JADES与CEERS中电离光子产生效率的光谱分析：对电离光子预算的启示
A spectroscopic analysis of the ionizing photon production efficiency in JADES and CEERS: implications for the ionizing photon budget
AI总结：
本文利用JADES和CEERS的JWST光谱数据测量163个高红移星系的电离光子产生效率，发现其随红移和紫外光度等参数显著变化，并结合再电离模型约束宇宙再电离结束于红移5至7。
摘要：
我们利用JADES和CEERS的合并样本，基于JWST/NIRSpec和JWST/NIRCam数据来约束电离光子产生效率（$ξ_{\ m ion}$）。我们研究了163个红移范围在1.06 < z < 6.71的天体，这些天体具有显著的（3$σ$）H$α$和H$β$光谱探测，以便通过巴尔末减缩修正星云尘埃消光，从而约束内禀H$α$光度。我们通过最佳拟合光谱能量分布模型约束尘埃修正后的紫外光度。在假设莱曼连续谱逃逸分数f$_{\ m esc}$=0的情况下，我们发现样本的中位log$_{10}$($ξ{\ m ion,0}$/erg Hz$^{-1}$) = $25.29^{+0.29}_{-0.37}$。我们发现$ξ_{\ m ion,0}$与红移z之间存在显著相关性，其中17个z > 4.64的天体的中位log$_{10}$($ξ_{\ m ion,0}$/erg Hz$^{-1}$) = $25.38^{+0.38}_{-0.38}$，而更低红移天体的中位log$_{10}$($ξ_{\ m ion,0}$/erg Hz$^{-1}$) = $25.24^{+0.30}_{-0.33}$。我们还发现$ξ_{\ m ion,0}$与LUV、Wλ([O iii])、[O iii]λ5007/[O ii]λλ3726, 3729之间存在显著的正相关，并与金属丰度存在反相关。与一些先前结果不同，我们发现$ξ_{\ m ion,0}$与恒星质量、恒星尘埃消光或紫外斜率之间没有趋势。将$ξ_{\ m ion,0}$、z和MUV的多元拟合应用于一个经验驱动的再电离模型，并结合Keck莱曼连续谱光谱巡天对z ~ 3处莱曼连续谱直接观测得到的f$_{\ m esc}$估计，我们发现进入星系际介质的电离光子数量使得再电离在z ~ 5 - 7结束。
英文摘要：
We have used a combined sample of JADES and CEERS objects in order to constrain ionizing photon production efficiency ($ξ_{\rm ion}$) from JWST/NIRSpec and JWST/NIRCam data. We examine 163 objects at 1.06 < z < 6.71 with significant (3$σ$) spectroscopic detections of H$α$ and H$β$ in order to constrain intrinsic H$α$ luminosities corrected from nebular dust attenuation via Balmer decrements. We constrain dust-corrected UV luminosities from best-fit spectral-energy distribution modeling. We find a sample median log$_{10}$($ξ{\rm ion,0}$/erg Hz$^{-1}$) = $25.29^{+0.29}_{-0.37}$, assuming f$_{\rm esc}$=0 for the escape fraction of Lyman continuum emission. We find significant correlation between $ξ_{\rm ion,0}$ and z, with 17 objects at z > 4.64 having median log$_{10}$($ξ_{\rm ion,0}$/erg Hz$^{-1}$) = $25.38^{+0.38}){-0.38}$, with those below having log$_{10}$($ξ_{\rm ion,0}$/erg Hz$^{-1}$) = $25.24^{+0.30}_{-0.33}$. We also find significant, positive correlations between $ξ_{\rm ion,0}$ and LUV; Wλ([O iii]); [O iii]λ5007/[O ii]λλ3726, 3729; and inverse correlations with metallicity. In contrast with some previous results, we find no trends between $ξ_{\rm ion,0}$ and stellar mass, stellar dust attenuation, or UV slope. Applying a multivariate fit to $ξ_{\rm ion,0}$, z, and MUV to an empirically-motivated model of reionization, and folding in f$_{\rm esc}$ estimates from direct observations of the Lyman continuum at z ~ 3 from the Keck Lyman Continuum Spectroscopic survey, we find that the number of ionizing photons entering the IGM causes reionization to end at z ~ 5 - 7.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
