VEGAS巡天中的Hydra I星系团星系族群 III. 低表面亮度特征与团内光的领域
Galaxy populations in the Hydra I cluster from the VEGAS survey III. The realm of low surface brightness features and intra-cluster light
AI总结：
本研究利用VEGAS项目的VST深场g/r波段图像分析Hydra I星系团低表面亮度结构与团内光，揭示核心、北部和东南部的不同演化过程，并估计团内光约占总光度12%。
摘要：
在本文中，我们分析了Hydra I星系团中的光分布，以探索其低表面亮度特征、测量团内光，并探讨该星系团的组装历史。为此，我们使用了作为VEGAS项目一部分、由VST获取的深场宽视场g波段和r波段图像。VST拼接图覆盖了星系团核心周围约0.4倍维里半径的范围，使我们能够将光分布测绘至μ_g约28 mag/arcsec^2的暗弱表面亮度水平。在星系团的这一区域内，有44个亮于m_B<16 mag的星系团成员，并且该区域包含300多个矮星系。与所有星系团成员（亮星系和矮星系）的投影分布相似，我们发现大部分星系光集中在星系团核心，该核心也发射X射线；此外还存在两个过密区：相对于星系团核心的北部（N）和东南部（SE）。我们展示了对所有明亮星系团成员光分布的分析。在移除前景恒星和其他天体后，我们测量了弥散的团内光，并将其分布与星系团中的球状星团和矮星系的分布进行了比较。我们发现，大多数弥散光低表面亮度特征以及星系间可能存在引力相互作用的迹象都位于核心和北部（N）群中，而冲压剥离经常被发现影响东南部（SE）群内的星系。所有这些特征证实该星系团中的质量组装仍在进行。通过将投影相空间与这些观测性质相结合，我们追踪了组装历史的不同阶段。我们还探讨了在星系团中探测到的团内光的主要形成通道；该团内光贡献了星系团总光度的约12%。
英文摘要：
In this paper, we analyse the light distribution in the Hydra I cluster of galaxies to explore their low surface brightness features, measure the intra-cluster light, and address the assembly history of the cluster. For this purpose, we used deep wide-field g- and r-band images obtained with the VST as part of the VEGAS project. The VST mosaic covers ~0.4 times the virial radius around the core of the cluster, which enabled us to map the light distribution down to faint surface brightness levels of mu_g ~ 28 mag/arcsec^2. In this region of the cluster, 44 cluster members are brighter than m_B<16 mag, and the region includes more than 300 dwarf galaxies. Similar to the projected distribution of all cluster members (bright galaxies and dwarfs), we find that the bulk of the galaxy light is concentrated in the cluster core, which also emits in the X-rays, and there are two overdensities: in the north (N) and south-east (SE) with respect to the cluster core. We present the analysis of the light distribution of all the bright cluster members. After removing foreground stars and other objects, we measured the diffuse intra-cluster light and compared its distribution with that of the globular clusters and dwarf galaxies in the cluster. We find that most of the diffuse light low surface brightness features, and signs of possible gravitational interaction between galaxies reside in the core and in the group in the N, while ram-pressure stripping is frequently found to affect galaxies within the SE group. All these features confirm that the mass assembly in this cluster is still ongoing. By combining the projected phase-space with these observed properties, we trace the different stages of the assembly history. We also address the main formation channels for the intra-cluster light detected in the cluster, which contributes ~ 12% to the total luminosity of the cluster.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
