从孤立星系到宇宙学流体动力学模拟的银河系HI-暗物质晕质量关系
The galactic HI-to-halo mass relation from isolated galaxies to cosmological hydrodynamic simulations
- Instituto de Astrofísica de Andalucía (CSIC)（安达卢西亚天体物理研究所）
- Laboratoire de Physique et de Chimie de l’Environnement, Université Joseph Ki-Zerbo（约瑟夫·基泽尔博大学环境物理与化学实验室）
- Université de Strasbourg, CNRS, Observatoire astronomique de Strasbourg（斯特拉斯堡大学）
- Center for Astrophysics and Space Science (CASS), New York University Abu Dhabi（阿布扎比纽约大学天体物理学与空间科学中心）
- New York University Abu Dhabi（阿布扎比纽约大学）
机构由 AI 辅助整理，请以论文原文为准。
AI总结：
本研究利用AMIGA和GHASP样本扩展了HI质量与暗物质晕质量关系的分析，确认该比值在盘状星系中近似恒定（$\log(M_{HI}/M_{200})=-1.90$），与模拟预测的恒星质量依赖性形成对比，暗示存在质量无关的自调控机制。
AI中文摘要：
HI与暗物质（DM）晕质量之间的关系为理解气体吸积和星系形成的调控提供了关键见解。在先前基于SPARC和LITTLE THINGS样本的研究中，我们表明对于附近的盘状星系，HI质量与暗物质晕质量之比随恒星质量近似保持恒定（$\log(M_{HI}/M_{200})=-1.90$，1σ弥散为0.37 dex）。在本工作中，我们通过纳入来自孤立星系星际介质分析（AMIGA）样本和Gassendi HAlpha旋涡星系巡天（GHASP）的星系来扩展该分析。AMIGA样本提供了本地宇宙中经过最严格筛选的孤立星系样本，非常适合检验先前样本中发现的该关系是否在无相互作用的星系中成立。我们利用高分辨率旋转曲线和红外测光构建质量模型，并推导暗物质晕参数。我们确认了HI与暗物质晕质量之间的正比关系，并发现HI质量与晕质量之比在恒星质量跨越近五个数量级（$7\leq\log(M_{\star}/M_\odot)\leq 11.5$）的范围内近似恒定，为$\log(M_{HI}/M_{200})=-1.90$，1σ弥散为0.36 dex。AMIGA和GHASP样本在统计上与先前针对SPARC和LITTLE THINGS样本发现的关系一致，表明该关系在跨越广泛孤立程度的星系中是稳健的。相比之下，诸如SIMBA、IllustrisTNG和NIHAO等宇宙学流体动力学模拟预测了该关系对恒星质量的依赖性，并且在盘状星系的高恒星质量端（$M_{\star}>10^{10}M_\odot$）出现断裂。因此，我们的结果进一步表明，HI质量与晕质量之比在旋转支持的盘状星系中表现出显著的自相似性，暗示着当前理论模型中尚未理解的与质量无关的自调控机制。
英文摘要：
The relation between HI and dark matter (DM) halo masses provides key insights into gas accretion and the regulation of galaxy formation. In a previous study based on SPARC and LITTLE THINGS samples, we showed that the ratio between HI mass and DM halo mass remains approximately constant with stellar mass for nearby disc galaxies ($\log(M_{HI}/M_{200})=-1.90$ with a $1σ$ scatter of 0.37 dex). In this work, we extend that analysis by incorporating galaxies from the Analysis of the interstellar Medium in Isolated GAlaxies (AMIGA) sample and from the Gassendi HAlpha survey of SPirals (GHASP). The AMIGA sample provides the most rigorously selected sample of isolated galaxies in the local Universe, well-suited for testing whether the relation found in the previous samples holds in interaction-free galaxies. We construct mass models from high-resolution rotation curves and infrared photometry, and derive DM halo parameters. We confirm the proportionality between HI and DM halo masses and find a nearly constant HI-mass-to-halo-mass ratio of $\log(M_{HI}/M_{200})=-1.90$ over nearly five orders of magnitude in stellar mass ($7\leq\log(M_{\star}/M_\odot)\leq 11.5$), with a $1σ$ scatter of 0.36 dex. The AMIGA and GHASP samples are statistically consistent with the relation previously found for the SPARC and LITTLE THINGS samples, indicating that it is robust across galaxies spanning a broad range of isolation levels. In contrast, cosmological hydrodynamic simulations such as SIMBA, IllustrisTNG, and NIHAO predict a dependence on stellar mass, with a break at the high stellar mass end for disc galaxies ($M_{\star}>10^{10}M_{\odot}$). Our results thus further demonstrate that the HI-mass-to-halo-mass ratio is remarkably self-similar across rotationally-supported disc galaxies, hinting at mass-independent self-regulation mechanisms that are not yet understood in current theoretical models.
