Tully-Fisher analysis of the multiple cluster system Abell 901/902
Tully-Fisher analysis of the multiple cluster system Abell 901/902
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DOI：
10.1051/0004-6361/201321561
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发表时间：
2013-04
影响因子：
6.5
通讯作者：
Benjamin Bosch;A. Bohm;C. Wolf;A. Arag'on-Salamanca;B. Ziegler;M. Barden;M. Gray;M. Balogh;K. Meisenheimer;S. Schindler
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作者：
Benjamin Bosch;A. Bohm;C. Wolf;A. Arag'on-Salamanca;B. Ziegler;M. Barden;M. Gray;M. Balogh;K. Meisenheimer;S. Schindler
我们从位于 $z\sim 0.165$ 的 Abell 901/902 区域中 182 个盘状星系（96 个在星团中，86 个在场中）的光学发射线得出旋转曲线。我们重点分析 B 波段和恒星质量 Tully-Fisher 关系。我们研究了正常螺旋星系和“尘红色”星系之间可能的环境依赖性和差异，即由于恒星形成率相对较低而具有红色的盘状星系。我们发现星团星系和场星系的最佳拟合 TF 斜率之间没有显着差异。在固定斜率下，具有高质量旋转曲线的现场群体（57 个对象）比簇群体（55 个对象）亮 $\Delta M_{B}=-0\fm42\pm0\fm15$。我们证明这种细微的差异至少部分是环境影响。对于靠近核心区域的星系，星团 TFR 的散射会增加，这也表明了环境影响。有趣的是，在给定的旋转速度（即总质量）下，尘埃红色星系朝着核心变得越来越暗。这表明这些星系中的恒星形成正处于淬灭过程中。对于较小的星团中心半径，在固定旋转速度下，正常螺旋星系的光度稍高。这些星系可能富含气体（与尘土飞扬的红色星系相比），冲压压力剥离的开始增加了它们的恒星形成率。 TF 分析的结果与我们之前的发现一致并补充。尘红色星系可能是坠落场螺旋星系转变为星团 S0 的中间阶段，这可能解释了众所周知的星系团中 S0 分数随宇宙时间增加的现象。
We derive rotation curves from optical emission lines of 182 disk galaxies (96 in the cluster and 86 in the field) in the region of Abell 901/902 located at $z\sim 0.165$. We focus on the analysis of B-band and stellar-mass Tully-Fisher relations. We examine possible environmental dependencies and differences between normal spirals and "dusty red" galaxies, i.e. disk galaxies that have red colors due to relatively low star formation rates. We find no significant differences between the best-fit TF slope of cluster and field galaxies. At fixed slope, the field population with high-quality rotation curves (57 objects) is brighter by $\Delta M_{B}=-0\fm42\pm0\fm15$ than the cluster population (55 objects). We show that this slight difference is at least in part an environmental effect. The scatter of the cluster TFR increases for galaxies closer to the core region, also indicating an environmental effect. Interestingly, dusty red galaxies become fainter towards the core at given rotation velocity (i.e. total mass). This indicates that the star formation in these galaxies is in the process of being quenched. The luminosities of normal spiral galaxies are slightly higher at fixed rotation velocity for smaller cluster-centric radii. Probably these galaxies are gas-rich (compared to the dusty red population) and the onset of ram-pressure stripping increases their star-formation rates. The results from the TF analysis are consistent with and complement our previous findings. Dusty red galaxies might be an intermediate stage in the transformation of infalling field spiral galaxies into cluster S0s, and this might explain the well-known increase of the S0 fraction in galaxy clusters with cosmic time.