欧几里得快速数据发布（Q1）：通过近期熄灭星系探索熄灭过程在时间、环境和质量上的复杂性
Euclid Quick Data Release (Q1). Exploring the complexity of quenching processes across time, environment, and mass through recently quenched galaxies
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- INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚天体物理与空间科学天文台）
- Astronomical Institute, Tohoku University（东北大学天文学研究所）
- Alma Mater Studiorum Università di Bologna（博洛尼亚大学）
- University of Geneva（日内瓦大学）
- CEA Saclay（萨克雷法国原子能和替代能源委员会）
- INAF-Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）
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中文总结 AI 辅助
本研究利用欧几里得Q1数据，通过UVJ颜色分类识别近期熄灭星系，分析其比例、效率及性质随红移和环境的变化，揭示快速与缓慢熄灭机制及形态转变，证明欧几里得在星系熄灭研究中的潜力。
中文摘要 AI 辅助
近期熄灭星系（RQGs）为理解星系熄灭提供了洞见。我们利用欧几里得首次快速数据发布（Q1）对RQGs进行了光度与光谱分析。利用静止系UVJ颜色，我们在0.2<z<3.0的红移范围内将星系分类为恒星形成星系（SFGs）、宁静星系（QGs）和近期熄灭星系，并依据模型演化轨迹将RQGs分为快速熄灭型（fRQGs）和缓慢熄灭型（sRQGs）。RQGs的相对比例及其熄灭效率均随宇宙时间下降。在早期宇宙，快速熄灭在大质量星系中更为高效，而在晚期宇宙，它仅在低质量星系中变得高效。缓慢熄灭在z<1.5时变得更加高效，并随宇宙时间从高质量星系向中等质量星系推进。在z<0.5时，大多数RQGs位于低密度环境中，而在z>0.5时它们也存在于高密度环境中，这表明在致密区域中熄灭发生得更早。RQGs在恒星质量、恒星形成率、比恒星形成率、Sersic指数和半径方面表现出介于SFGs和QGs之间的中间性质。大多数RQGs呈现规则形态，排除了并合作为主要机制。我们发现fRQGs保持盘状形态，而sRQGs更为集中，表明它们处于形态转变的不同阶段。我们的分析表明多种机制驱动熄灭。具有光谱红移的星系的叠加光谱证实了QGs中古老、被动的恒星族群，而sRQGs的光谱显示出微弱的Hα发射，表明存在残余的恒星形成活动或活动星系核（AGN）的贡献。RQGs的近期熄灭性质通过DESI叠加光谱中强烈的巴尔默吸收线得到确认。叠加的欧几里得QG光谱与之前的模板以及年龄大于5Gyr（z<1）的恒星族群模型一致。这些结果展示了欧几里得在研究星系熄灭方面的潜力，未来的数据发布将进一步提升这一能力。
英文摘要
Recently quenched galaxies (RQGs) provide insights into galaxy quenching. We present a photometric and spectroscopic analysis of RQGs using the first Euclid Quick Data Release (Q1). Using rest-frame UVJ colours, we classify star-forming (SFGs), quiescent (QGs), and recently quenched galaxies at 0.2<z<3.0, separating RQGs into fast- and slow-quenching types (fRQGs and sRQGs) following model evolutionary tracks. The relative fractions of RQGs and their quenching efficiencies both decrease with cosmic time. At early epochs, fast quenching is more efficient in massive galaxies, whereas it becomes efficient only at low masses at later epochs. Slow quenching becomes more efficient at z<1.5, progressing from high to intermediate masses with cosmic time. Most RQGs at z<0.5 reside in low-density environments, while they also exist in high-density environments at z>0.5, suggesting earlier quenching in dense regions. RQGs show intermediate properties between SFGs and QGs in stellar mass, star-formation rate, specific star-formation rate, Sersic index, and radius. Most RQGs exhibit regular morphologies, excluding merger as a primary mechanism. We find that fRQGs retain disc-like morphologies, whereas sRQGs are more concentrated, suggesting different stages of morphological transformation. Our analysis suggests that multiple mechanisms drive quenching. Stacked spectra of galaxies with spectroscopic redshifts confirm old, passive populations in QGs, while sRQG spectrum shows weak Ha emission, indicating residual star-formation activity or AGN contribution. The recently-quenched nature of RQGs is confirmed by strong Balmer absorption lines in stack DESI spectra. The stacked Euclid QG spectrum agrees with previous templates and stellar population models older than 5Gyr at z<1. These results demonstrate Euclid's potential for studying galaxy quenching, to be further enhanced by future releases.[Abrg.]
