z≈1 恒星形成星系的 Hi 质量函数

Aditya Chowdhury, Nissim Kanekar and Jayaram N. Chengalur
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引用次数: 0

摘要

我们通过对恒星形成星系的 Hi 质量(MHi)和 B 波段光度(MB)之间的比例关系的测量,结合对 z ≈ 1 波段 B 波段光度函数的文献估计,首次提出了基于直接 Hi 21 厘米观测数据对 z ≈ 1 波段恒星形成星系 Hi 质量函数(HiMF)的估计值。我们利用对 DEEP2 星场的 GMRT-CATz1 勘测,在三个独立的 MB 子样本中测量了 z = 0.74-1.45 时蓝星系的平均 Hi 质量,从而确定了 MHi-MB 关系。具体做法是分别堆叠每个子样本中星系的 21 厘米 Hi 发射信号,在 (3.5-4.4)σ 重要度处探测每个子样本的 21 厘米 Hi 平均发射信号。我们发现z≈1时的MHi-MB关系与z≈0时的MHi-MB关系是一致的。我们将z≈1时的MHi-MB关系估计值与z≈1时的B波段光度函数结合起来,确定了z≈1时的HiMF。我们发现,在MHi-MB关系中假定的散射范围很宽的情况下,z≈1时MHi>1010M⊙(高于本地Hi质量函数的膝点)的星系数量密度比z≈0时的高出≈4-5倍。我们以 ≳99.7% 的置信度排除了 MHi > 1010M⊙ 的星系数量密度在 z≈1 和 z≈0 之间保持不变的假设。这是自宇宙正午纪起星系HiMF演化的第一个具有统计意义的证据。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
The Hi Mass Function of Star-forming Galaxies at z ≈ 1
We present the first estimate, based on direct Hi 21 cm observations, of the Hi mass function (HiMF) of star-forming galaxies at z ≈ 1, obtained by combining our measurement of the scaling relation between Hi mass (MHi) and B-band luminosity (MB) of star-forming galaxies with a literature estimate of the B-band luminosity function at z ≈ 1. We determined the MHi–MB relation by using the GMRT-CATz1 survey of the DEEP2 fields to measure the average Hi mass of blue galaxies at z = 0.74–1.45 in three separate MB subsamples. This was done by separately stacking the Hi 21 cm emission signals of the galaxies in each subsample to detect, at (3.5–4.4)σ significance, the average Hi 21 cm emission of each subsample. We find that the MHi–MB relation at z ≈ 1 is consistent with that at z ≈ 0. We combine our estimate of the MHi–MB relation at z ≈ 1 with the B-band luminosity function at z ≈ 1 to determine the HiMF at z ≈ 1. We find that the number density of galaxies with MHi > 1010M⊙ (higher than the knee of the local Hi mass function) at z ≈ 1 is a factor of ≈4–5 higher than that at z ≈ 0, for a wide range of assumed scatters in the MHi–MB relation. We rule out the hypothesis that the number density of galaxies with MHi > 1010M⊙ remains unchanged between z ≈ 1 and z ≈ 0 at ≳99.7% confidence. This is the first statistically significant evidence for evolution in the HiMF of galaxies from the epoch of cosmic noon.
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