arXiv 2108.032532021-08astro-ph.GAastro-ph.CO

HI选择星系的暗物质晕

The Dark Matter Halos of HI Selected Galaxies

Saili Dutta, Nishikanta Khandai, Sandeep Rana

备注：: 17 pages, 11 figures, 2 tables, Accepted for publication in MNRAS
DOI：: 10.1093/mnras/stab3618

摘要：

本文根据阿尔法巡天（$α.40$）40%数据中的7857个星系，给出了中性氢质量（$M_{\text{HI}}$）函数（HIMF）和速度宽度（$w_{50}$）函数（HIWF）。HIMF（HIWF）的低质量（速度宽度）端主要由蓝色的星系人口占主导地位，而红色的人口占主导地位的HIMF（HIWF）在高质量（速度宽度）端。我们使用反卷积方法来估计HI旋转速度（$V_{\text{rot}}$）函数（HIVF）从HIWF的总，红色和蓝色的样品。红色和蓝色样本的HIWF和HIVF与其HIMF相比在函数的拐点处分离良好。然后，我们使用最近的堆积的ALOTHFA调查的结果来约束晕质量（$M_{\text{h}}$）HI选择星系的功能。这使我们能够获得$M_{\text{HI}} - w_{50} - V_{\text{rot}} - M_{\text{h}}$，我们目前的各种缩放关系。$M_{\text{HI}} - M_{\text{h}}$关系在小质量时有一个陡的斜率~2.10，在大于过渡晕质量$\log_{10}(M_{\text{ht}} h^2_{70}/M_{\odot})=10.62$的质量时，斜率为~0.34。我们的比例关系是强大的，并与$α.40$的体积有限的样品一致。$M_{\text{HI}} - M_{\text{h}}$关系在性质上类似于$M_{\text{star}} - M_{\text{h}}$关系，但过渡晕质量比$M_{\text{star}} - M_{\text{h}}$关系小约1.4倍。我们的研究结果表明，重子过程，如加热和反馈在较大的质量晕抑制HI气体在较短的时间尺度相比，恒星形成。

英文摘要：

We present the neutral hydrogen mass ($M_{\text{HI}}$) function (HIMF) and velocity width ($w_{50}$) function (HIWF) based on a sample of 7857 galaxies from the 40% data release of the ALFALFA survey ($α.40$). The low mass (velocity width) end of the HIMF (HIWF) is dominated by the blue population of galaxies whereas the red population dominates the HIMF (HIWF) at the high mass (velocity width) end. We use a deconvolution method to estimate the HI rotational velocity ($V_{\text{rot}}$) functions (HIVF) from the HIWF for the total, red, and blue samples. The HIWF and HIVF for the red and blue samples are well separated at the knee of the function compared to their HIMFs. We then use recent stacking results from the ALFALFA survey to constrain the halo mass ($M_{\text{h}}$) function of HI-selected galaxies. This allows us to obtain various scaling relations between $M_{\text{HI}} - w_{50} - V_{\text{rot}} - M_{\text{h}}$, which we present. The $M_{\text{HI}} - M_{\text{h}}$ relation has a steep slope ~2.10 at small masses and flattens to ~0.34 at masses larger than a transition halo mass, $\log_{10}(M_{\text{ht}} h^2_{70}/M_{\odot})=10.62$. Our scaling relation is robust and consistent with a volume-limited sample of $α.40$. The $M_{\text{HI}} - M_{\text{h}}$ relation is qualitatively similar to the $M_{\text{star}} - M_{\text{h}}$ relation but the transition halo mass is smaller by ~1.4 dex compared to that of the $M_{\text{star}} - M_{\text{h}}$ relation. Our results suggest that baryonic processes like heating and feedback in larger mass halos suppress HI gas on a shorter time scale compared to star-formation.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

摘要：

英文摘要：

相关论文