论文标题
人口III星级何时结束？
When did Population III star formation end?
论文作者
论文摘要
我们通过将宇宙学仿真数据与半分析模型相结合，构建了一个研究人群III（POP III）星形成人群III（POP III）的形成。我们发现，由于辐射反馈（即Lyman-Werner和电离辐射）巨大的光环（$ M _ {\ rm halo} \ gtrsim 10^{9} {9} \ \ \ \ \ \ \ rm m _ {\ odot} $）是主要的（$ \ gtrsim 90 $％$ Z $ ZT $ ZT $ ZT $ ZT $ ZT $ ZT $ ZT）金属贫困气体的口袋可以生存，形成流行的III星，在超新星释放的金属效率低下。金属混合是一个关键过程，不仅可以确定\ textIt {active} pop iii星的总质量$ m _ {\ rm popiii} $确定$ m _ {\ rm popiii} $的总质量，这是每个主机halo，这是直接检测和识别POP III主机的关键参数。由于我们对结构形成期间金属混合的了解有限，这两个方面仍然不确定。当前的预测范围从回离的早期终止（$ z \ sim 5 $）到连续的流行III星星形成延长至$ z = 0 $，以不可忽视的费率$ \ sim 10^{ - 7} \ \ \ \ \ \ \ \ \ rm m _ {\ odot} \ odot} popiii} \ sim 10^{3} -10^{6} \ \ rm m _ {\ odot} $。这导致了直接检测POP III主机的广泛的红移极限，$ z {\ rm popiii} \ sim 0.5-12.5 $，检测率$ \ sillesim 0.1-20 \ \ rm arcmin arcmin^{ - 2} $，用于当前和未来的太空电视（E. e.g.g. hsst and jw firs）。我们的模型还预测，宇宙体积的大多数（$ \ gtrsim 90 $％）被无金属气体占据。测量该无金属相的体积填充分数可以限制金属混合参数和POP III星形成。
We construct a theoretical framework to study Population III (Pop III) star formation in the post-reionization epoch ($z\lesssim 6$) by combining cosmological simulation data with semi-analytical models. We find that due to radiative feedback (i.e. Lyman-Werner and ionizing radiation) massive haloes ($M_{\rm halo}\gtrsim 10^{9}\ \rm M_{\odot}$) are the major ($\gtrsim 90$%) hosts for potential Pop III star formation at $z\lesssim 6$, where dense pockets of metal-poor gas may survive to form Pop III stars, under inefficient mixing of metals released by supernovae. Metal mixing is the key process that determines not only when Pop III star formation ends, but also the total mass, $M_{\rm PopIII}$, of \textit{active} Pop III stars per host halo, which is a crucial parameter for direct detection and identification of Pop III hosts. Both aspects are still uncertain due to our limited knowledge of metal mixing during structure formation. Current predictions range from early termination at the end of reionization ($z\sim 5$) to continuous Pop III star formation extended to $z=0$ at a non-negligible rate $\sim 10^{-7}\ \rm M_{\odot}\ yr^{-1}\ Mpc^{-3}$, with $M_{\rm PopIII}\sim 10^{3}-10^{6}\ \rm M_{\odot}$. This leads to a broad range of redshift limits for direct detection of Pop III hosts, $z_{\rm PopIII}\sim 0.5-12.5$, with detection rates $\lesssim 0.1-20\ \rm arcmin^{-2}$, for current and future space telescopes (e.g. HST, WFIRST and JWST). Our model also predicts that the majority ($\gtrsim 90$%) of the cosmic volume is occupied by metal-free gas. Measuring the volume filling fractions of this metal-free phase can constrain metal mixing parameters and Pop III star formation.
