用引力波间接证实Pop III大质量恒星的存在
Possible Indirect Confirmation of the Existence of Pop III Massive Stars by Gravitational Wave
摘要：
我们进行人口合成模拟人口III（流行III）合并的中子星（NS-NS），中子星-黑洞双星（NS-BH），并在宇宙的年龄合并的双黑洞（BH-BH）。我们发现Pop III BH-BH的典型质量是$\sim 30\ \rm{M}_{\odot}$，因此KAGRA、Adv. LIGO、Adv. Virgo和GEO网络可以探测到z=0.28的引力波的内旋啁啾信号。我们的模拟表明，合并的Pop III BH-BH的检测率是$140 (68) \cdot ({\rm SFR}_{\rm p}/10^{-2.5} \rm{M}_{\odot} {\rm yr}^{-1} {\rm Mpc}^{-3}) \cdot {\rm Err}_{\rm sys} ~{\rm events} ~{\rm yr}^{-1}$的平坦（Salpeter）的初始质量函数（IMF），分别，其中$\rm SFR_p$和$\rm Err_{sys}$的Pop III恒星形成率的峰值和可能的系统误差，由于在Pop III人口合成的假设，分别。$\rm Err_{sys}=1$对应于Pop I星的常规参数。通过对合并的Pop III BH-BH的啁啾信号的观测，我们可以根据普朗克卫星测量的宇宙学参数确定双星的质量和红移。我们的模拟表明，合并的Pop III BH-BH的累积红移分布几乎只依赖于宇宙学参数。如果Pop III大质量BH-BH的并合速率大于Pop I BH-BH的并合速率，我们就有可能通过引力波的探测来证实质量为$\sim 30~\rm M_{\odot}$的Pop III大质量恒星的存在。
英文摘要：
We perform population synthesis simulations for Population III (Pop III) coalescing binary neutron stars (NS-NSs), neutron star - black hole binaries (NS-BHs), and binary black holes (BH-BHs) which merge within the age of the universe. We found that the typical mass of Pop III BH-BHs is $\sim 30\ \rm{M}_{\odot}$ so that the inspiral chirp signal of gravitational waves can be detected up to z=0.28 by KAGRA, Adv. LIGO, Adv. Virgo and GEO network. Our simulations suggest that the detection rate of the coalescing Pop III BH-BHs is $140 (68) \cdot ({\rm SFR}_{\rm p}/10^{-2.5} \rm{M}_{\odot} {\rm yr}^{-1} {\rm Mpc}^{-3}) \cdot {\rm Err}_{\rm sys} ~{\rm events} ~{\rm yr}^{-1}$ for the flat (Salpeter) initial mass function (IMF), respectively, where $\rm SFR_p$ and $\rm Err_{sys}$ are the peak value of the Pop III star formation rate and the possible systematic errors due to the assumptions in Pop III population synthesis, respectively. $\rm Err_{sys}=1$ correspond to conventional parameters for Pop I stars. From the observation of the chirp signal of the coalescing Pop III BH-BHs, we can determine both the mass and the redshift of the binary for the cosmological parameters determined by Planck satellite. Our simulations suggest that the cumulative redshift distribution of the coalescing Pop III BH-BHs depends almost only on the cosmological parameters. We might be able to confirm the existence of Pop III massive stars of mass $\sim 30~\rm M_{\odot}$ by the detections of gravitational waves if the merger rate of the Pop III massive BH-BHs dominates that of Pop I BH-BHs.
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