arXiv 2103.092452021-03astro-ph.GA

MOSDEF调查：质量-金属丰度关系和z~1.5处FMR的存在

The MOSDEF Survey: The Mass-Metallicity relationship and the existence of the FMR at z~1.5

Michael W. Topping, Alice E. Shapley, Ryan L. Sanders, Mariska Kriek, Naveen A. Reddy, Alison L. Coil, Bahram Mobasher, Brian Siana, William R. Freeman, Irene S… 展开作者

Michael W. Topping, Alice E. Shapley, Ryan L. Sanders, Mariska Kriek, Naveen A. Reddy, Alison L. Coil, Bahram Mobasher, Brian Siana, William R. Freeman, Irene Shivaei, Mojegan Azadi, Sedona H. Price, Gene C. K. Leung, Tara Fetherolf, Laura de Groot, Tom Zick, Francesca M. Fornasini, Guillermo Barro, Jordan N. Runco

备注：: 14 Pages, 9 figures, Accepted to MNRAS
DOI：: 10.1093/mnras/stab1793

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摘要：

分析了MOSFIRE深演化场巡天中z~1.5星系的静止-光学发射线比值。使用复合光谱，我们调查的质量金属丰度关系（MZR）在z~1.5，并测量其演变到z=0。当使用基于N2线比的气相金属丰度时，我们发现MZR从z~1.5到z=0的演化依赖于恒星质量，由$M_*<10^{9.75}M_{\odot}$处的$Δ\rm log(\rm O/H)\sim0.25$ dex演化到$M_*>10^{10.5}M_{\odot}$处的$Δ\rm log(\rm O/H)\sim0.05$。相比之下，基于O3 N2的MZR显示所有质量的$Δ\rm log(\rm O/H)\sim0.30$的恒定偏移，与先前基于独立金属丰度指标的MOSDEF结果一致，并表明O3 N2为我们的z~1.5样品提供了更稳健的金属丰度校准。我们通过测量平均$M_*$ -特异性SFR和$M_*-\log(\rm O3N2)$关系的相关离散度，研究了MZR对SFR的二级依赖性。我们发现了$\log(\rm O/H)$和sSFR偏移之间的反相关性，表明存在$M_*$-SFR-Z关系，尽管意义有限。此外，我们发现，我们的z~1.5堆栈位于沿z=0金属丰度序列在固定的$μ=\log(M_*/M_{\odot})-0.6\times\log(\rm SFR / M_{\odot} yr^{-1})$表明，z~1.5堆栈可以描述为z=0的基本金属丰度关系（FMR）。然而，使用不同的校准可以移动计算的金属丰度的本地FMR，表明适当的校准是必不可少的理解红移的金属丰度演化。最后，了解[NII]/H $α$如何与星系性质成比例，对于准确描述混合[NII]和H $α$对红移和H $α$通量测量的影响至关重要，这些测量将在未来利用低分辨率光谱进行大规模调查，如欧几里得和罗马太空望远镜。

英文摘要：

We analyze the rest-optical emission-line ratios of z~1.5 galaxies drawn from the MOSFIRE Deep Evolution Field (MOSDEF) survey. Using composite spectra we investigate the mass-metallicity relation (MZR) at z~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~1.5 to z=0 depends on stellar mass, evolving by $Δ\rm log(\rm O/H)\sim0.25$ dex at $M_*<10^{9.75}M_{\odot}$ down to $Δ\rm log(\rm O/H)\sim0.05$ at $M_*>10^{10.5}M_{\odot}$. In contrast, the O3N2-based MZR shows a constant offset of $Δ\rm log(\rm O/H)\sim0.30$ 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~1.5 sample. We investigated the secondary dependence of the MZR on SFR by measuring correlated scatter about the mean $M_*$-specific SFR and $M_*-\log(\rm O3N2)$ relations. We find an anti-correlation between $\log(\rm O/H)$ and sSFR offsets, indicating the presence of a $M_*$-SFR-Z relation, though with limited significance. Additionally, we find that our z~1.5 stacks lie along the z=0 metallicity sequence at fixed $μ=\log(M_*/M_{\odot})-0.6\times\log(\rm SFR / M_{\odot} yr^{-1})$ suggesting that the z~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$α$ scales with galaxy properties is crucial to accurately describe the effects of blended [NII] and H$α$ on redshift and H$α$ flux measurements in future large surveys utilizing low-resolution spectra such as with Euclid and the Roman Space Telescope.

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摘要：

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