Size-mass relation of the brightest cluster galaxies at z ∼ 1

被引:0
|
作者
Yang, Lilan [1 ,2 ]
Silverman, John [1 ,3 ,4 ]
Oguri, Masamune [5 ,6 ]
Ding, Xuheng [1 ,4 ]
Toba, Yoshiki [7 ,8 ,9 ]
Huang, Song [10 ,11 ]
Kawinwanichakij, Lalitwadee [12 ]
机构
[1] Univ Tokyo, Kavli Inst Phys & Math Universe Kavli IPMU, Tokyo Inst Adv Study, WPI,UTIAS, Chiba 2778583, Japan
[2] Rochester Inst Technol, Sch Phys & Astron, Lab Multiwavelength Astrophys, 84 Lomb Mem Dr, Rochester, NY 14623 USA
[3] Univ Tokyo, Sch Sci, Dept Astron, 7-3-1 Hongo,Bunkyo Ku, Tokyo 1130033, Japan
[4] Univ Tokyo, Ctr Data Driven Discovery, Kavli IPMU WPI, UTIAS, Kashiwa, Chiba 2778583, Japan
[5] Chiba Univ, Ctr Frontier Sci, Chiba 2638522, Japan
[6] Chiba Univ, Grad Sch Sci, Dept Phys, Chiba 2638522, Japan
[7] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan
[8] Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,AS NTU 1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan
[9] Ehime Univ, Res Ctr Space & Cosm Evolut, 2-5 Bunkyo Cho, Matsuyama, Ehime 7908577, Japan
[10] Tsinghua Univ, Dept Astron, Beijing 100084, Peoples R China
[11] Tsinghua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China
[12] Swinburne Univ Technol, Ctr Astrophys & Supercomp, POB 218, Hawthorn, Vic 3122, Australia
基金
日本学术振兴会;
关键词
galaxies: evolution; galaxies: fundamental parameters; galaxies: structure; SUBARU STRATEGIC PROGRAM; STELLAR MASS; STRUCTURAL-PROPERTIES; LUMINOSITY FUNCTION; QUIESCENT GALAXIES; EVOLUTION; GROWTH; DEPENDENCE; SEQUENCE; HALOES;
D O I
10.1093/mnras/stae1374
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present the size-mass relation of the brightest cluster galaxies (BCGs) at 0.1 < z < 1.4 using the imaging data obtained by the Hyper Suprime-Cam Subaru Strategic Program. Our sample consists of 471 photometrically selected BCGs with stellar mass logM(*)/M-circle dot = 11-12. We measure the size of the BCGs using i-band imaging and model fits based on a single S & eacute;rsic light profile. Stellar masses are determined through spectral energy distribution fitting using S & eacute;rsic-modelled photometry data across five optical bands (grizy). The size-mass scaling relation of BCGs is $r_\mathrm{ e}\propto M_*<^>{0.73-1.00}$ at z < 1, with a slope that does not evolve significantly. The slope of the size-mass relation for BCGs is steeper than other non-BCG galaxies, which implies that BCGs are a special galaxy population. The size of BCGs at a given stellar mass evolves rapidly as proportional to (1 + z)(-1.58 +/- 0.13) and increases with redshift by a factor of 2.5 from z similar to 1.2 to z similar to 0.2. The rapid size growth is in agreement with semi-analytical model results, indicating that the BCG growth is dominated by frequent minor mergers. Furthermore, we explore the size-mass relationship of BCGs with respect to the halo mass of the cluster and find there is no significant correlation, which might imply that a dependence on the environment predominantly affects the outer envelope of the BCGs.
引用
收藏
页码:4006 / 4016
页数:11
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