A joint SZ-X-ray-optical analysis of the dynamical state of 288 massive galaxy clusters

被引：29

作者：

Zenteno, A. ^{[1
]}

Hernandez-Lang, D. ^{[1
,2
,3
]}

Klein, M. ^{[2
,4
]}

Cervantes, C. Vergara ^{[5
]}

Hollowood, D. L. ^{[6
]}

Bhargava, S. ^{[5
]}

Palmese, A. ^{[7
,8
,9
]}

Strazzullo, V. ^{[10
]}

Romer, A. K. ^{[5
]}

Mohr, J. J. ^{[2
,4
]}

Jeltema, T. ^{[6
]}

Saro, A. ^{[11
,12
,13
]}

Lidman, C. ^{[18
]}

Gruen, D. ^{[14
,15
]}

Ojeda, V. ^{[16
]}

Katzenberger, A. ^{[17
]}

Aguena, M. ^{[19
,20
]}

Allam, S. ^{[7
,8
]}

Avila, S. ^{[21
]}

Bayliss, M. ^{[22
]}

Bertin, E. ^{[23
,24
]}

Brooks, D. ^{[25
]}

Buckley-Geer, E. ^{[7
,8
]}

Burke, D. L. ^{[14
,15
]}

Capasso, R. ^{[26
]}

Carnero Rosell, A. ^{[27
]}

Carrasco Kind, M. ^{[28
,29
]}

Carretero, J. ^{[30
]}

Castander, F. J. ^{[31
,32
]}

Costanzi, M. ^{[33
]}

da Costa, L. N. ^{[34
]}

De Vicente, J. ^{[27
]}

Desai, S. ^{[35
]}

Diehl, H. T. ^{[7
,8
]}

Doel, P. ^{[25
]}

Eifler, T. F. ^{[36
,37
]}

Evrard, A. E. ^{[38
,39
]}

Flaugher, B. ^{[7
,8
]}

Floyd, B. ^{[40
]}

Fosalba, P. ^{[31
,32
]}

Frieman, J. ^{[7
,8
,9
]}

Garcia-Bellido, J. ^{[21
]}

Gerdes, D. W. ^{[38
,39
]}

Gonzalez, J. R. ^{[41
]}

Gruendl, R. A. ^{[28
,29
]}

Gschwend, J. ^{[20
,34
]}

Gutierrez, G. ^{[8
]}

Hartley, W. G. ^{[42
,43
,44
]}

Hinton, S. R. ^{[45
]}

Honscheid, K. ^{[46
,47
]}

机构：

[1] NSFs Natl Opt Infrared Astron Res Lab, Cerro Tololo Inter Amer Observ, Casilla 603, La Serena, Chile

[2] Ludwig Maximilians Univ Munchen, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany

[3] NSFs Natl Opt Infrared Astron Re search Lab, Gemini Observ, Casilla 603, La Serena, Chile

[4] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany

[5] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England

[6] Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA

[7] Fermilab Natl Accelerator Lab, Box 500, Batavia, IL 60510 USA

[8] Fermilab Natl Accelerator Lab, Box 500, Batavia, IL 60510 USA

[9] Univ Chicago, Kavli Inst Cosmol Phys, Chicago 60637, IL USA

[10] Univ Trieste, Dept Phys, Astron Unit, Via Tiepolo 11, I-34131 Trieste, Italy

[11] IFPU Inst Fundamental Phys Universe, Via Beirut 2, I-34014 Trieste, Italy

[12] 1INAF Osservatorio Astron Trieste, Via G B Tiepolo 11, I-34143 Trieste, Italy

[13] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA

[14] Stanford Univ, Kavli Inst Particle Astrophys Cosmol, Box 2450, Stanford, CA 94305 USA

[15] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA

[16] Univ Serena, Dept Fis Astron, Ave Juan Cisternas 1200, La Serena 1720236, Chile

[17] Ludwig Maximilians Univ Munchen, Dept Geog, Luisenstr 37, D-80333 Munich, Germany

[18] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2601, Australia

[19] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 S ao Paulo, SP, Brazil

[20] Lab Interinstituc & Astron LIneA, Rua Gal Jos Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[21] Univ Autonoma Madrid, Inst Fis Teo, UAM CSIC, E-28049 Madrid, Spain

[22] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA

[23] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France

[24] UPMC Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France

[25] UCL, Dept Phys Astron, Gower St, London WC1E 6BT, England

[26] Stockholm Univ, baNova Univ Ctr, Dept Phys, Oskar Klein Ctr, Stockholm, Sweden

[27] CIEMAT, Madrid 28040, Spain

[28] Univ Illinois UrbanaChampaign, Dept Astron, 1002 Green St, Urbana, IL 61801 USA

[29] Natl Ctr Supercomputing Applicat, 1205 West Clark St, Urbana, IL 61801 USA

[30] Barcelona Inst Sci & Technol, Inst Fis Altes Energies IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain

[31] Inst dEstudis Espacials Catalunya IEEC, E-08034 Barcelona, Spain

[32] CSIC, Inst Space Sci ICE, Campus UAB, E-08193 Barcelona, Spain

[33] Inst Fundamental Phys Universe, Via Beirut 2, I-34014 Trieste, Italy

[34] Observ Nacl, Rua Gal Jos Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[35] IIT Hyderabad, Dept Phys, Kandi 502285, Telangana, India

[36] Univ Arizona, Dept Astron, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA

[37] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA

[38] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[39] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA

[40] Univ Missouri, Dept Phys & Astron, 5110 Rockhill Rd, Kansas City, MO 64110 USA

[41] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[42] Univ Geneva, Dept Phys Ther, 24 Quai Ernest Ansermet, CH-1211 Geneva, Switzerland

[43] Univ Geneva, Ctr Astroparticle Phys, 24 Quai Ernest Ansermet, CH-1211 Geneva, Switzerland

[44] Swiss Fed Inst Technol, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland

[45] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia

[46] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA

[47] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA

[48] Ctr Astrophys Harvard Smithsonian, 60 Garden St, Cambridge, MA 02138 USA

[49] Macquarie Univ, Australian Astron Opt, N Ryde, NSW 2113, Australia

[50] Lowell Observ, 1400 Mars Hill Rd, Flagstaff, AZ 86001 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2020年 / 495卷 / 01期

基金：

美国国家科学基金会; 英国科学技术设施理事会; 澳大利亚研究理事会; 欧洲研究理事会;

关键词：

galaxies: evolution; galaxies: luminosity function; mass function; galaxies: clusters: general; K-BAND PROPERTIES; DARK-MATTER; LUMINOSITY FUNCTIONS; SUNYAEV-ZELDOVICH; STELLAR MASS; MS; 1054-03; MERGERS; OCCUPATION; EVOLUTION; MACS;

D O I：

10.1093/mnras/staa1157

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We use imaging from the first three years of the Dark Energy Survey to characterize the dynamical state of 288 galaxy clusters at 0.1 less than or similar to z less than or similar to 0.9 detected in the South Pole Telescope (SPT) Sunyaev-Zeldovich (SZ) effect survey (SPT-SZ). We examine spatial offsets between the position of the brightest cluster galaxy (BCG) and the centre of the gas distribution as traced by the SPT-SZ centroid and by the X-ray centroid/peak position from Chandra and XMM data. We show that the radial distribution of offsets provides no evidence that SPT SZ-selected cluster samples include a higher fraction of mergers than X-ray-selected cluster samples. We use the offsets to classify the dynamical state of the clusters, selecting the 43 most disturbed clusters, with half of those at z greater than or similar to 0.5, a region seldom explored previously. We find that Schechter function fits to the galaxy population in disturbed clusters and relaxed clusters differ at z > 0.55 but not at lower redshifts. Disturbed clusters at z > 0.55 have steeper faint-end slopes and brighter characteristic magnitudes. Within the same redshift range, we find that the BCGs in relaxed clusters tend to be brighter than the BCGs in disturbed samples, while in agreement in the lower redshift bin. Possible explanations includes a higher merger rate, and a more efficient dynamical friction at high redshift. The red-sequence population is less affected by the cluster dynamical state than the general galaxy population.

引用

页码：705 / 725

页数：21

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