Host galaxy properties of mergers of stellar binary black holes and their implications for advanced LIGO gravitational wave sources
Host galaxy properties of mergers of stellar binary black holes and their implications for advanced LIGO gravitational wave sources
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恒星双黑洞合并的主星系特性及其对先进 LIGO 引力波源的影响
DOI：
10.1093/mnras/stx3087
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发表时间：
2017-11
期刊：
影响因子：
--
通讯作者：
Yuetong Zhao
中科院分区：
文献类型：
--
作者：
Liang Cao;Youjun Lu;Yuetong Zhao
了解恒星双黑洞(SBBH)合并的宿主星系的性质，对于揭示高级LIGO探测到的SBBH引力波源的起源以及识别它们的电磁对应物具有重要意义。在这里，我们通过实施半解析的SBBH形成公式并合并到宇宙星系形成模型中，对SBBH的宿主星系性质进行了全面的分析。如果SBBH形成和合并之间的时间延迟从$1a$Gyr到哈勃时间，红移$z\la0.3$的SBBH合并优先发生在恒星质量$M_*\Ga2\倍10^{10}\mSun$和金属丰度$Z$峰值为$\sim0.6Z_\odot$的大星系中。然而，重的SBBH合并的宿主星系的恒星质量分布是双峰的，一个峰值在$sim10^9\mSun$，另一个峰值在$sim2\x 10^{10}\mSun$。具有$Z0.2ZOOT$的宿主星系对重合并的贡献率远大于对轻合并的贡献。如果SBBH是在早期宇宙中形成的(例如，$z>；6$)，则它们在$z\la0.3$处探测到的合并优先发生在更大质量的星系中，包括$M_*>；3倍于10^{10}\mSun$的星系，以及金属含量以$0.2Z_ODOT$为主、在$Z\sim0.6Z_\ODOT$处达到峰值的星系，这是由于它们的宿主星系后来的宇宙组装和富集化。0.3美元的SBBH合并主要发生在螺旋星系中，但如果SBBH合并是在早期宇宙中形成的，那么发生在椭圆星系中的SBBH合并的比例可能会很大；其中约三分之二的合并发生在暗物质晕的中心星系中。我们还给出了较高红移的SBBH合并的宿主星系性质的结果。
Understanding the host galaxy properties of stellar binary black hole (SBBH) mergers is important for revealing the origin of the SBBH gravitational-wave sources detected by advanced LIGO and helpful for identifying their electromagnetic counterparts. Here we present a comprehensive analysis of the host galaxy properties of SBBHs by implementing semi-analytical recipes for SBBH formation and merger into cosmological galaxy formation model. If the time delay between SBBH formation and merger ranges from $\la$\,Gyr to the Hubble time, SBBH mergers at redshift $z\la0.3$ occur preferentially in big galaxies with stellar mass $M_*\ga2\times10^{10}\msun$ and metallicities $Z$ peaking at $\sim0.6Z_\odot$. However, the host galaxy stellar mass distribution of heavy SBBH mergers ($M_{\bullet\bullet}\ga50\msun$) is bimodal with one peak at $\sim10^9\msun$ and the other peak at $\sim2\times10^{10}\msun$. The contribution fraction from host galaxies with $Z\la0.2Z_\odot$ to heavy mergers is much larger than that to less heavy mergers. If SBBHs were formed in the early universe (e.g., $z>6$), their mergers detected at $z\la0.3$ occur preferentially in even more massive galaxies with $M_*>3\times10^{10}\msun$ and in galaxies with metallicities mostly $\ga0.2Z_\odot$ and peaking at $Z\sim0.6Z_\odot$, due to later cosmic assembly and enrichment of their host galaxies. SBBH mergers at $z\la0.3$ mainly occur in spiral galaxies, but the fraction of SBBH mergers occur in elliptical galaxies can be significant if those SBBHs were formed in the early universe; and about two thirds of those mergers occur in the central galaxies of dark matter halos. We also present results on the host galaxy properties of SBBH mergers at higher redshift.
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DOI：
10.3847/2041-8205/830/1/l18
发表时间：
2016-06
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
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通讯作者：
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DOI：
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发表时间：
2002-01
影响因子：
4.8
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J. Hurley;C. Tout;O. Pols
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8.6
作者：
Sai Wang;Yi-Fan Wang;Q. Huang;T. Li
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影响因子：
4.8
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Oliver D. Elbert;J. Bullock;M. Kaplinghat
DOI：
10.3847/1538-4357/aadae5
发表时间：
2017-02
期刊：
The Astrophysical Journal
影响因子：
--
作者：
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