发表机构
INAF – Osservatorio Astronomico di Roma; Centro de Astrobiología (CAB), CSIC-INTA; European Space Agency (ESA); Space Telescope Science Institute (STScI); Scuola Normale Superiore; Peking University; University of Michigan; Indiana University（罗马天文台; 天体生物学中心; 欧洲航天局; 太空望远镜科学研究所; 比萨高等师范学院; 北京大学; 密歇根大学; 印第安纳大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
该研究分析z=9.878的透镜星系GHZ1，发现其质量大、尘埃少、恒星形成活跃，化学丰度符合标准演化，为理解早期星系演化提供关键参考。
AI 中文摘要
[删节版] 詹姆斯·韦布空间望远镜（JWST）运行的最初几年揭示了一个令人惊讶的$z \gtrsim 10$紫外明亮天体数量，其中许多天体的特征是紧凑性、异常的化学丰度模式和复杂的星际介质物理（例如，氮增强系统）。为了评估这些天体是早期星系演化的一个阶段还是一个特殊群体，理解该时期没有异常丰度模式的系统的物理至关重要。我们详细分析了GHZ1（$z=9.878$），一个在Abell2744场中适度（$\mu = 1.715$）透镜化的紫外明亮（$M_{UV} = -20.07$）星系，其特征是延伸的尺寸（$R_{e} \sim 410$ pc）。这些性质与许多氮增强星系的性质形成对比，使GHZ1成为评估早期星系演化的主要驱动因素和差异起源的绝佳实验室。通过JWST的NIRSpec（PRISM-CLEAR配置）和MIR/LRS光谱观测，我们分析了GHZ1的完整紫外和光学发射。我们使用光谱-测光SED拟合来表征恒星演化，并使用发射线光谱来约束其化学增丰。我们发现GHZ1是$z\sim 10$处最庞大的系统之一（log(M$_{\star}$ [M$_{\odot}$]) = 9.17$_{-0.26}^{+0.27}$），具有中等程度的尘埃消光（$A_{V} = 0.21_{-0.12}^{+0.12}$~mag）和持续的恒星形成（在过去10 Myr内中值SFR $= 8.75_{-1.72}^{+1.71}$ M$_{\odot}\cdot$yr$^{-1}$）。其化学增丰模式（12+log(O/H) = $7.81_{-0.11}^{+0.12}$，log(C/O) = $-0.66_{-0.13}^{+0.13}$，log(N/O)$< -1.04$）与大质量恒星初级产生主导的标准演化一致。我们还推导出H$\alpha$/H$\beta$巴耳末比值低于Case B预测。我们推测[...]。
英文摘要
[Abridged] The first operating years of the James Webb Space Telescope (JWST) have revealed a surprising number of $z \gtrsim 10$ UV-bright objects, many of them characterized by their compactness, anomalous chemical abundance patterns and complex ISM physics (e.g. N-enhanced systems). To assess whether these objects are a phase of early galaxy evolution or a peculiar population, it is essential to understand the physics of systems without anomalous abundance patterns in this epoch. We present a detailed analysis of GHZ1 ($z=9.878$), a moderately ($μ= 1.715$) lensed UV-bright ($M_{UV} = -20.07$) galaxy in the Abell2744 field, characterized by an extended size ($R_{e} \sim 410$ pc). These properties, which contrast with the properties of many of the N-enhanced galaxies, make GHZ1 an excellent laboratory to assess what are the major drivers of early galaxy evolution and the origin of the differences. By means of JWST spectroscopic observations from NIRSpec (PRISM-CLEAR configuration) and the MIR/LRS, we analyzed the full UV and optical emission from GHZ1. We used a spectro-photometric SED fitting to characterize the stellar evolution and the emission line spectra to constrain its chemical enrichment. We find that GHZ1 is among the most massive systems at $z\sim 10$ (log(M$_{\star}$ [M$_{\odot}$]) = 9.17$_{-0.26}^{+0.27}$), with a moderate amount of dust attenuation ($A_{V} = 0.21_{-0.12}^{+0.12}$~mag) and ongoing star formation (with a median SFR $= 8.75_{-1.72}^{+1.71}$ M$_{\odot}\cdot$yr$^{-1}$ over the last 10 Myr). Its chemical enrichment patterns (12+log(O/H) = $7.81_{-0.11}^{+0.12}$, log(C/O) = $-0.66_{-0.13}^{+0.13}$, log(N/O)$< -1.04$) are consistent with a standard evolution dominated by primary production from massive stars. We also derive an H$α$/H$β$ Balmer ratio below Case B predictions. We speculate that [...].
Comments23 pages, 19 figures. Submitted to A&A
