CLASH-VLT: Substructure in the galaxy cluster MACS J1206.2-0847 from kinematics of galaxy populations

被引：27

作者：

Girardi, M. ^{[1
,2
]}

Mercurio, A. ^{[3
]}

Balestra, I. ^{[2
]}

Nonino, M. ^{[2
]}

Biviano, A. ^{[2
]}

Grillo, C. ^{[4
]}

Rosati, P. ^{[5
]}

Annunziatella, M. ^{[1
,2
]}

Demarco, R. ^{[6
]}

Fritz, A. ^{[7
]}

Gobat, R. ^{[8
]}

Lemze, D. ^{[9
]}

Presotto, V. ^{[1
]}

Scodeggio, M. ^{[7
]}

Tozzi, P. ^{[10
]}

Caminha, G. Bartosch ^{[5
]}

Brescia, M. ^{[3
]}

Coe, D. ^{[11
]}

Kelson, D. ^{[12
]}

Koekemoer, A. ^{[11
]}

Lombardi, M. ^{[13
]}

Medezinski, E. ^{[9
]}

Postman, M. ^{[11
]}

Sartoris, B. ^{[1
,2
]}

Umetsu, K. ^{[14
]}

Zitrin, A. ^{[15
]}

Boschin, W. ^{[16
,17
,18
]}

Czoske, O. ^{[19
]}

De Lucia, G. ^{[2
]}

Kuchner, U. ^{[19
]}

Maier, C. ^{[19
]}

Meneghetti, M. ^{[20
,21
,22
]}

Monaco, P. ^{[1
,2
]}

Monna, A. ^{[23
]}

Munari, E. ^{[1
,2
]}

Seitz, S. ^{[23
,24
]}

Verdugo, M. ^{[19
]}

Ziegler, B. ^{[19
]}

机构：

[1] Univ Trieste, Dipartimento Fis, I-34143 Trieste, Italy

[2] INAF Osservatorio Astron Trieste, I-34133 Trieste, Italy

[3] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy

[4] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark

[5] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy

[6] Univ Concepcion, Dept Astron, Concepcion, Chile

[7] INAF IASF Milano, I-20133 Milan, Italy

[8] KIAS, Seoul 130722, South Korea

[9] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[10] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy

[11] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[12] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA

[13] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy

[14] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan

[15] CALTECH, Pasadena, CA 91125 USA

[16] Fdn Galileo Galilei INAF, Brena Baja 38712, La Palma, Spain

[17] Inst Astrofis Canarias, Tenerife 38205, Spain

[18] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain

[19] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria

[20] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy

[21] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy

[22] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[23] Univ Observ Munich, D-81679 Munich, Germany

[24] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany

来源：

ASTRONOMY & ASTROPHYSICS | 2015年 / 579卷

关键词：

galaxies: clusters: individual: MACS J1206.2-0847; galaxies: clusters: general; galaxies: kinematics and dynamics; galaxies: evolution; cosmology: observations; SCALE-INDEPENDENT METHOD; POST-STARBURST GALAXIES; STAR-FORMATION ACTIVITY; HUBBLE-SPACE-TELESCOPE; VELOCITY DISPERSIONS; MASSIVE CLUSTER; RICH CLUSTERS; ENVIRONMENTAL DEPENDENCE; INTERNAL DYNAMICS; MERGING CLUSTERS;

D O I：

10.1051/0004-6361/201425599

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. In the effort to understand the link between the structure of galaxy clusters and their galaxy populations, we focus on MACS J1206.2-0847 at z similar to 0.44 and probe its substructure in the projected phase space through the spectrophotometric properties of a large number of galaxies from the CLASH-VLT survey. Methods. Our analysis is mainly based on an extensive spectroscopic dataset of 445 member galaxies, mostly acquired with VIMOS at VLT as part of our ESO Large Programme, sampling the cluster out to a radius similar to 2R(200) (4 h(70)(-1) Mpc). We classify 412 galaxies as passive, with strong H delta absorption (red and blue galaxies), and with emission lines from weak to very strong. A number of tests for substructure detection are applied to analyze the galaxy distribution in the velocity space, in 2D space, and in 3D projected phase-space. Results. Studied in its entirety, the cluster appears as a large-scale relaxed system with a few secondary, minor overdensities in 2D distribution. We detect no velocity gradients or evidence of deviations in local mean velocities. The main feature is the WNW-ESE elongation. The analysis of galaxy populations per spectral class highlights a more complex scenario. The passive galaxies and red strong H delta galaxies trace the cluster center and the WNW-ESE elongated structure. The red strong H delta galaxies also mark a secondary, dense peak similar to 2 h(70)(-1) Mpc at ESE. The emission line galaxies cluster in several loose structures, mostly outside R-200. Two of these structures are also detected through our 3D analysis. The observational scenario agrees with MACS J1206.2-0847 having WNW-ESE as the direction of the main cluster accretion, traced by passive galaxies and red strong H delta galaxies. The red strong H delta galaxies, interpreted as poststarburst galaxies, date a likely important event 1-2 Gyr before the epoch of observation. The emission line galaxies trace a secondary, ongoing infall where groups are accreted along several directions.

引用

页数：19

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