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arXiv 2102.11282astro-ph.GAastro-ph.CO
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星系的恒星质量和晕质量之间依赖于形态关系的动力学证据

Dynamical evidence for a morphology-dependent relation between the stellar and halo masses of galaxies

Lorenzo Posti, S. Michael Fall

备注：
Accepted for publication in A&A. Figure 3 shows the main result of the paper
发表信息：
A&A 649, A119 (2021)
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摘要：

本文从早型星系的近红外光度（对于$M_\star$）和球状星团系统的位置-速度分布（对于$M_{\rm h}$）出发，导出了早型星系的恒星-晕质量关系（SHMR），即$f_\star\propto M_\star/M_{\rm h}$对$M_\star$和$M_{\rm h}$的关系。我们个人的估计$M_{\rm h}$是基于拟合的动力学模型与表示的作用角变量的分布函数，并施加一个先验$M_{\rm h}$的浓度-质量关系在标准的$Λ$ CDM宇宙学。我们发现，早型星系的SHMR下降的质量超过一个峰值在$M_\star\sim 5\times 10^{10}M_\odot$和$M_{\rm h}\sim 10^{12}M_\odot$（附近的银河系的质量）。这一结果是一致的标准SHMR来自一般人口的星系丰度匹配，并与以前的，不太强大的衍生早期类型的SHMR。然而，它形成鲜明对比的单调上升SHMR晚期类型来自扩展HI旋转曲线和相同的$Λ$ CDM之前$M_{\rm h}$，我们采用的早期类型。大质量星系的SHMR或多或少是连续变化的，从上升到下降，减少盘分数和减少哈勃类型。我们还表明，不同的SHMR晚和早期类型是一致的，它们的恒星速度和质量之间的相似的标度关系（塔利-费舍尔和费伯-杰克逊关系）。恒星和晕维里速度之间的关系的差异占的相似性的标度关系。我们认为，所有这些经验研究结果是一个图片中，银河系盘主要是建立顺利和逐步流入，调节年轻恒星的反馈，而银河系球状体之间的合作合并，黑洞燃料，并从AGN的反馈建立的自然后果。

英文摘要：

We derive the stellar-to-halo mass relation (SHMR), namely $f_\star\propto M_\star/M_{\rm h}$ versus $M_\star$ and $M_{\rm h}$, for early-type galaxies from their near-IR luminosities (for $M_\star$) and the position-velocity distributions of their globular cluster systems (for $M_{\rm h}$). Our individual estimates of $M_{\rm h}$ are based on fitting a dynamical model with a distribution function expressed in terms of action-angle variables and imposing a prior on $M_{\rm h}$ from the concentration-mass relation in the standard $Λ$CDM cosmology. We find that the SHMR for early-type galaxies declines with mass beyond a peak at $M_\star\sim 5\times 10^{10}M_\odot$ and $M_{\rm h}\sim 10^{12}M_\odot$ (near the mass of the Milky Way). This result is consistent with the standard SHMR derived by abundance matching for the general population of galaxies, and with previous, less robust derivations of the SHMR for early types. However, it contrasts sharply with the monotonically rising SHMR for late types derived from extended HI rotation curves and the same $Λ$CDM prior on $M_{\rm h}$ as we adopt for early types. The SHMR for massive galaxies varies more or less continuously, from rising to falling, with decreasing disc fraction and decreasing Hubble type. We also show that the different SHMRs for late and early types are consistent with the similar scaling relations between their stellar velocities and masses (Tully-Fisher and Faber-Jackson relations). Differences in the relations between the stellar and halo virial velocities account for the similarity of the scaling relations. We argue that all these empirical findings are natural consequences of a picture in which galactic discs are built mainly by smooth and gradual inflow, regulated by feedback from young stars, while galactic spheroids are built by a cooperation between merging, black-hole fuelling, and feedback from AGNs.

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