arXiv 1507.081472015-07-29astro-ph.GAastro-ph.CO

Pop III和Pop II在宇宙再电离过程中的近红外辐射背景、引力波背景和恒星形成率

The near-infrared radiation background, gravitational wave background and star formation rate of Pop III and Pop II during cosmic reionization

Y. P. Yang, F. Y. Wang, Z. G. Dai

备注：: 12 pages, 7 figures, accepted by A&A
发表信息：: A&A 582, A7 (2015)
DOI：: 10.1051/0004-6361/201525623

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摘要：

在本文中，我们得到了早期恒星的NIRB和SBGW，这是由再电离和恒星形成率的观测约束。通过考虑再电离和金属富集演化的不同星族的恒星形成模型，研究了从Pop III到Pop II星的转变。我们计算了两个主要的金属污染通道所产生的超新星驱动的原星系外流和“遗传通道”。我们得到了Pop III和Pop II的SFR以及它们的NIRB和SBGW辐射。我们预测富金属IGM星系（通过“遗传通道”被污染的星系）的金属丰度上限在$z\sim13$（$z\sim11$）达到$Z_{\rm crit}=10^{-3.5}Z_{\odot}$，这与我们的恒星形成模型是一致的。我们从再电离观测的角度对Pop III星的SFR进行了约束。对于$z>6$，在$\sim 1 μm$处，NIRB的峰强度约为$0.03-0.2~nW m^{-2}{sr}^{-1}$。NIRB信号的预测结果与金属丰度的演化趋势一致。我们还得到了这些早期恒星形成的黑洞的引力波背景。预测的引力波背景有一个峰值振幅$Ω_{GW}\simeq8\times10^{-9}$在$ν=158$ Hz的Pop II恒星遗迹。然而，Pop III.2恒星产生的背景比Pop II恒星小得多，在$ν=28~Hz$处有一个峰值幅度为$Ω_{GW}\simeq1.2\times10^{-11}$。Pop III.1的背景向低频移动，并且由于缺少来自具有$140~M_{\odot}<M_\ast<260~M_{\odot}$的恒星的引力波信号，Pop III.1恒星的$Ω_{GW}$振幅在$ν\simeq 10$ Hz处出现最小值。

英文摘要：

In this paper, we obtain the NIRB and SBGWs from the early stars, which are constrained by the observation of reionization and star formation rate. We study the transition from Pop III to Pop II stars via the star formation model of different population, which takes into account the reionization and the metal enrichment evolution. We calculate the two main metal pollution channels arising from the supernova-driven protogalactic outflows and "genetic channel". We obtain the SFRs of Pop III and Pop II and their NIRB and SBGWs radiation. We predict that the upper limit of metallicity in metal-enriched IGM (the galaxies whose polluted via "genetic channel") reaches $Z_{\rm crit}=10^{-3.5}Z_{\odot}$ at $z\sim13$ ($z\sim11$), which is consistent with our star formation model. We constrain on the SFR of Pop III stars from the observation of reionization. The peak intensity of NIRB is about $0.03-0.2~nW m^{-2}{sr}^{-1}$ at $\sim 1 μm$ for $z>6$. The prediction of NIRB signal is consistent with the metallicity evolution. We also obtain the gravitational wave background from the black holes formed by these early stars. The predicted gravitational wave background has a peak amplitude of $Ω_{GW}\simeq8\times10^{-9}$ at $ν=158$ Hz for Pop II star remnants. However, the background generated by Pop III.2 stars is much less than Pop II stars, with a peak amplitude of $Ω_{GW}\simeq1.2\times10^{-11}$ at $ν=28~Hz$. The background of Pop III.1 shifts to lower frequencies, and the amplitude of $Ω_{GW}$ for Pop III.1 stars shows a minimum value at $ν\simeq 10$ Hz, due to the lack of gravitational wave signals from the stars with $140~M_{\odot}<M_\ast<260~M_{\odot}$.

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