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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >CO emissions from optically selected galaxies at z similar to 0.1-0.2: Tight anti-correlation between molecular gas fraction and 4000 angstrom break strength
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CO emissions from optically selected galaxies at z similar to 0.1-0.2: Tight anti-correlation between molecular gas fraction and 4000 angstrom break strength

机译：光学选择的星系在z处的CO排放类似于0.1-0.2：分子气体分数与4000埃断裂强度之间的紧密反相关

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摘要

We performed (CO)-C-12(J = 1-0) (hereafter, CO) observations toward 12 normal star-forming galaxies with stellar masses of M-star = 10(10.6)-10(11.3) M-circle dot at z = 0.1-0.2 with the 45 m telescope at the Nobeyama Radio Observatory. The samples were selected with D-n(4000), that is, the strength of the 4000 angstrom break, instead of the commonly used far-infrared (FIR) flux. We successfully detected the CO emissions from eight galaxies with signal-to-noise ratio larger than three, demonstrating the effectiveness of the D-n(4000)-based sample selection. For the first time, we find a tight anti-correlation between D-n(4000) and molecular gas fraction (f(mol)) using literature data of nearby galaxies in which the galaxies with more fuel for star formation have younger stellar populations. We find that our CO-detected galaxies at z similar to 0.1-0.2 also follow the same relation as nearby galaxies. This implies that the galaxies evolve along this D-n(4000)-f(mol) relation, and that D-n(4000) seems to be able to be used as a proxy for fmol, which requires many time-consuming observations. Based on the comparison with the model calculation with a population synthesis code, we find that star formation from metal enriched gas and its quenching in the early time are necessary to reproduce galaxies with large D-n(4000) and non-zero gas fraction.
机译：我们对12个正常恒星形成星系进行了（CO）-C-12（J = 1-0）（以下称CO）观测，恒星质量为M-star = 10（10.6）-10（11.3）M圆点用Nobeyama无线电天文台的45 m望远镜在z = 0.1-0.2处。使用D-n（4000）（即4000埃断裂强度）代替了常用的远红外（FIR）通量选择了样品。我们成功地检测到信噪比大于三个的8个星系中的CO排放，证明了基于D-n（4000）的样本选择的有效性。首次，我们使用附近星系的文献数据发现D-n（4000）与分子气体分数（f（mol））之间存在紧密的反相关关系，在该数据中，具有更多燃料以形成恒星的星系具有更年轻的恒星群体。我们发现，z处的CO探测到的星系类似于0.1-0.2，也与附近的星系具有相同的关系。这意味着星系沿着这种D-n（4000）-f（mol）关系演化，并且D-n（4000）似乎可以用作fmol的代理，这需要许多费时的观察。通过与具有总体合成代码的模型计算的比较，我们发现，富金属气体形成的恒星及其早期淬火对于重现D-n（4000）和非零气体分数的星系是必要的。

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