论文标题
$ \ mathrm {m _ {\ star}} $ - sfr关系的贝叶斯层次结构建模与Astrodep中的1 <z <6
Bayesian hierarchical modelling of the $\mathrm{M_{\star}}$-SFR relation from 1<z<6 in ASTRODEEP
论文作者
论文摘要
哈勃前沿场代表了探测恒星形成星系的主要序列的高红移进化，这要归功于空白场的质量，这要归功于大型星系簇的前景镜头。我们使用beagle sed拟合代码来得出出色的质量，$ \ mathrm {m _ {\ star}} = \ log（m/\ mathrm {m _ {\ odot}}}）$，sfrs，sfrs，sfrs，sfrs，sfrs，sfrs， $ψ= \ log（ψ/\ mathrm {m _ {\ odot}} \，\ mathrm {yr}^{ - 1}）$和来自Astrodepep目录中星系的RedShifts。我们适合主序列的完全贝叶斯分层模型，超过$ 1.25 <z <6 $的$ $ψ=α__\ mathrm {9.7}（z） +β（\ mathrm {\ mathrm {m _ {\ star}}} -9.7） - 9.7） + \ \ \ \ \ \ \ \ \ \ \ n}（n} n}（0，0，nirit）$ extlier。 $ \ mathrm {m _ {\ star}} = 9.7 $在$ \ mathrm处的红移依赖性截距被参数化为$α_\ mathrm {9.7}（z）= \ log [n（1 + z）^γ] + 0.7 $。我们的结果与高红移的主要序列的归一化相一致，这是在红色转移依赖的浓度速率上，以$γ= 2.40^{+0.18} _ { - 0.18} $，其依赖于红色的变速率。我们测量$β= 0.79^{+0.03} _ { - 0.04} $和$σ= 0.26^{+0.02} _ { - 0.02} $的斜率和内在散布。我们发现，通过过滤器的组合（Hubble +基于地面的KS频段 + Spitzer 3.6和4.5 $ \ Mathrm {μm} $）提供的SED取样不足以约束$ \ mathrm {m _ {\ star}}}} $和$ n $ nift Seperce的完整动态范围，甚至在观察到的Main Sepcection上，甚至是$ nows powers fords powers powers powers。尽管此过滤器集代表了高红移星系SED的最佳当前采样到$ z> 3 $，但对低质量和高红移的主要序列的测量仍然很大程度上取决于SED拟合中使用的先验（以及其他拟合假设）。 JWST的未来数据集应改善这一点。
The Hubble Frontier Fields represent the opportunity to probe the high-redshift evolution of the main sequence of star-forming galaxies to lower masses than possible in blank fields thanks to foreground lensing of massive galaxy clusters. We use the BEAGLE SED-fitting code to derive stellar masses, $\mathrm{M_{\star}}=\log(M/\mathrm{M_{\odot}})$, SFRs, $Ψ=\log(ψ/\mathrm{M_{\odot}}\,\mathrm{yr}^{-1})$ and redshifts from galaxies within the ASTRODEEP catalogue. We fit a fully Bayesian hierarchical model of the main sequence over $1.25<z<6$ of the form $Ψ= α_\mathrm{9.7}(z) + β(\mathrm{M_{\star}}-9.7) + \mathcal{N}(0,σ^2)$ while explicitly modelling the outlier distribution. The redshift-dependent intercept at $\mathrm{M_{\star}}=9.7$ is parametrized as $α_\mathrm{9.7}(z) = \log[N (1+z)^γ] + 0.7$. Our results agree with an increase in normalization of the main sequence to high redshifts that follows the redshift-dependent rate of accretion of gas onto dark matter halos with $γ=2.40^{+0.18}_{-0.18}$. We measure a slope and intrinsic scatter of $β=0.79^{+0.03}_{-0.04}$ and $σ=0.26^{+0.02}_{-0.02}$. We find that the sampling of the SED provided by the combination of filters (Hubble + ground-based Ks-band + Spitzer 3.6 and 4.5 $\mathrm{μm}$) is insufficient to constrain $\mathrm{M_{\star}}$ and $Ψ$ over the full dynamic range of the observed main sequence, even at the lowest redshifts studied. While this filter set represents the best current sampling of high-redshift galaxy SEDs out to $z>3$, measurements of the main sequence to low masses and high redshifts still strongly depend on priors employed in SED fitting (as well as other fitting assumptions). Future data-sets with JWST should improve this.
