GALAXY AND MASS ASSEMBLY (GAMA): WITNESSING THE ASSEMBLY OF THE CLUSTER ABELL 1882

被引：13

作者：

Owers, M. S. ^{[1
]}

Baldry, I. K. ^{[2
]}

Bauer, A. E. ^{[1
]}

Bland-Hawthorn, J. ^{[3
]}

Brown, M. J. I. ^{[4
]}

Cluver, M. E. ^{[1
]}

Colless, M. ^{[5
]}

Driver, S. P. ^{[6
,7
]}

Edge, A. C. ^{[8
]}

Hopkins, A. M. ^{[1
]}

van Kampen, E. ^{[9
]}

Lara-Lopez, M. A. ^{[1
]}

Liske, J. ^{[10
]}

Loveday, J. ^{[10
]}

Pimbblet, K. A. ^{[3
]}

Ponman, T. ^{[11
]}

Robotham, A. S. G. ^{[5
,6
]}

机构：

[1] Australian Astron Observ, N Ryde, NSW 1670, Australia

[2] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5UX, Merseyside, England

[3] Univ Sydney, Sch Phys A28, Sydney Inst Astron, Sydney, NSW 2006, Australia

[4] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia

[5] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia

[6] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland

[7] Univ Western Australia, ICRAR, Crawley, WA 6009, Australia

[8] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England

[9] European So Observ, D-85748 Garching, Germany

[10] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England

[11] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England

来源：

ASTROPHYSICAL JOURNAL | 2013年 / 772卷 / 02期

基金：

澳大利亚研究理事会;

关键词：

galaxies: clusters: individual (ABELL 1882); surveys; X-rays: galaxies: clusters; XMM-NEWTON OBSERVATIONS; COLD-FRONT CLUSTER; DIGITAL SKY SURVEY; X-RAY; STAR-FORMATION; MERGING CLUSTERS; RADIO HALO; SHAPLEY CONCENTRATION; CHANDRA OBSERVATION; INTERNAL DYNAMICS;

D O I：

10.1088/0004-637X/772/2/104

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a combined optical and X-ray analysis of the rich cluster ABELL 1882 (A1882) with the aim of identifying merging substructure and understanding the recent assembly history of this system. Our optical data consist of spectra drawn from the Galaxy and Mass Assembly survey, which lends itself to this kind of detailed study thanks to its depth and high spectroscopic completeness. We use 283 spectroscopically confirmed cluster members to detect and characterize substructure. We complement the optical data with X-ray data taken with both Chandra and XMM. Our analysis reveals that A1882 harbors two main components, A1882A and A1882B, which have a projected separation of similar to 2 Mpc and a line of sight velocity difference of v(los) similar to -428(-139)(+187) km s(-1). The primary system, A1882A, has velocity dispersion sigma(v) = 500(-26)(+23) km s(-1) and Chandra (XMM) temperature kT = 3.57 +/- 0.17 keV (3.31(-0.27)(+0.28) keV) while the secondary, A1882B, has sigma(v) = 457(-101)(+108) km s(-1) and Chandra (XMM) temperature kT = 2.39 +/- 0.28 keV (2.12 +/- 0.20 keV). The optical and X-ray estimates for the masses of the two systems are consistent within the uncertainties and indicate that there is twice as much mass in A1882A (M-500 = 1.5-1.9 x 10(14) M-circle dot) when compared with A1882B (M-500 = 0.8-1.0 x 10(14) M-circle dot). We interpret the A1882A/A1882B system as being observed prior to a core passage. Supporting this interpretation is the large projected separation of A1882A and A1882B and the dearth of evidence for a recent (<2 Gyr) major interaction in the X-ray data. Two-body analyses indicate that A1882A and A1882B form a bound system with bound incoming solutions strongly favored. We compute blue fractions of f(b) = 0.28 +/- 0.09 and 0.18 +/- 0.07 for the spectroscopically confirmed member galaxies within r(500) of the centers of A1882A and A1882B, respectively. These blue fractions do not differ significantly from the blue fraction measured from an ensemble of 20 clusters with similar mass and redshift.

引用

页数：18

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