Evolution of cosmic star formation in the SCUBA-2 Cosmology Legacy Survey
Evolution of cosmic star formation in the SCUBA-2 Cosmology Legacy Survey
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DOI：
10.1093/mnras/stx031
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发表时间：
2017-05-01
影响因子：
4.8
通讯作者：
van der Werf, P. P.
中科院分区：
文献类型：
--
作者：
Bourne, N.;Dunlop, J. S.;van der Werf, P. P.
本文对红移为0.5 < z < 6的大质量星系中宇宙星星的形成历史和尘埃遮蔽进行了新的探索。我们利用SCUBA-2 CLS的最深450和850 μ m成像，覆盖AEGIS、COSMOS和UDS领域的230弧分（2），以及Herschel的100-250 μ m成像。我们证明了T-PHOT解融合代码的能力，以达到低于混乱的限制，使用多波长前目录从CANDELS/3D-HST。通过结合红外和紫外数据，我们测量总星星形成率（SFR）和恒星质量之间的关系，z类似于5，表明紫外衍生的尘埃校正低估了大质量星系的SFR。我们调查之间的关系，在我们的样本，这是类似于低红移的星暴星系的遮蔽和紫外线斜率（IRX-beta关系），虽然它偏离在高恒星质量。我们的数据提供了M-* > 10（10）M-O星系在0.5 < z 10时总SFR密度（SFRD）的新测量结果< 6. This is dominated by obscured star formation by a factor of >。其中三分之一是由450 μ m探测到的光源造成的，而五分之一是由紫外光源（比L-UV（*）亮）造成的，尽管这些光源在很大程度上是模糊的。通过外推我们的结果，包括所有的恒星质量，我们估计了一个总的SFRD，这是在很好的协议与以前的结果，从红外和紫外数据在z
We present a new exploration of the cosmic star formation history and dust obscuration in massive galaxies at redshifts 0.5 < z < 6. We utilize the deepest 450-and 850-mu m imaging from SCUBA-2 CLS, covering 230 arcmin(2) in the AEGIS, COSMOS and UDS fields, together with 100-250 mu m imaging from Herschel. We demonstrate the capability of the T-PHOT deconfusion code to reach below the confusion limit, using multiwavelength prior catalogues from CANDELS/3D-HST. By combining IR and UV data, we measure the relationship between total star formation rate (SFR) and stellar mass up to z similar to 5, indicating that UV-derived dust corrections underestimate the SFR in massive galaxies. We investigate the relationship between obscuration and the UV slope (the IRX-beta relation) in our sample, which is similar to that of low-redshift starburst galaxies, although it deviates at high stellar masses. Our data provide new measurements of the total SFR density (SFRD) in M-* > 10(10) M-O galaxies at 0.5 < z < 6. This is dominated by obscured star formation by a factor of > 10. One third of this is accounted for by 450 mu m-detected sources, while one-fifth is attributed to UV-luminous sources (brighter than L-UV(*)), although even these are largely obscured. By extrapolating our results to include all stellar masses, we estimate a total SFRD that is in good agreement with previous results from IR and UV data at z