The GEEC2 spectroscopic survey of Galaxy groups at 0.8 < z < 1

被引：45
作者：
Balogh, Michael L. [1 ,2 ]
McGee, Sean L. [2 ]
Mok, Angus [1 ,3 ]
Wilman, David J. [4 ]
Finoguenov, Alexis [5 ]
Bower, Richard G. [6 ]
Mulchaey, John S. [7 ]
Parker, Laura C. [3 ]
Tanaka, Masayuki [8 ]
机构：
[1] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada
[2] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands
[3] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada
[4] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany
[5] Univ Helsinki, Dept Phys, FI-00014 Helsinki, Finland
[6] Univ Durham, Dept Phys, Durham DH1 3LE, England
[7] Observ Carnegie Inst, Pasadena, CA 91101 USA
[8] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan
来源：
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2014年 / 443卷 / 03期
基金：
加拿大自然科学与工程研究理事会;
关键词：
galaxies: evolution; galaxies: groups: general; DIGITAL SKY SURVEY; BRIGHTEST CLUSTER GALAXIES; STAR-FORMATION HISTORIES; DARK-MATTER HALOS; DEEP-FIELD-SOUTH; X-RAY GROUPS; STELLAR MASS; REDSHIFT SURVEY; COSMOS SURVEY; GROUP CATALOG;
D O I：
10.1093/mnras/stu1332
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We present the data release of the Gemini-South GMOS spectroscopy in the fields of 11 galaxy groups at 0.8 < z < 1, within the COSMOS field. This forms the basis of the Galaxy Environment Evolution Collaboration 2 (GEEC2) project to study galaxy evolution in haloes with M similar to 10(13)M circle dot across cosmic time. The final sample includes 162 spectroscopically confirmed members with R < 24.75, and is >50 per cent complete for galaxies within the virial radius, and with stellar mass M-star > 10(10.3) M circle dot. Including galaxies with photometric redshifts, we have an effective sample size of similar to 400 galaxies within the virial radii of these groups. We present group velocity dispersions, dynamical and stellar masses. Combining with the GCLASS sample of more massive clusters at the same redshift, we find the total stellar mass is strongly correlated with the dynamical mass, with log M-200 = 1.20(logM(star) - 12) + 14.07. This stellar fraction of similar to 1 per cent is lower than predicted by some halo occupation distribution models, though the weak dependence on halo mass is in good agreement. Most groups have an easily identifiable most massive galaxy (MMG) near the centre of the galaxy distribution, and we present the spectroscopic properties and surface brightness fits to these galaxies. The total stellar mass distribution in the groups, excluding the MMG, compares well with an NFW (Navarro Frenk & White) profile with concentration 4, for galaxies beyond similar to 0.2R(200). This is more concentrated than the number density distribution, demonstrating that there is some mass segregation.
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收藏
页码：2679 / 2694
页数：16
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