The evolution of active galactic nuclei in clusters of galaxies from the Dark Energy Survey

被引：26

作者：

Bufanda, E. ^{[1
]}

Hollowood, D. ^{[1
]}

Jeltema, T. E. ^{[1
]}

Rykoff, E. S. ^{[2
,3
]}

Rozo, E. ^{[4
]}

Martini, P. ^{[5
,6
]}

Abbott, T. M. C. ^{[7
]}

Abdalla, F. B. ^{[8
,9
]}

Allam, S. ^{[10
]}

Banerji, M. ^{[11
,12
]}

Benoit-Levy, A. ^{[13
,14
]}

Bertin, E. ^{[13
,14
]}

Brooks, D. ^{[8
]}

Carnero Rosell, A. ^{[15
,16
]}

Kind, M. Carrasco ^{[17
,18
]}

Carretero, J. ^{[19
,20
]}

Cunha, C. E. ^{[2
]}

da Costa, L. N. ^{[15
,16
]}

Desai, S. ^{[21
,22
]}

Diehl, H. T. ^{[10
]}

Dietrich, J. P. ^{[21
,22
]}

Evrard, A. E. ^{[23
,24
]}

Fausti Neto, A. ^{[15
]}

Flaugher, B. ^{[10
]}

Frieman, J. ^{[10
,25
]}

Gerdes, D. W. ^{[24
]}

Goldstein, D. A. ^{[26
,27
]}

Gruen, D. ^{[2
,3
]}

Gruendl, R. A. ^{[17
,18
]}

Gutierrez, G. ^{[10
]}

Honscheid, K. ^{[5
,28
]}

James, D. J. ^{[7
]}

Kuehn, K. ^{[29
]}

Kuropatkin, N. ^{[10
]}

Lima, M. ^{[15
,30
]}

Maia, M. A. G. ^{[15
,16
]}

Marshall, J. L. ^{[31
,32
]}

Melchior, P. ^{[33
]}

Miquel, R. ^{[34
]}

Mohr, J. J. ^{[21
,22
,35
]}

Ogando, R. ^{[15
,16
]}

Plazas, A. A. ^{[36
]}

Romer, A. K. ^{[37
]}

Rooney, P. ^{[37
]}

Sanchez, E. ^{[38
]}

Santiago, B. ^{[15
,39
]}

Scarpine, V. ^{[10
]}

Sevilla-Noarbe, I. ^{[38
]}

Smith, R. C. ^{[7
]}

Soares-Santos, M. ^{[10
]}

机构：

[1] Univ Calif Santa Cruz, Dept Phys & Santa Cruz, Inst Particle Phys, Santa Cruz, CA 95064 USA

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

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

[4] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA

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

[6] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA

[7] Natl Optic Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile

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

[9] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa

[10] Fermilab Natl Accelerator Lab, PO 500, Batavia, IL 60510 USA

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

[12] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England

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

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

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

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

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

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

[19] IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans,S-N, E-08193 Barcelona, Spain

[20] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Barcelona, Spain

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

[22] Excellence Cluster Univ, Boltzmannstr 2, D-85748 Garching, Germany

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

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

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

[26] Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA

[27] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA

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

[29] Australian Astron Observ, N Ryde, NSW 2113, Australia

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

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

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

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

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

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

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

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

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

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

[40] Univ Estadual Paulista, ICTP South Amer Inst Fundamental Res, Inst Fis Teor, Sao Paulo, Brazil

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

[42] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2017年 / 465卷 / 03期

基金：

美国国家科学基金会; 欧洲研究理事会;

关键词：

galaxies: active; X-rays: galaxies; X-rays: galaxies: clusters; SUPERMASSIVE BLACK-HOLES; STAR-FORMATION ACTIVITY; AGN HOST GALAXIES; SIMILAR-TO; X-RAY; VELOCITY DISPERSION; MULTIWAVELENGTH SURVEY; REDSHIFT CLUSTERS; FUNDAMENTAL PLANE; INACTIVE GALAXIES;

D O I：

10.1093/mnras/stw2824

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The correlation between active galactic nuclei (AGNs) and environment provides important clues to AGN fuelling and the relationship of black hole growth to galaxy evolution. In this paper, we analyse the fraction of galaxies in clusters hosting AGN as a function of redshift and cluster richness for X-ray-detected AGN associated with clusters of galaxies in Dark Energy Survey (DES) Science Verification data. The present sample includes 33 AGNs with LX > 1043 erg s(-1) in non-central, host galaxies with luminosity greater than 0.5L(*) from a total sample of 432 clusters in the redshift range of 0.1< z <0.95. Analysis of the present sample reveals that the AGN fraction in red-sequence cluster members has a strong positive correlation with redshift such that the AGN fraction increases by a factor of similar to 8 from low to high redshift, and the fraction of cluster galaxies hosting AGN at high redshifts is greater than the low-redshift fraction at 3.6 sigma. In particular, the AGN fraction increases steeply at the highest redshifts in our sample at z > 0.7. This result is in good agreement with previous work and parallels the increase in star formation in cluster galaxies over the same redshift range. However, the AGN fraction in clusters is observed to have no significant correlation with cluster mass. Future analyses with DES Year 1 through Year 3 data will be able to clarify whether AGN activity is correlated to cluster mass and will tightly constrain the relationship between cluster AGN populations and redshift.

引用

页码：2531 / 2539

页数：9

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