ Watson Res Ctr, IBM Res Div, 1101 Kitchawan Rd, Yorktown Hts, NY 10598 USA

[12] Vassar Coll, Dept Phys & Astron, Poughkeepsie, NY 12604 USA

[13] Colby Coll, Dept Phys & Astron, Waterville, ME 04901 USA

[14] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA

[15] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA

[16] Univ Minnesota, Minnesota Inst Astrophys, 116 Church St SE, Minneapolis, MN 55455 USA

[17] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA

[18] Minnesota State Univ, Dept Phys & Astron, Mankato, MN 56001 USA

[19] Inst Astrofis Canarias, E-38200 Tenerife, Spain

来源：

ASTROPHYSICAL JOURNAL | 2021年 / 919卷 / 02期

基金：

欧洲研究理事会; 国家重点研发计划;

关键词：

EXTRAGALACTIC HII-REGIONS; GAS-PHASE METALLICITY; STELLAR MASS; ILLUSTRISTNG SIMULATIONS; FORMING GALAXIES; OXYGEN ABUNDANCE; MOSDEF SURVEY; FUNDAMENTAL RELATION; CHEMICAL ENRICHMENT; FORMATION HISTORIES;

D O I：

10.3847/1538-4357/ac1105

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 similar to 2 and reaches an order of magnitude lower in stellar mass (10(8) M (circle dot)). Using stacked spectra, we find that the MZR evolves by 0.3 dex relative to z similar to 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 H alpha 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.

引用

页数：29

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