arXiv 1809.040992018-09-11astro-ph.GA

SFR-M $_*$关联扩展到高红移的低质量

The SFR-M$_*$ Correlation Extends to Low Mass at High Redshift

Kartheik G. Iyer, Eric Gawiser, Romeel Davé, Philip Davis, Steven L. Finkelstein, Dritan Kodra, Anton M. Koekemoer, Peter Kurczynski, Jeffery A. Newman, Camilla… 展开作者

Kartheik G. Iyer, Eric Gawiser, Romeel Davé, Philip Davis, Steven L. Finkelstein, Dritan Kodra, Anton M. Koekemoer, Peter Kurczynski, Jeffery A. Newman, Camilla Pacifici, Rachel Somerville

备注：: 22 pages, 10 figures. Accepted for publication in ApJ
DOI：: 10.3847/1538-4357/aae0fa

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摘要：

为了更全面地了解星系演化，SED拟合可以用来恢复恒星质量（M $_*$）和恒星形成率（SFR）之外的量。我们使用通过Iyer \& Gawiser（2017）的致密基方法重建的恒星形成历史（SFHS），用于Candels GOODS-S场中$0.5<z<6$的$17,873$星系样本，以研究SFR-M $_*$相关性的性质和演化。重建的SFHS代表SFR-M $_*$空间中的轨迹，使我们能够研究星系的时代早于观察到的传播他们沿着这些轨迹向后的时间。我们研究了SFR-M $_*$关联在$z=1,2,3,4,5,6$使用直接拟合星系在这些时期和SFR-M $_*$轨道的星系在较低的红移观察。通过KS检验，发现使用这两种方法获得的SFR-M $_*$相关性彼此一致。使用SFHS从半解析模型和宇宙学流体动力学模拟验证测试证实了该方法的灵敏度变化的斜率，归一化和形状的SFR-M $_*$相关性。这种技术使我们能够通过$\sim 1$ dex进一步探测高z处的相关性的低质量区域，并且在$\sim 10\times$的有效体积上比直接拟合可能的更大。我们发现，SFR-M $_*$相关性与在$z>4$处线性下降至M $_*\sim 10^7 M_\odot$一致。相关性的演化可以用$\log SFR= (0.80\pm 0.029 - 0.017\pm 0.010\times t_{univ})\log M_*$ $- (6.487\pm 0.282-0.039\pm 0.008\times t_{univ})$来描述，其中$t_{univ}$是以Gyr为单位的宇宙年龄。

英文摘要：

To achieve a fuller understanding of galaxy evolution, SED fitting can be used to recover quantities beyond stellar masses (M$_*$) and star formation rates (SFRs). We use Star Formation Histories (SFHs) reconstructed via the Dense Basis method of Iyer \& Gawiser (2017) for a sample of $17,873$ galaxies at $0.5<z<6$ in the CANDELS GOODS-S field to study the nature and evolution of the SFR-M$_*$ correlation. The reconstructed SFHs represent trajectories in SFR-M$_*$ space, enabling us to study galaxies at epochs earlier than observed by propagating them backwards in time along these trajectories. We study the SFR-M$_*$ correlation at $z=1,2,3,4,5,6$ using both direct fits to galaxies observed at those epochs and SFR-M$_*$ trajectories of galaxies observed at lower redshifts. The SFR-M$_*$ correlations obtained using the two approaches are found to be consistent with each other through a KS test. Validation tests using SFHs from semi-analytic models and cosmological hydrodynamical simulations confirm the sensitivity of the method to changes in the slope, normalization and shape of the SFR-M$_*$ correlation. This technique allows us to further probe the low-mass regime of the correlation at high-z by $\sim 1$ dex and over an effective volume of $\sim 10\times$ larger than possible with just direct fits. We find that the SFR-M$_*$ correlation is consistent with being linear down to M$_*\sim 10^7 M_\odot$ at $z>4$. The evolution of the correlation is well described by $\log SFR= (0.80\pm 0.029 - 0.017\pm 0.010\times t_{univ})\log M_*$ $- (6.487\pm 0.282-0.039\pm 0.008\times t_{univ})$, where $t_{univ}$ is the age of the universe in Gyr.

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