The MOSDEF survey: the mass-metallicity relationship and the existence of the FMR at z ∼ 1.5

被引:20
作者
Topping, Michael W. [1 ,2 ]
Shapley, Alice E. [1 ]
Sanders, Ryan L. [3 ]
Kriek, Mariska [4 ]
Reddy, Naveen A. [5 ]
Coil, Alison L. [6 ]
Mobasher, Bahram [5 ]
Siana, Brian [5 ]
Freeman, William R. [5 ]
Shivaei, Irene [2 ]
Azadi, Mojegan [7 ]
Price, Sedona H. [8 ]
Leung, Gene C. K. [6 ]
Fetherolf, Tara [5 ]
de Groot, Laura [9 ]
Zick, Tom [4 ]
Fornasini, Francesca M. [7 ]
Barro, Guillermo [10 ]
Runco, Jordan N. [1 ]
机构
[1] Univ Calif Los Angeles, Dept Phys & Astron, 430 Portola Plaza, Los Angeles, CA 90095 USA
[2] Univ Arizona, Dept Astron, Steward Observ, 933N Cherry Ave, Tucson, AZ 85721 USA
[3] Univ Calif Davis, Dept Phys, One Shields Ave, Davis, CA 95616 USA
[4] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA
[5] Univ Calif Riverside, Dept Phys & Astron, 900 Univ Ave, Riverside, CA 92521 USA
[6] Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA
[7] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA
[8] Max Planck Inst Extraterr Phys, Postfach 1312, D-85741 Garching, Germany
[9] Coll Wooster, Dept Phys, 1189 Beall Ave, Wooster, OH 44691 USA
[10] Univ Pacific, Dept Phy, 3601 Pacific Ave, Stockton, CA 95211 USA
关键词
galaxies: evolution; galaxies: high-redshift; galaxies: ISM; STAR-FORMING GALAXIES; FMOS-COSMOS SURVEY; IONIZED-GAS; CHEMICAL-COMPOSITION; INTERSTELLAR-MEDIUM; STELLAR MASS; LRIS SURVEY; EVOLUTION; DUST; OUTFLOWS;
D O I
10.1093/mnras/stab1793
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We analyse the rest-optical emission-line ratios of z similar to 1.5 galaxies drawn from the Multi-Object Spectrometer for Infra-Red Exploration Deep Evolution Field (MOSDEF) survey. Using composite spectra, we investigate the mass-metallicity relation (MZR) at z similar to 1.5 and measure its evolution to z = 0. When using gas-phase metallicities based on the N2 line ratio, we find that the MZR evolution from z similar to 1.5 to z = 0 depends on stellar mass, evolving by Delta log(O/H) similar to 0.25 dex at M-* < 10(9.75) M-circle dot down to Delta log(O/H) similar to 0.05 at M-* greater than or similar to 10(10.5) M-circle dot. In contrast, the O3N2-based MZR shows a constant offset of Delta log(O/H) similar to 0.30 across all masses, consistent with previous MOSDEF results based on independent metallicity indicators, and suggesting that O3N2 provides a more robust metallicity calibration for our z similar to 1.5 sample. We investigated the secondary dependence of the MZR on star formation rate (SFR) by measuring correlated scatter about the mean M-*-specific SFR and M-*-log(O3N2) relations. We find an anticorrelation between log(O/H) and sSFR offsets, indicating the presence of a M-*-SFR-Z relation, though with limited significance. Additionally, we find that our z similar to 1.5 stacks lie along the z = 0 metallicity sequence at fixed mu = log(M-*/M-circle dot) - 0.6 x log(SFR/M-circle dot yr(-1)) suggesting that the z similar to 1.5 stacks can be described by the z = 0 fundamental metallicity relation (FMR). However, using different calibrations can shift the calculated metallicities off of the local FMR, indicating that appropriate calibrations are essential for understanding metallicity evolution with redshift. Finally, understanding how [NII]/H alpha scales with galaxy properties is crucial to accurately describe the effects of blended [NII] and H alpha on redshift and H alpha fiux measurements in future large surveys utilizing low-resolution spectra such as with Euclid and the Roman Space Telescope.
引用
收藏
页码:1237 / 1249
页数:13
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