arXiv 1507.030172015-07astro-ph.GA

MOSDEF巡天：利用z ~ 2处的H $α$和H $β$发射线研究恒星形成速率与恒星质量的关系

The MOSDEF Survey: Dissecting the star-formation rate vs. stellar mass relation using H$α$ and H$β$ emission lines at z ~ 2

Irene Shivaei, Naveen A. Reddy, Alice E. Shapley, Mariska Kriek, Brian Siana, Bahram Mobasher, Alison L. Coil, William R. Freeman, Ryan Sanders, Sedona H. Price… 展开作者

Irene Shivaei, Naveen A. Reddy, Alice E. Shapley, Mariska Kriek, Brian Siana, Bahram Mobasher, Alison L. Coil, William R. Freeman, Ryan Sanders, Sedona H. Price, Laura de Groot, Mojegan Azadi

备注：: 13 pages, 8 figures, 2 tables, ApJ accepted version
DOI：: 10.1088/0004-637X/815/2/98

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摘要：

我们提出了恒星形成率（SFR）与恒星质量（$M_*$）关系的结果（即，“主序星”）在恒星形成星系之间在1.37 $\leq$ $z$ $\leq$ 2.61使用MOSFIRE深演化场（MOSDEF）调查。基于261个星系的H $α$和H $β$光谱样本，我们在$M_*$（$\sim10^{9.5}-10^{11.5}M_\odot$）中估算了大范围的强尘埃校正瞬时SFR。我们发现log（SFR（H $α$））和log（$M_*$）之间的相关性，斜率为0.65 $\pm$ 0.08（0.58 $\pm$ 0.10），1.4<z<2.6（2.1<z<2.6）。我们发现，不同的假设的尘埃校正，如使用颜色过剩的恒星连续校正星云线，样本选择偏差对红色恒星形成星系，不占巴尔末吸收可以产生陡峭的斜率的日志（SFR）日志（$M_*$）的关系。我们的样品不受这些偏差的影响，因为它是静止帧光学选择的，H $α$和H $β$是针对巴尔末吸收校正的，H $α$光度是使用从巴尔末衰减计算的星云色过量进行尘埃校正的。在考虑测量不确定性之后，log（SFR（H $α$））-log（$M_*$）关系的分散度在2.1<z<2.6处为0.31 dex，其比log（SFR（UV））-log（$M_*$）中的分散度大0.05 dex。基于模拟的SFR- $M_*$关系与一些内在的散射的比较，我们认为，在没有直接测量的衰减/消光曲线和IMF的星系到星系的变化，不能使用的SFR（H $α$）和SFR（UV）- $M_*$关系的散射的差异，以限制在高红移星系的恒星形成的随机性。

英文摘要：

We present results on the star-formation rate (SFR) versus stellar mass ($M_*$) relation (i.e., the "main sequence") among star-forming galaxies at 1.37$\leq$$z$$\leq$2.61 using the MOSFIRE Deep Evolution Field (MOSDEF) survey. Based on a sample of 261 galaxies with H$α$ and H$β$ spectroscopy, we have estimated robust dust-corrected instantaneous SFRs over a large range in $M_*$ ($\sim10^{9.5}-10^{11.5}M_\odot$). We find a correlation between log(SFR(H$α$)) and log($M_*$) with a slope of 0.65$\pm$0.08 (0.58$\pm$0.10) at 1.4<z<2.6 (2.1<z<2.6). We find that different assumptions for the dust correction, such as using the color-excess of the stellar continuum to correct the nebular lines, sample selection biases against red star-forming galaxies, and not accounting for Balmer absorption can yield steeper slopes of the log(SFR)-log($M_*$) relation. Our sample is immune from these biases as it is rest-frame optically selected, H$α$ and H$β$ are corrected for Balmer absorption, and the H$α$ luminosity is dust-corrected using the nebular color-excess computed from the Balmer decrement. The scatter of the log(SFR(H$α$))-log($M_*$) relation, after accounting for the measurement uncertainties, is 0.31 dex at 2.1<z<2.6, which is 0.05 dex larger than the scatter in log(SFR(UV))-log($M_*$). Based on comparisons to a simulated SFR-$M_*$ relation with some intrinsic scatter, we argue that in the absence of direct measurements of galaxy-to-galaxy variations in the attenuation/extinction curves and the IMF, one cannot use the difference in the scatter of the SFR(H$α$)- and SFR(UV)-$M_*$ relations to constrain the stochasticity of star formation in high-redshift galaxies.

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