Is diffuse intracluster light a good tracer of the galaxy cluster matter distribution?

被引：32

作者：

Sampaio-Santos, H. ^{[1
,2
]}

Zhang, Y. ^{[3
]}

Ogando, R. L. C. ^{[1
,2
]}

Shin, T. ^{[4
]}

Golden-Marx, Jesse B. ^{[5
,6
]}

Yanny, B. ^{[3
]}

Herner, K. ^{[3
]}

Hilton, M. ^{[7
]}

Choi, A. ^{[8
]}

Gatti, M. ^{[9
]}

Gruen, D. ^{[10
,11
,12
]}

Hoyle, B. ^{[13
,14
]}

Rau, M. M. ^{[15
]}

De Vicente, J. ^{[16
]}

Zuntz, J. ^{[17
]}

Abbott, T. M. C. ^{[18
]}

Aguena, M. ^{[2
,19
]}

Allam, S. ^{[3
]}

Annis, J. ^{[3
]}

Avila, S. ^{[20
]}

Bertin, E. ^{[21
,22
]}

Brooks, D. ^{[23
]}

Burke, D. L. ^{[11
,12
]}

Kind, M. Carrasco ^{[24
,25
]}

Carretero, J. ^{[9
]}

Chang, C. ^{[26
,27
]}

Costanzi, M. ^{[28
,29
]}

da Costa, L. N. ^{[1
,2
]}

Diehl, H. T. ^{[3
]}

Doel, P. ^{[23
]}

Everett, S. ^{[30
]}

Evrard, A. E. ^{[6
,31
]}

Flaugher, B. ^{[3
]}

Fosalba, P. ^{[32
,33
]}

Frieman, J. ^{[3
,27
]}

Garcia-Bellido, J. ^{[20
]}

Gaztanaga, E. ^{[32
,33
]}

Gerdes, D. W. ^{[6
,31
]}

Gruendl, R. A. ^{[24
,25
]}

Gschwend, J. ^{[1
,2
]}

Gutierrez, G. ^{[3
]}

Hinton, S. R. ^{[34
]}

Hollowood, D. L. ^{[30
]}

Honscheid, K. ^{[8
,35
]}

James, D. J. ^{[36
]}

Jarvis, M. ^{[4
]}

Jeltema, T. ^{[30
]}

Kuehn, K. ^{[37
,38
]}

Kuropatkin, N. ^{[3
]}

Lahav, O. ^{[23
]}

机构：

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

[2] Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[3] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA

[4] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA

[5] Shanghai Jiao Tong Univ, Dept Astron, Shanghai 200240, Peoples R China

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

[7] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, Westville Campus,Private Bag X54001, ZA-4000 Durban, South Africa

[8] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA

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

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

[11] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA

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

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

[14] Ludwig Maximilians Univ Munchen, Fak Phys, Univ Sternwarte, Scheinerstr 1, D-81679 Munich, Germany

[15] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Dept Phys, Pittsburgh, PA 15312 USA

[16] Ctr Invest Energet Medioambientales & Tecnol CIEM, E-28040 Madrid, Spain

[17] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland

[18] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile

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

[20] Univ Autonoma Madrid, Inst Fis Teor UAM CSIC, Madrid 28049, Spain

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

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

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

[24] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA

[25] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA

[26] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA

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

[28] INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34143 Trieste, Italy

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

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

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

[32] Inst Estudis Espacials Catalunya IEEC, E-08034 Barcelona, Spain

[33] CSIC, Inst Space Sci ICE, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain

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

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

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

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

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

[39] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA

[40] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA

[41] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain

[42] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[43] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA

[44] Univ Fed Rio Grande do Sul, Inst Fis, Caixa Postal 15051, BR-91501970 Porto Alegre, RS, Brazil

[45] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England

[46] Oak Ridge Natl Lab, Comp Sci & Math Div, Oak Ridge, TN 37831 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2021年 / 501卷 / 01期

基金：

欧洲研究理事会; 英国科学技术设施理事会; 美国国家科学基金会;

关键词：

galaxies: clusters: general; galaxies: photometry; dark matter; DARK ENERGY SURVEY; ILLUSTRISTNG SIMULATIONS; STELLAR HALOES; OPTICAL LIGHT; MASS; EVOLUTION; CALIBRATION; LUMINOSITY;

D O I：

10.1093/mnras/staa3680

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We explore the relation between diffuse intracluster light (central galaxy included) and the galaxy cluster (baryonic and dark) matter distribution using a sample of 528 clusters at 0.2 <= z <= 0.35 found in the Dark Energy Survey (DES) Year 1 data. The surface brightness of the diffuse light shows an increasing dependence on cluster total mass at larger radius, and appears to be self-similar with a universal radial dependence after scaling by cluster radius. We also compare the diffuse light radial profiles to the cluster (baryonic and dark) matter distribution measured through weak lensing and find them to be comparable. The IllustrisTNG galaxy formation simulation, TNG300, offers further insight into the connection between diffuse stellar mass and cluster matter distributions - the simulation radial profile of the diffuse stellar component does not have a similar slope with the total cluster matter content, although that of the cluster satellite galaxies does. Regardless of the radial trends, the amount of diffuse stellar mass has a low-scatter scaling relation with cluster's total mass in the simulation, out-performing the total stellar mass of cluster satellite galaxies. We conclude that there is no consistent evidence yet on whether or not diffuse light is a faithful radial tracer of the cluster matter distribution. Nevertheless, both observational and simulation results reveal that diffuse light is an excellent indicator of the cluster's total mass.

引用

页码：1300 / 1315

页数：16

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