Lyman-$\alpha$ 森林一维流量功率谱对 QSO 辅助再电离模型的约束
Lyman-$α$ forest 1D flux power spectrum constraints on QSO-assisted reionization models
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- University of Hertfordshire（赫特福德大学）
- University of Edinburgh（爱丁堡大学）
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中文总结 AI 辅助
利用 Lyman-$\alpha$ 森林功率谱约束 QSO 辅助再电离模型，发现 HeIII 区域温度提升改善拟合，并排除部分微弱 QSO 群体。
中文摘要 AI 辅助
最近的 JWST 观测揭示了在红移 4 < z < 6 处存在大量微弱的类星体（QSO）群体，其中包括一个高度红化的“小红点”亚群。我们利用 Lyman-$\alpha$ 森林一维流量功率谱对星系际介质（IGM）中热涨落的敏感性，对 QSO 的光谱特性施加统计约束。通过后处理来自 Sherwood-Relics 系列 Lyman-$\alpha$ 森林模拟的模拟 Lyman-$\alpha$ 森林光谱，并加入由 QSO 引起的 HeII 再电离，结合已发表的 4.2 < z < 5.0 之间 Lyman-$\alpha$ 森林一维流量功率谱的精密测量，我们发现，在 HeIII 区域内增加 IGM 的温度提升可以改善与测量功率谱的一致性。虽然“小红点”群体对 HeII 再电离的贡献与软光谱 QSO 的温和温度提升 $\Delta T_b=1\times10^4$ K 以及硬光谱 QSO 的 $\Delta T_b=2\times10^4$ K 均一致，但 JWST 发现的更大微弱 QSO 群体（$M_{\rm UV} > -21.6$）的贡献，如果其光谱足够硬，能够在 HeIII 区域将 IGM 温度提升 $\Delta T_b=2\times10^4$ K 或更高，则在 2$\sigma$ 水平上被排除。
英文摘要
Recent JWST observations have revealed a large population of faint Quasi-Stellar Objects (QSOs) at redshifts 4 < z < 6, including a highly reddened sub-population of Little Red Dots. We exploit the sensitivity of the Lyman-$α$ forest 1D flux power spectrum to thermal fluctuations in the Intergalactic Medium (IGM) to place statistical constraints on the spectral properties of the QSOs. By post-processing simulated Lyman-$α$ forest spectra from the Sherwood-Relics suite of Lyman-$α$ forest simulations with added HeII reionization by QSOs, in conjunction with published precision measurements of the Lyman-$α$ forest 1D flux power spectrum between 4.2 < z < 5.0, we find that the addition of temperature boosts of the IGM within the HeIII regions improves agreement with the measured power spectra. While the contribution of the Little Red Dot population to HeII reionization is consistent with both a mild temperature boost of $ΔT_b=1\times10^4$ K for soft spectra QSOs and $ΔT_b=2\times10^4$ K for hard spectra QSOs, a contribution from the larger population of faint QSOs found by JWST having $M_{\rm UV} > -21.6$ is excluded at the 2$σ$ level if their spectra are sufficiently hard to boost the IGM temperature in HeIII regions by $ΔT_b=2\times10^4$ K or greater.
