来自核星团中第一批恒星遗迹的引力波
Gravitational waves from the remnants of the first stars in nuclear star clusters
摘要：
我们研究人口III（Pop III）的二进制残留合并在核星团（NSC）的早期结构形成的半分析方法。在这个框架内，我们跟踪的动力学的Pop III二进制（紧凑的对象）残留物在宇宙结构形成过程中，并构建人口的Pop III二进制残留物落入NSCs的动力学摩擦的场星。神经干细胞内随后的演化则来自三体相遇和引力波（GW）发射。我们发现7.5%的Pop III双星残骸将落入星系中心（$< 3\ \rm pc$）。这些双星中约有$5-50\%$将在NSCs中以$z>0$合并，包括那些初始分离非常大的双星（高达1~pc）。合并率密度（MRD）在$z\sim 5-7$与$\sim 0.4-10\ \rm yr^{-1}\ \rm Gpc^{-3}$处达到峰值，导致第三代GW探测器的探测率$\sim 170-2700\ \rm yr^{-1}$可以达到$z\sim 10$。低质量（$\lesssim 10^{6}\ \rm M_{\odot}$）NSC形成于高红移（$z\gtrsim 4.5$）主机大多数（$\gtrsim 90\%$）我们的合并，其中主要包括黑洞（BH）的质量$\sim 40-85\ \rm M_{\odot}$，类似于LIGO事件中发现的最大质量的BH。特别是，我们的模型可以产生像GW 190521涉及BH在标准质量间隙的脉动对不稳定超新星的MRD $\sim 0.01-0.09\ \rm yr^{-1}\ Gpc^{-3}$在$z\sim 1$，与LIGO推断一致。
英文摘要：
We study Population III (Pop III) binary remnant mergers in nuclear star clusters (NSCs) with a semi-analytical approach for early structure formation. Within this framework, we keep track of the dynamics of Pop III binary (compact object) remnants during cosmic structure formation, and construct the population of Pop III binary remnants that fall into NSCs by dynamical friction of field stars. The subsequent evolution within NSCs is then derived from three-body encounters and gravitational-wave (GW) emission. We find that 7.5% of Pop III binary remnants will fall into the centres ($< 3\ \rm pc$) of galaxies. About $5-50\%$ of these binaries will merge at $z>0$ in NSCs, including those with very large initial separations (up to 1~pc). The merger rate density (MRD) peaks at $z\sim 5-7$ with $\sim 0.4-10\ \rm yr^{-1}\ \rm Gpc^{-3}$, leading to a promising detection rate $\sim 170-2700\ \rm yr^{-1}$ for 3rd-generation GW detectors that can reach $z\sim 10$. Low-mass ($\lesssim 10^{6}\ \rm M_{\odot}$) NSCs formed at high redshifts ($z\gtrsim 4.5$) host most ($\gtrsim 90\%$) of our mergers, which mainly consist of black holes (BHs) with masses $\sim 40-85\ \rm M_{\odot}$, similar to the most massive BHs found in LIGO events. Particularly, our model can produce events like GW190521 involving BHs in the standard mass gap for pulsational pair-instability supernovae with a MRD $\sim 0.01-0.09\ \rm yr^{-1}\ Gpc^{-3}$ at $z\sim 1$, consistent with that inferred by LIGO.
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