arXiv 1402.35942014-02-14astro-ph.COastro-ph.GA

星系团的性质。II。后溅镀锌板

Galaxy properties in clusters. II. Backsplash Galaxies

H. Muriel, V. Coenda

备注：: Accepted for publication in Astronomy & Astrophysics (A&A)
DOI：: 10.1051/0004-6361/201322033

摘要：

我们探索星系团的外围星系的属性和它们对最近的动力学历史的依赖，以了解星系团核心对星系演化的真正影响。我们分析了1000多个星系的性质，亮度超过$M_{^{0.1}r}$ =-19.6的90个星系团（$1<r/r_{vir}<2$）的红移范围内的外围$0.05<z<0.10$。使用视线速度，我们选择了高，低速度子样本。理论预测表明，第一个子样本中的相当一部分应该是后溅星系，也就是说，已经在星系团中心附近轨道运行的物体。一个显着比例的高相对速度HV星系的样本似乎是由坠落的对象。我们的研究结果表明，在固定的恒星质量，晚型星系的低速LV样品系统的年龄较大，红色，并形成了较少的恒星在过去3个陀螺比星系的HV样品。这一结果与假设星团中心区域通过冲压压力剥离或扼杀等过程有效淬灭恒星形成的模型一致。在恒星质量固定的情况下，LV星系比HV星系具有更高的表面亮度和更小的尺寸。这些结果与围绕星系团中心区域的星系更有可能遭受潮汐效应的情况是一致的，产生质量损失以及物质向更紧凑的配置重新分配。最后，我们发现在LV样本中ET星系的比例较高，支持星系团的中心区域可能有助于向早期类型的形态类型的转变的想法。

英文摘要：

We explore the properties of galaxies on the outskirts of clusters and their dependence on recent dynamical history in order to understand the real impact that the cluster core has on the evolution of galaxies. We analyse the properties of more than 1000 galaxies brighter than $M_{^{0.1}r}$=-19.6 on the outskirts of 90 clusters ($1<r/r_{vir}<2$) in the redshift range $0.05<z<0.10$. Using the line of sight velocity, we selected high and low velocity subsamples. Theoretical predictions indicate that a significant fraction of the first subsample should be backsplash galaxies, that is, objects that have already orbited near the cluster centre. A significant proportion of the sample of high relative velocity HV galaxies seems to be composed of infalling objects. Our results suggest that, at fixed stellar mass, late type galaxies in the low velocity LV sample are systematically older, redder and have formed fewer stars during the last 3 Gyrs than galaxies in the HV sample. This result is consistent with models that assume that the central regions of clusters are effective in quenching the star formation by means of processes such as ram pressure stripping or strangulation. At fixed stellar mass, LV galaxies show some evidence of having higher surface brightness and smaller size than HV galaxies. These results are consistent with the scenario where galaxies that have orbited the central regions of clusters are more likely to suffer tidal effects, producing loss of mass as well as a redistribution of matter towards more compact configurations. Finally, we found a higher fraction of ET galaxies in the LV sample, supporting the idea that the central region of clusters of galaxies may contribute to the transformation of morphological types towards earlier types.

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