The ALMaQUEST survey IX: the nature of the resolved star forming main sequence
The ALMaQUEST survey IX: the nature of the resolved star forming main sequence
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ALMaQUEST 巡天 IX：已解析恒星形成主序带的性质
DOI：
10.1093/mnras/stab3672
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发表时间：
2022
影响因子：
4.8
通讯作者：
Baker W
中科院分区：
文献类型：
--
作者：
Baker W
我们研究了星星形成率表面密度（ΣSFR）、恒星质量（Σ*）和分子气体质量（）之间标度关系的性质，旨在区分主要的（即更基本的）关系和那些关系。其他关系的间接副产品。我们使用ALMA-MANGA淬火和星星形成调查，并通过使用偏相关和随机森林回归技术分析数据。我们明确地发现，最强的内在相关性之间的是CSFRand（即解决施密特-肯尼库特关系），其次是之间的相关性和CSFRand *（解决分子气体主序列，rMGMS）。一旦考虑到这两个相关性，我们发现，没有证据表明任何内在的相关性之间的星星形成率（SFR）的分子气体的量完全驱动，而它对恒星质量的依赖性（即解决星星形成主序星，rSFMS）只是作为分子气体和恒星质量之间的关系的结果出现。
We investigate the nature of the scaling relations between the surface density of star formation rate (ΣSFR), stellar mass (Σ*), and molecular gas mass (), aiming at distinguishing between the relations that are primary, i.e. more fundamental, and those which are instead an indirect by-product of the other relations. We use the ALMA-MaNGA QUEnching and STar formation survey and analyse the data by using both partial correlations and random forest regression techniques. We unambiguously find that the strongest intrinsic correlation is between ΣSFRand(i.e. the resolved Schmidt–Kennicutt relation), followed by the correlation betweenand Σ*(resolved molecular gas main sequence, rMGMS). Once these two correlations are taken into account, we find that there is no evidence for any intrinsic correlation between ΣSFRand Σ*, implying that star formation rate (SFR) is entirely driven by the amount of molecular gas, while its dependence on stellar mass (i.e. the resolved star forming main sequence, rSFMS) simply emerges as a consequence of the relationship between molecular gas and stellar mass.