arXiv 2512.062712025-12-06astro-ph.GA

CLASSY XIV：氮的例外——高红移类比中的多相富集与反馈

CLASSY XIV: The Nitrogen Exception -- Multi-Phase Enrichment and Feedback in High-$z$ Analogs

Space Telescope Science Institute（太空望远镜科学研究所）；Observatoire de Paris, Université PSL, CNRS, Sorbonne Université（巴黎天文台，巴黎文理研究大学，法国国家科学研究中心，索邦大学）；University of Edinburgh（爱丁堡大学）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；Johns Hopkins University（约翰斯·霍普金斯大学）；Rutgers University（罗格斯大学）；University of Hertfordshire（赫特福德大学）

Bethan L. James, Valentina Abril-Melgarejo, Karla Z. Arellano-Córdova, Adarsh Ranjan, Kaelee S. Parker, Danielle A. Berg, Matilde Mingozzi, Alessandra Aloisi, J… 展开作者

Bethan L. James, Valentina Abril-Melgarejo, Karla Z. Arellano-Córdova, Adarsh Ranjan, Kaelee S. Parker, Danielle A. Berg, Matilde Mingozzi, Alessandra Aloisi, John Chisholm, Timothy Heckman, Alaina Henry, Svea Hernandez, Kristen B. W. McQuinn, Xinfeng Xu, Chiaki Kobayashi, The CLASSY Collaboration

备注：: 32 pages, 15 figures, 10 tables, submitted to ApJ

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AI总结：

研究通过分析多相富集和反馈机制，揭示了恒星形成星系中氮和氧丰度的差异及其与恒星质量、喷流速度等参数的关系。

摘要：

我们首次对31个本地恒星形成星系的两个星际介质（ISM）相的金属含量进行了分析，这些星系来自COS Legacy Archive Spectroscopic SurveY（CLASSY）数据库，被选为高红移系统的类比。利用共空间的紫外吸收和光学发射线光谱学，我们比较了N、O、S和Fe在低电离（中性）和高电离（电离）气体中的丰度，提供了在当前恒星爆发后不久以及在更长时间尺度上当来自先前事件的抛射物冷却并混合后的多相视图。我们发现O和S，主要由短寿命的大质量恒星产生，两种相之间混合良好，散射反映局部不均匀性。Fe主要由Ia型超新星在约10亿年的时间尺度上产生，在中性气体中更高，这反映了较老的Fe富集材料的延迟混合或通过核心坍缩超新星抛射物中尘埃形成导致Fe在电离相中的优先消耗。N表现出最大的相位偏移，N/H_ion系统性地比N/H_neu高约0.7个数量级，这种偏移的幅度与恒星质量、金属icity、恒星形成率以及最强烈地与ISM喷流速度相关。在电离相中，N/O比值在3-6 Myr内相对于中性气体迅速上升，与N富集主要由沃尔夫-雷亚特星而非中间质量AGB星主导一致，在更长时间尺度上。这些结果表明，局部恒星反馈、喷流和相依赖混合共同调节恒星形成星系的化学演化，为最近在宇宙黎明时期观测到的极端N/O丰度提供了关键见解。

英文摘要：

We present a first-of-its-kind analysis of the metal content across two interstellar medium (ISM) phases in a sample of 31 local star-forming galaxies from the COS Legacy Archive Spectroscopic SurveY (CLASSY), selected as analogues of high-$z$ systems. Using co-spatial UV absorption and optical emission-line spectroscopy, we compare abundances of N, O, S, and Fe in the low-ionization (neutral) and high-ionization (ionized) gas, providing a multi-phase view of enrichment shortly after the current starburst and over longer timescales when ejecta from previous episodes have cooled and mixed. We find that O and S, produced predominantly in short-lived massive stars, are well mixed between the two phases, with scatter reflecting local inhomogeneities. Fe, predominantly produced by Type Ia supernovae on $\sim$1 Gyr timescales, is higher in the neutral gas, reflecting either delayed mixing of older Fe-enriched material or preferential depletion of Fe from the ionized phase through dust formation in core-collapse supernova ejecta. N exhibits the largest phase offset, with N/H$_{ion}$ systematically $\sim$0.7 dex higher than N/H$_{neu}$, and the magnitude of this offset correlates with stellar mass, metallicity, star-formation rate, and most strongly with the ISM outflow velocity. N/O ratios in the ionized phase rise rapidly within 3-6 Myr relative to the neutral gas, consistent with N enrichment dominated by Wolf-Rayet stars rather than intermediate-mass AGB stars on longer timescales. These results demonstrate that localized stellar feedback, outflows, and phase-dependent mixing collectively regulate the chemical evolution of star-forming galaxies, providing key insight into the extreme N/O abundances recently observed in galaxies at cosmic dawn.

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