Photometric redshifts as a tool for studying the Coma cluster galaxy populations

被引:17
作者
Adami, C. [1 ,2 ]
Ilbert, O. [1 ,2 ,3 ]
Pello, R. [4 ]
Cuillandre, J. C. [5 ]
Durret, F. [6 ]
Mazure, A. [1 ,2 ]
Picat, J. P. [4 ]
Ulmer, M. P. [1 ,2 ,7 ]
机构
[1] Univ Aix Marseille, OAMP, LAM, F-13388 Marseille 13, France
[2] Univ Aix Marseille, CNRS, F-13388 Marseille 13, France
[3] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA
[4] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France
[5] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA
[6] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France
[7] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA
关键词
galaxies: clusters: individual: Coma; galaxies: luminosity function; mass function;
D O I
10.1051/0004-6361:200809845
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Aims. We apply photometric redshift techniques to an investigation of the Coma cluster galaxy luminosity function (GLF) at faint magnitudes, in particular in the u* band where basically no studies are presently available at these magnitudes. Methods. Cluster members were selected based on probability distribution function from photometric redshift calculations applied to deep u*, B, V, R, I images covering a region of almost 1 deg(2) (completeness limit R similar to 24). In the area covered only by the u* image, the GLF was also derived after a statistical background subtraction. Results. Global and local GLFs in the B, V, R, and I bands obtained with photometric redshift selection are consistent with our previous results based on a statistical background subtraction. The GLF in the u* band shows an increase in the faint end slope towards the outer regions of the cluster. The analysis of the multicolor type spatial distribution reveals that late type galaxies are distributed in clumps in the cluster outskirts, where X-ray substructures are also detected and where the GLF in the u* band is steeper. Conclusions. We can reproduce the GLFs computed with classical statistical subtraction methods by applying a photometric redshift technique. The u* GLF slope is steeper in the cluster outskirts, varying from alpha similar to -1 in the cluster center to alpha similar to -2 in the cluster periphery. The concentrations of faint late type galaxies in the cluster outskirts could explain these very steep slopes, assuming a short burst of star formation in these galaxies when entering the cluster.
引用
收藏
页码:681 / 692
页数:12
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