Pop III星团的质量分布：A-SLOTH对JWST可观测性的预测
Mass distribution of Pop III star clusters: A-SLOTH predictions for JWST observability
AI总结：
利用半解析代码A-SLOTH，结合扩展Press-Schechter形式和N体模拟，预测Pop III星暴晕的巴尔默线流量，发现JWST/NIRSpec在5≤z≤11下无法探测到这些线，因为所需的大质量Pop III星团在物理上难以形成。
摘要：
本研究旨在模拟Pop III星暴晕的前四条巴尔默系跃迁的预期光度，并评估其在$5 \le z \le 11$范围内被JWST/NIRSpec探测的可能性，同时检验可探测性所需的大质量Pop III恒星系统在物理上是否预期形成。我们使用半解析代码A-SLOTH，结合从扩展Press-Schechter (EPS)形式构建的并合树和针对类银河晕及8 Mpc$/h$盒子中晕群体的宇宙学$N$体模拟。将预测的谱线流量与从曝光时间计算器(ETC)导出的JWST探测极限进行比较，假设信噪比为5的10,000秒NIRSpec曝光。对于我们的默认模型参数，Pop III H$\alpha$流量峰值约为$\sim10^{-20}$ erg s$^{-1}$ cm$^{-2}$，比JWST探测阈值($\sim6\times10^{-19}$ erg s$^{-1}$ cm$^{-2}$)低1-2个数量级。其他巴尔默线比H$\alpha$更弱，同样无法探测。这是因为在我们的模型中，产生可探测巴尔默发射所需的大质量Pop III恒星系统并未形成。Pop III恒星形成以短暂的、反馈调节的爆发进行，这些爆发因辐射和超新星反馈而终止，产生的年轻Pop III恒星质量仅为$\sim10^{1}$-$10^{4}\\ \mathrm{M}_\odot$。相比之下，可探测的巴尔默发射需要Pop III恒星质量$M_{\star,\mathrm{III}}\gtrsim 10^{5}\\ \mathrm{M}_\odot$，具体取决于可观测红移。
英文摘要：
This study aims to model the expected luminosities of the first four Balmer-series transitions from Pop.\,III star-forming halos and assess their detectability with JWST/NIRSpec across $5 \le z \le 11$, while testing whether the massive Pop.\,III stellar systems required for detectability are physically expected to form. We use the semi-analytical code A-SLOTH with merger trees constructed from the extended Press-Schechter (EPS) formalism and cosmological $N$-body simulations targeting Milky Way-like halos and the halo population in an 8~Mpc$/h$ box. Predicted line fluxes are compared to JWST detection limits derived from the Exposure Time Calculator (ETC), assuming a 10\,000~s NIRSpec exposure at a signal-to-noise ratio of 5. For our default model parameters, Pop.\,III H$α$ fluxes peak at $\sim10^{-20}$\,erg\,s$^{-1}$\,cm$^{-2}$, 1--2 orders of magnitude below the JWST detection threshold ($\sim6\times10^{-19}$\,erg\,s$^{-1}$\,cm$^{-2}$). The other Balmer lines are weaker than H$α$ and are likewise undetectable. This is because, in our models, the massive Pop.\,III stellar systems required to generate detectable Balmer emission do not form. Pop.\,III star formation proceeds in short, feedback-regulated episodes that are terminated by radiative and supernova feedback, yielding young Pop.\,III stellar masses of only $\sim10^{1}$--$10^{4}\,\mathrm{M}_\odot$. In contrast, detectable Balmer emission would require Pop.\,III stellar masses of $M_{\star,\mathrm{III}}\gtrsim 10^{5}\,\mathrm{M}_\odot$, depending on the observable redshift.
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