The thesan project: galaxy sizes during the epoch of reionization

IF 4.7 3区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS
Xuejian Shen, Mark Vogelsberger, Josh Borrow, Yongao Hu, Evan Erickson, Rahul Kannan, Aaron Smith, Enrico Garaldi, Lars Hernquist, Takahiro Morishita, Sandro Tacchella, Oliver Zier, Guochao Sun, Anna-Christina Eilers, Hui Wang
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Abstract

We investigate galaxy sizes at redshift z ≳ 6 with the cosmological radiation-magneto-hydrodynamic simulation suite thesan(-hr). These simulations simultaneously capture reionization of the large-scale intergalactic medium and resolved galaxy properties. The intrinsic sizes ($r^{\ast }_{1/2}$) of simulated galaxies increase moderately with stellar mass at $M_{\ast } \lesssim 10^{8}{\, \rm M_\odot }$ and decrease fast at larger masses, resulting in a hump feature at $M_{\ast }\sim 10^{8}{\, \rm M_\odot }$ that is insensitive to redshift. Low-mass galaxies are in the initial phase of size growth and are better described by a spherical shell model with feedback-driven outflows competing with the cold inflowing gas streams. In contrast, massive galaxies fit better with the disk formation model. They generally experience a phase of rapid compaction and gas depletion, likely driven by internal disk instability rather than external processes. We identify four compact quenched galaxies in the (95.5 cMpc)3 volume of thesan-1 at z ≃ 6 and their quenching follows reaching a characteristic stellar surface density akin to the massive compact galaxies at cosmic noon. Compared to observations, we find that the median UV effective radius ($R^{\rm UV}_{\rm eff}$) of simulated galaxies is at least three times larger than the observed ones at $M_{\ast }\lesssim 10^{9}{\, \rm M_\odot }$ or MUV ≳ −20 at 6 ≲ z ≲ 10. The population of compact galaxies ($R^{\rm UV}_{\rm eff}\lesssim 300\, {\rm pc}$) galaxies at $M_{\ast }\sim 10^{8}{\, \rm M_\odot }$ is missing in our simulations. This inconsistency persists across many other cosmological simulations with different galaxy formation models and demonstrates the potential of using galaxy morphology to constrain physics of galaxy formation at high redshifts.
Thesan 项目:再电离时代的星系大小
我们利用宇宙学辐射-磁流体动力学模拟套件 thesan(-hr)研究了红移 z ≳ 6 时的星系大小。这些模拟同时捕捉了大尺度星系际介质的再电离和解析的星系特性。模拟星系的本征尺寸($r^{\ast }_{1/2}$)随着恒星质量的增加而适度增加,达到$M_{\ast }_{1/2}$。\lesssim 10^{8}{\, \rm M_\odot }$时随着恒星质量的增加而适度增大,而在质量较大时则迅速减小,从而在$M_{ast }\sim 10^{8}{\, \rm M_\odot }$时出现对红移不敏感的驼峰特征。低质量星系正处于体积增长的初始阶段,球壳模型可以更好地描述它们,该模型中反馈驱动的外流与冷内流气体流相互竞争。相比之下,大质量星系更适合圆盘形成模型。它们通常会经历一个快速压缩和气体耗竭的阶段,这很可能是由内部盘的不稳定性而不是外部过程驱动的。我们在 z ≃ 6时的thesan-1(95.5 cMpc)3体积中发现了四个紧凑淬火星系,它们的淬火是在达到与宇宙正午大质量紧凑星系相似的恒星表面密度之后发生的。与观测结果相比,我们发现在6 ≲ z ≲ 10时,模拟星系的中位紫外有效半径($R^{/rm UV}_{\rm eff}$)比观测到的星系大至少三倍,即$M_{ast}lesssim 10^{9}\{, \rm M_\odot }$或MUV ≳ -20。我们的模拟中缺少M_{ast }\sim 10^{8}{\,\rm M_\odot }$的紧凑星系(R^{\rm UV}_{\rm eff}\lesssim 300\, {\rm pc}$)。这种不一致性在许多其他采用不同星系形成模型的宇宙学模拟中都存在,这也证明了利用星系形态学来约束高红移下星系形成物理学的潜力。
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来源期刊
CiteScore
9.10
自引率
37.50%
发文量
3198
审稿时长
3 months
期刊介绍: Monthly Notices of the Royal Astronomical Society is one of the world''s leading primary research journals in astronomy and astrophysics, as well as one of the longest established. It publishes the results of original research in positional and dynamical astronomy, astrophysics, radio astronomy, cosmology, space research and the design of astronomical instruments.
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