将X射线发射与GAMA星系群中的星系种群联系起来
Linking X-ray emission to galaxy populations in GAMA groups
- Instituto de Astronomía Teórica y Experimental, CONICET - UNC（理论与实验天文学研究所，阿根廷国家科学研究委员会-科尔多瓦大学）
- Facultad de Matemática, Astronomía, Física y Computación, Universidad Nacional de Córdoba（数学、天文学、物理与计算学院，科尔多瓦国立大学）
- Observatorio Astronómico, Universidad Nacional de Córdoba（天文台，科尔多瓦国立大学）
- 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）
- IFPU-Institute for Fundamental Physics of the Universe（基础宇宙物理学研究所）
机构由 AI 辅助整理，请以论文原文为准。
中文总结 AI 辅助
本研究通过对比有/无X射线探测的GAMA星系群，发现可探测的热星系群内介质促进星系淬灭和快速转变，其作用超越暗晕质量，影响星系演化。
中文摘要 AI 辅助
我们研究了可探测的热星系群内介质的存在如何影响星系颜色和恒星形成特性，以及这些趋势如何依赖于星系群内的动力学阶段。我们分析了红移0.1 ≤ z ≤ 0.2范围内，具有和不具有X射线探测（XG和NXG）的GAMA星系群中的星系，使用了具有相似暗晕质量分布的样本，并与场对照样本进行了比较。星系根据紫外-光学颜色被分类为红色、绿色或蓝色，群星系进一步根据投影相空间位置和宿主暗晕质量划分为动力学类别。我们检查了星系种群作为轨道类别、恒星形成活动、核活动和星系群中心距离的函数。星系种群在XG中比在NXG中系统性地更加演化，蓝色和恒星形成星系比例更低，而红色和被动星系比例更高。绿色星系比例在不同环境和轨道类别中保持稳定，尽管高质量的新到达星系显示出轻微的绿色系统过剩，同时保持相对较高的恒星形成比例和较低的被动比例，这表明存在一个中间淬灭阶段。活动星系核比例没有显示出环境依赖性，而星暴后星系比例在XG中强烈增加，达到近20%，这与增强的快速淬灭一致。星系属性在XG中比在NXG中显示出更强的径向分离，即使在R/R200 ~ 3处，颜色比例也与场值不同，这与预处理一致。尽管暗晕质量分布相似，XG和NXG之间的系统性差异表明，仅暗晕质量并不能决定星系属性。可探测的热星系群内介质与增强的环境处理、更强的淬灭和更频繁的快速转变相关，这突出了星系群内介质的热力学状态（超越暗晕质量）在塑造星系群尺度上的星系演化中的作用。
英文摘要
We study how the presence of a detectable hot intragroup medium affects galaxy colour and star-formation properties, and how these trends depend on dynamical stage within the group. We analysed galaxies in GAMA groups with and without X-ray detection (XG and NXG) at 0.1 <= z <= 0.2, using samples with similar halo-mass distributions, compared with a field control sample. Galaxies were classified as red, green, or blue by UV-optical colour, and group galaxies further classified into dynamical classes based on projected phase-space position and host halo mass. We examined galaxy populations as a function of orbital class, star-formation activity, nuclear activity, and cluster-centric distance. The galaxy population is systematically more evolved in XG than NXG, with lower blue and star-forming fractions and higher red and passive fractions. The green fraction is stable across environments and orbital classes, though high-mass recent arrivals show a mild excess of green systems while retaining relatively high star-forming and low passive fractions, suggesting an intermediate quenching stage. The active galactic nucleus fraction shows no environmental dependence, while the post-starburst fraction increases strongly in XG, reaching nearly 20 percent, consistent with enhanced rapid quenching. Galaxy properties show stronger radial segregation in XG than NXG, with colour fractions differing from field values even at R/R200 ~ 3, consistent with preprocessing. Despite similar halo-mass distributions, the systematic differences between XG and NXG show that halo mass alone does not determine galaxy properties. A detectable hot intragroup medium is associated with enhanced environmental processing, stronger quenching, and more frequent rapid transitions, highlighting the role of the intragroup medium's thermodynamical state, beyond halo mass, in shaping galaxy evolution at group scales.
