AI 中文总结
利用JWST/NIRSpec PRISM在z>3系统搜寻[Ne V]发射，识别25个源，发现其光度与AGN重叠，主要由黑洞吸积驱动，可作为早期黑洞增长的探针。
AI 中文摘要
我们利用JWST/NIRSpec PRISM光谱在z>3处进行了首次系统性的高电离星云发射（SHINE）搜寻，使用[Ne V]λ3426发射线。从超过9000个星系中，我们识别出25个[Ne V]发射体，红移范围z=3.059-9.444，log10(L_[Ne V]/erg s^-1)=40.70-42.86。它们的[Ne V]光度与本地[Ne V]选活动星系核（AGN）的光度重叠，并超过本地贫金属[Ne V]发射体的光度，尽管这类低光度系统会低于我们的灵敏度。该群体具有多样性，涵盖紧凑和延展形态，以及广泛的连续谱性质和恒星质量范围，包括质量非常低的宿主星系。其中包含具有宽巴尔默发射的源，以及其他在更高分辨率光谱中不需要宽分量的源。[Ne V]发射体与传统AGN诊断仅部分重叠：大多数不满足基于强静止光学窄线比的保守高红移AGN标准，只有少数具有采纳的宽线分类。独立选择的宽线AGN和“小红点”的[Ne V]上限过浅，无法确立群体范围的[Ne V]缺失。六个源有可靠的Chandra对应体，表明X射线弱性在明亮[Ne V]发射体中并非普遍。强[Ne V]/[Ne III]发射与更红的紫外斜率及更强的巴尔默跃变相关，但与紫外光度无关，可能将强高电离发射与近期恒星形成变化联系起来。观测到的明亮[Ne V]发射发生率在z>3处无显著演化，尽管稳健的[Ne III]探测比例在增加。高[Ne V]光度和硬线比有利于黑洞吸积作为主导能源，确立了[Ne V]发射作为早期黑洞增长的补充探针。
英文摘要
We conduct the first systematic Search for High-Ionization Nebular Emission (SHINE) using [Ne V]$\lambda3426$ in JWST/NIRSpec PRISM spectroscopy at $z>3$. From more than 9,000 galaxies, we identify 25 [Ne V] emitters spanning $z=3.059$-$9.444$ and $\log_{10}(L_{\rm [Ne\,V]}/erg\,s^{-1})=40.70$-$42.86$. Their [Ne V] luminosities overlap with those of local [Ne V]-selected active galactic nuclei (AGNs) and exceed those of local metal-poor [Ne V] emitters, although such low-luminosity systems would fall below our sensitivity. The population is diverse, spanning compact and extended morphologies and a broad range of continuum properties and stellar masses, including very low-mass hosts. It includes sources with broad Balmer emission as well as others whose higher-resolution spectra do not require a broad component. The [Ne V] emitters overlap only partly with conventional AGN diagnostics: most do not satisfy conservative high-redshift AGN criteria based on strong rest-optical narrow-line ratios, and only a minority have adopted broad-line classifications. [Ne V] upper limits for independently selected broad-line AGNs and little red dots are too shallow to establish a population-wide [Ne V] deficit. Six sources have secure Chandra counterparts, showing that X-ray weakness is not universal among luminous [Ne V] emitters. Strong [Ne V]/[Ne III] emission is associated with redder ultraviolet slopes and stronger Balmer breaks, but not with UV luminosity, possibly linking strong high-ionization emission to recent changes in star formation. The observed incidence of luminous [Ne V] emission shows no significant evolution over $z>3$, despite an increasing robust [Ne III] detection fraction. The high [Ne V] luminosities and hard line ratios favor black-hole accretion as the dominant power source, establishing [Ne V] emission as a complementary probe of early black-hole growth.
CommentsApJ, submitted. Comments welcome and greatly appreciated
