An ALMA/NOEMA survey of the molecular gas properties of high-redshift star-forming galaxies
An ALMA/NOEMA survey of the molecular gas properties of high-redshift star-forming galaxies
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DOI：
10.1093/mnras/staa3862
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发表时间：
2020-09
影响因子：
4.8
通讯作者：
J. Birkin;A. Weiss;J. Wardlow;I. Smail;A. Swinbank;U. Dudzevivciut.e;F. An;Y. Ao;S. Chapman;Chian-Chou Chen;E. D. Cunha;H. Dannerbauer;B. Gullberg;J. Hodge;S. Ikarashi;R. Ivison;Y. Matsuda;S. Stach;F. Walter;W.-H. Wang;P. Werf
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文献类型：
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作者：
J. Birkin;A. Weiss;J. Wardlow;I. Smail;A. Swinbank;U. Dudzevivciut.e;F. An;Y. Ao;S. Chapman;Chian-Chou Chen;E. D. Cunha;H. Dannerbauer;B. Gullberg;J. Hodge;S. Ikarashi;R. Ivison;Y. Matsuda;S. Stach;F. Walter;W.-H. Wang;P. Werf
我们已经使用阿尔马和NOEMA研究了61个ALMA确定的亚毫米星系（SMG）的COSMOS，UDS和ECDFS领域的分子气藏。我们在50个源中检测到12 CO（$J_{\rm up} =$2 -5）发射线，在8个源中检测到[C i]（3 P1 - 3 P0）发射线，$z =$1.2 -4.8，中位红移为2.9 ± 0.2。通过补充我们的数据与文献来源，我们构建了一个统计的CO谱线能量分布，并发现12 CO线的亮度在SMG的Jup 106峰值，与类似的研究一致。我们还测试的相关性的CO，[C i]，和灰尘作为示踪剂的气体质量，发现这三个相关性很好，虽然CO和灰尘的质量估计从3毫米的连续是优选的。我们估计SMG主要位于恒星形成的主序上或略高于主序，对于我们的样本，气体耗尽的中位时标tdep = Mgas/SFR为2.1亿± 4.0亿年。此外，tdep在z = 1-5范围内随红移而下降，而分子气体分数μgas = Mgas/M* 在相同的红移范围内增加。最后，我们证明了我们的SMG的重子总质量和动力学谱线宽度Mbaryon-σ的分布与后发座星系团中早型星系的分布一致，为SMG是大质量局域球状星系的祖先提供了强有力的支持.在此基础上，我们认为，在S870 μ m ~ 5 mJy的870 μm通量极限以上和以下的SMG粒子数可能对应于在局域早型星系中所看到的慢转子和快转子的划分。
We have used ALMA and NOEMA to study the molecular gas reservoirs in 61 ALMA-identified submillimetre galaxies (SMGs) in the COSMOS, UDS, and ECDFS fields. We detect 12CO ($J_{\rm up} =$ 2–5) emission lines in 50 sources, and [C i](3P1 − 3P0) emission in eight, at $z =$ 1.2–4.8 and with a median redshift of 2.9 ± 0.2. By supplementing our data with literature sources, we construct a statistical CO spectral line energy distribution and find that the 12CO line luminosities in SMGs peak at Jup ∼ 6, consistent with similar studies. We also test the correlations of the CO, [C i], and dust as tracers of the gas mass, finding the three to correlate well, although the CO and dust mass as estimated from the 3-mm continuum are preferable. We estimate that SMGs lie mostly on or just above the star-forming main sequence, with a median gas depletion timescale, tdep = Mgas/SFR, of 210 ± 40 Myr for our sample. Additionally, tdep declines with redshift across z ∼ 1–5, while the molecular gas fraction, μgas = Mgas/M*, increases across the same redshift range. Finally, we demonstrate that the distribution of total baryonic mass and dynamical line width, Mbaryon–σ, for our SMGs is consistent with that followed by early-type galaxies in the Coma cluster, providing strong support to the suggestion that SMGs are progenitors of massive local spheroidal galaxies. On the basis of this, we suggest that the SMG populations above and below an 870-μm flux limit of S870 ∼ 5 mJy may correspond to the division between slow and fast rotators seen in local early-type galaxies.