发表机构
Instituto de Fisica de Cantabria (CSIC-Universidad de Cantabria); University of Southampton; National Observatory of Athens（坎塔布里亚物理研究所（西班牙科学研究中心-坎塔布里亚大学）; 南安普顿大学; 雅典国家天文台）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过VIPERS和Stripe 82数据，发现暗晕质量与恒星形成活动的关系依赖星系形态，bulge主导星系中该联系更强，而盘主导星系中较弱。
AI 中文摘要
理解星系中恒星形成熄灭的机制，需要厘清内部结构与大规模环境的各自作用。我们研究了星系形态和比恒星形成率（sSFR）与宿主暗物质晕（DMHs）典型质量之间的关系，以及暗晕—恒星形成联系是否依赖于形态。我们分析了VIPERS和Stripe 82天区中$0.5 \leq z \leq 1.2$的非活动星系，结合基于DESI的Sérsic分类以及来自光谱能量分布拟合的恒星质量和恒星形成率。星系被分为盘主导和 bulge 主导系统，并按分位数划分sSFR区间，以尽量减少形态之间的恒星质量差异。每个区间以其$\u0394{\rm MS}=\log {\rm SFR}-\log {\rm SFR}_{\rm MS}$中位数表征，特征暗晕质量则通过投影星系互相关函数推断。暗晕质量与恒星形成活动的关系强烈依赖于形态：盘主导星系在所探测的$\Delta{\rm MS}$范围内暗晕质量变化很小，而bulge主导星系在高$\Delta{\rm MS}$时占据较低质量的暗晕，在较低$\Delta{\rm MS}$时则占据较高且彼此一致的暗晕质量。这些趋势不太可能主要由恒星质量差异驱动。因此，典型暗晕质量本身并不能直接对应到熄灭状态；相反，暗晕环境与恒星形成活动之间的联系在bulge主导星系中比在盘主导星系中更强。
英文摘要
Understanding the mechanisms responsible for quenching star formation in galaxies requires disentangling the roles of internal structure and large-scale environment. We investigate how galaxy morphology and specific star formation rate (sSFR) relate to the typical masses of host dark-matter halos (DMHs), and whether the halo--star formation connection depends on morphology. We analyse non-active galaxies in the VIPERS and Stripe 82 fields at $0.5 \leq z \leq 1.2$, combining DESI-based Sérsic classifications with stellar masses and SFRs from spectral energy distribution fitting. Galaxies are separated into disc- and bulge-dominated systems and divided into quantile-based sSFR bins designed to minimise stellar-mass differences between morphologies. Each bin is characterised by its median $Δ{\rm MS}=\log {\rm SFR}-\log {\rm SFR}_{\rm MS}$, and characteristic DMH masses are inferred from projected galaxy cross-correlations. The halo-mass relation with star formation activity depends strongly on morphology: disc-dominated galaxies show little variation in halo mass across the probed $Δ{\rm MS}$ range, whereas bulge-dominated galaxies occupy lower-mass halos at high $Δ{\rm MS}$ and higher, mutually consistent halo masses toward lower $Δ{\rm MS}$. These trends are unlikely to be driven mainly by stellar-mass differences. Typical halo mass alone therefore does not map cleanly onto quiescence; instead, the connection between halo environment and star formation activity is stronger in bulge-dominated than in disc-dominated galaxies.
CommentsA&A accepted, abstract has been abridged
