Suppression of star formation in low-mass galaxies caused by the reionization of their local neighbourhood
Suppression of star formation in low-mass galaxies caused by the reionization of their local neighbourhood
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由于当地邻居的再电离而导致低质量星系中恒星形成的抑制
DOI：
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发表时间：
2018
影响因子：
4.8
通讯作者：
Y. Hoffman
中科院分区：
文献类型：
--
作者：
Taha Dawoodbhoy;P. Shapiro;P. Ocvirk;D. Aubert;N. Gillet;Jun;I. Iliev;R. Teyssier;G. Yepes;S. Gottlober;Anson D’Aloisio;Hyunbae Park;Y. Hoffman
在低质量星系中，与再电离相关的光热抑制了恒星的形成。然而，再电离是不均匀的，在不同的时间影响不同的地区。为了建立再电离和抑制之间的因果关系，我们必须考虑到这种局部变化。我们分析了CoDa（“宇宙黎明”）I的结果，这是局部宇宙中再电离和星系形成的第一个完全耦合的辐射-流体动力学模拟，在一个足够大的体积中模拟全球的再电离，但具有足够的分辨率来跟踪该体积中所有原子冷却的星系晕。对于在给定时间确定的每个光晕，我们可以找到周围IGM再电离时的红移，以及它的瞬时恒星形成速率（' SFR'）和重子气体与暗物质的比率（$M_\text{gas}/M_\text{DM}$）。每个光晕的平均SFR为$M 10^{10} \text{M}_\odot$，该SFR通过局部再电离持续，随着时间的增加而增加。对于$10^9 < M < 10^{10} \text{M}_\odot$， SFR一般通过再电离适度增加，然后适度下降。一般来说，再电离时间越早的区域，光晕sfr越高。在$M < 10^9 \text{M}_\odot$的局部再电离后，$M_\text{gas}/ $M_\text{DM}$的局部再电离率急剧下降。局部再电离时间与局部物质过密度有关，这决定了局部结构形成速率和电离光子消耗。最早形成结构和再电离的斑块最终产生了比完成和维持自身再电离所需的更多的恒星，输出它们的“剩余”星光来帮助后来形成结构的区域再电离。
Photoheating associated with reionization suppressed star formation in low-mass galaxies. Reionization was inhomogeneous, however, affecting different regions at different times. To establish the causal connection between reionization and suppression, we must take this local variation into account. We analyze the results of CoDa (`Cosmic Dawn') I, the first fully-coupled radiation-hydrodynamical simulation of reionization and galaxy formation in the Local Universe, in a volume large enough to model reionization globally but with enough resolving power to follow all atomic-cooling galactic halos in that volume. For every halo identified at a given time, we find the redshift at which the surrounding IGM reionized, along with its instantaneous star formation rate (`SFR') and baryonic gas-to-dark matter ratio ($M_\text{gas}/M_\text{DM}$). The average SFR per halo with $M 10^{10} \text{ M}_\odot$, this SFR continued through local reionization, increasing with time, instead. For $10^9 < M < 10^{10} \text{ M}_\odot$, the SFR generally increased modestly through reionization, followed by a modest decline. In general, halo SFRs were higher for regions that reionized earlier. A similar pattern was found for $M_\text{gas}/M_\text{DM}$, which declined sharply following local reionization for $M < 10^9 \text{ M}_\odot$. Local reionization time correlates with local matter overdensity, which determines the local rates of structure formation and ionizing photon consumption. The earliest patches to develop structure and reionize ultimately produced more stars than they needed to finish and maintain their own reionization, exporting their `surplus' starlight to help reionize regions that developed structure later.
DOI：
10.1088/2041-8205/756/1/l16
发表时间：
2012-06
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
K. Ahn;I. Iliev;P. Shapiro;G. Mellema;J. Koda;Y. Mao
通讯作者：
K. Ahn;I. Iliev;P. Shapiro;G. Mellema;J. Koda;Y. Mao
DOI：
10.3847/2041-8213/aab14d
发表时间：
2018
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
Aubert D
通讯作者：
Aubert D