发表机构
NSF NOIRLab, Gemini Observatory; International Gemini Observatory/NSF NOIRLab; INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna; Institute for Theoretical Physics, Heidelberg University; Max-Planck-Institut für Astrophysik; Max-Planck-Institut für Astronomie; INAF-Osservatorio di Astrofisica e Scienza dello Spazio; Dipartimento di Fisica Enrico Fermi, Università di Pisa（美国国家光学红外天文实验室，双子座天文台; 国际双子座天文台/美国国家光学红外天文实验室; 意大利国家天体物理研究所博洛尼亚天文与空间科学观测站; 海德堡大学理论物理研究所; 马克斯·普朗克天体物理学研究所; 马克斯·普朗克天文学研究所; 意大利国家天体物理研究所天文与空间科学观测站; 比萨大学恩里科·费米物理系）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
基于JWST Aether巡天，发现三个z>6的强FeII类星体，其FeII强度极高，黑洞质量各异，表明宇宙黎明时期已存在快速增丰和增长的黑洞，并揭示了环境与射电性质的多样性。
AI 中文摘要
我们展示了在z>6时类星体主序列上的三个异常天体，这是由JWST/NIRSpec IFU观测从Aether巡天中揭示的，该巡天计划针对宇宙黎明时期约200个类星体。这些类星体J0216-5226、J0320-3521和J1429+5447表现出异常强的FeII发射和弱的Hβ及[OIII]谱线，表明在宇宙历史的最初10亿年内发生了快速的化学增丰。它们的FeII强度（$R_{\rm{FeII},\lambda4570} \equiv \rm{EW}_{\rm{FeII}}/\rm{EW}_{\rm{H}\beta}$）范围在约2.5-3.6之间，使它们跻身于SDSS类星体在（$0\lesssim z\lesssim 1$）中的前约3%。J0216-5226和J1429+5447的Hα发射线暗示黑洞质量约为$\sim1-7\times10^9$ M$_{\odot}$，其$\lambda_{\rm{Edd}}\sim0.1-0.6$，与典型的高红移类星体相当，尽管在强FeII发射体中，维里黑洞质量可能被系统性高估。相比之下，J0320-3521拥有一个质量较低的黑洞，约为$\sim0.2-2\times10^9$ M$_{\odot}$，表明可能存在超爱丁顿速率吸积，其$\lambda_{\rm{Edd}}$约为0.5-6.0。J0320-3521的IFU数据揭示了一个投影距离约1.5千秒差距的明显发射线区域，这与相互作用的伴星系或与类星体相关的电离气体一致。我们进一步识别了J1429+5447周围的复杂环境，包括两个候选伴星系或延伸的电离气体结构。这些具有明亮发射线区域的类星体J0320-3521和J1429+5447是射电噪源，而J0216-5226在射电波段未被探测到（$R_{5\rm{GHz,} \\,3\sigma}\lesssim4$）。综合来看，这些结果证实了先前的发现，即高度增丰、快速增长的黑洞在宇宙黎明时期已经存在。尽管样本量较小，我们的结果进一步强调了在类星体基本平面中共享相同极端区域的类星体之间，其环境和射电喷流性质的多样性。
英文摘要
We present three outliers on the quasar main sequence at z>6, as revealed by JWST/NIRSpec IFU observations from the Aether survey, a program targeting ~200 quasars at cosmic dawn. The quasars, J0216-5226, J0320-3521, and J1429+5447, exhibit exceptionally strong FeII emission and weak H$β$ and [OIII] lines, indicating rapid chemical enrichment within the first Gyr of cosmic history. Their FeII strengths ($R_{\rm{FeII},\lambda4570} \equiv \rm{EW}_{\rm{FeII}}/\rm{EW}_{\rm{H}β}$) range between ~2.5-3.6, placing them among the top ~3% of SDSS quasars at ($0\lesssim z\lesssim 1$). The H$α$ emission lines of J0216-5226 and J1429+5447 imply black hole masses of $\sim1-7\times10^9$ M$_{\odot}$ with $λ_{\rm{Edd}}\sim0.1-0.6$, comparable to typical high-z quasars, although virial black hole masses may be systematically overestimated in strong FeII emitters. In contrast, J0320-3521 hosts a lower mass black hole of $\sim0.2-2\times10^9$ M$_{\odot}$, suggesting possible super-Eddington rate accretion with $λ_{\rm{Edd}}$~0.5-6.0. The IFU data of J0320-3521 reveal a distinct emission-line region at a projected distance of ~1.5 kpc, consistent with either an interacting companion or ionized gas associated to the quasar. We further identify a complex environment around J1429+5447, including two candidate companion galaxies or extended ionized gas structures. These quasars with bright emission-line regions, J0320-3521 and J1429+5447, are radio-loud sources, while J0216-5226 remains undetected in radio ($R_{5\rm{GHz,} \,3σ}\lesssim4$). Together, these results confirm previous findings that highly enriched, rapidly growing black holes were already in place at cosmic dawn. Despite the small sample size, our results further highlight the diversity in environment and radio-jet properties among quasars that otherwise share the same extreme region of the quasar fundamental plane.
CommentsAccepted for publication in The Astrophysical Journal, 19 pages, 11 figures
