Gravitational wave quasinormal mode from Population III massive black hole binaries in various models of population synthesis
Gravitational wave quasinormal mode from Population III massive black hole binaries in various models of population synthesis
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DOI：
10.1093/ptep/ptw143
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发表时间：
2016-06
期刊：
影响因子：
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通讯作者：
T. Kinugawa;H. Nakano;Takashi Nakamura
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文献类型：
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作者：
T. Kinugawa;H. Nakano;Takashi Nakamura
着眼于双黑洞合并后的残余黑洞，我们发现可以以 $5.9-500~{\rm events~yr^{-1}}~({\rm SFR_p}/ (10^{-2.5}~M_\odot~{\rm yr^{-1}~Mpc^{-3}})) \cdot 的速率探测到族 III 双黑洞合并的衰荡引力波({\rm [f_b/(1+f_b)]/0.33})$ 用于各种参数和函数。该速率是针对第二代引力波探测器（例如 KAGRA）的 SNR$>8$ 事件进行估计的。这里，${\rm SFR_p}$和${\rm f_b}$分别是星族III恒星形成率的峰值和双星的比例。当我们仅考虑 SNR$>35$ 的事件时，事件率变为 $0.046-4.21~{\rm events~yr^{-1}}~({\rm SFR_p}/ (10^{-2.5}~M_\odot~{\rm yr^{-1}~Mpc^{-3}})) \cdot ({\rm [f_b/(1+f_b)]/0.33})$。这表明，对于残余黑洞的自旋 $q_f>0.95$，我们的事件率 SNR$>35$ 小于 $0.037~{\rm events~yr^{-1}}~({\rm SFR_p}/ (10^{-2.5}~M_\odot~{\rm yr^{-1}~Mpc^{-3}})) \cdot ({\rm [f_b/(1+f_b)]/0.33})$，而它是 $3-30~{\rm events~yr^{-1}}~({\rm SFR_p}/ (10^{-2.5}~M_\odot~{\rm yr^{-1}~Mpc^{-3}})) \cdot ({\rm [f_b/(1+f_b)]/0.33})$ 用于第三代探测器，例如爱因斯坦望远镜。如果我们检测到许多第三族双星黑洞合并，则可能不仅通过质量分布而且通过自旋分布来约束第三族双星演化路径。
Focusing on the remnant black holes after merging binary black holes, we show that ringdown gravitational waves of Population III binary black holes mergers can be detected with the rate of $5.9-500~{\rm events~yr^{-1}}~({\rm SFR_p}/ (10^{-2.5}~M_\odot~{\rm yr^{-1}~Mpc^{-3}})) \cdot ({\rm [f_b/(1+f_b)]/0.33})$ for various parameters and functions. This rate is estimated for the events with SNR$>8$ for the second generation gravitational wave detectors such as KAGRA. Here, ${\rm SFR_p}$ and ${\rm f_b}$ are the peak value of the Population III star formation rate and the fraction of binaries, respectively. When we consider only the events with SNR$>35$, the event rate becomes $0.046-4.21~{\rm events~yr^{-1}}~({\rm SFR_p}/ (10^{-2.5}~M_\odot~{\rm yr^{-1}~Mpc^{-3}})) \cdot ({\rm [f_b/(1+f_b)]/0.33})$. This suggest that for remnant black hole's spin $q_f>0.95$ we have the event rate with SNR$>35$ less than $0.037~{\rm events~yr^{-1}}~({\rm SFR_p}/ (10^{-2.5}~M_\odot~{\rm yr^{-1}~Mpc^{-3}})) \cdot ({\rm [f_b/(1+f_b)]/0.33})$, while it is $3-30~{\rm events~yr^{-1}}~({\rm SFR_p}/ (10^{-2.5}~M_\odot~{\rm yr^{-1}~Mpc^{-3}})) \cdot ({\rm [f_b/(1+f_b)]/0.33})$ for the third generation detectors such as Einstein Telescope. If we detect many Population III binary black holes merger, it may be possible to constrain the Population III binary evolution paths not only by the mass distribution but also by the spin distribution.