REDSHIFT EVOLUTION IN THE IRON ABUNDANCE OF THE INTRACLUSTER MEDIUM

被引：29

作者：

Anderson, Michael E. ^{[1
]}

Bregman, Joel N. ^{[1
]}

Butler, Suzanne C. ^{[1
,2
]}

Mullis, C. R. ^{[1
]}

机构：

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

[2] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

来源：

ASTROPHYSICAL JOURNAL | 2009年 / 698卷 / 01期

关键词：

galaxies: clusters: general; X-rays: galaxies: clusters; LUMINOSITY-TEMPERATURE RELATION; RAY SCALING RELATIONS; INTRA-CLUSTER MEDIUM; GALAXY CLUSTERS; XMM-NEWTON; HYDRODYNAMICAL SIMULATIONS; Z-GREATER-THAN-0.4; ENRICHMENT; ELEMENTS; HISTORY;

D O I：

10.1088/0004-637X/698/1/317

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Clusters of galaxies provide a closed box within which one can determine the chemical evolution of the gaseous baryons with cosmic time. We studied this metallicity evolution in the hot X-ray emitting baryons through an analysis of XMM-Newton observations of 29 galaxy clusters in the redshift range, 0.3 < z < 1.3. Taken alone, this data set does not show evidence for significant evolution. However, when we also include a comparable sample of 115 clusters observed with Chandra and a lower redshift sample of 70 clusters observed with XMM at z < 0.3, there is definitive evidence for a decrease in the metallicity. This decrease is approximately a factor of two from z = 0 to z approximate to 1, over which we find a least-squares best-fit line Z(z)/Z(circle dot) = (0.46 +/- 0.05) - (0.38 +/- 0.03) z. The greatest uncertainty in the evolution comes from poorly constrained metallicities in the highest redshift bin.

引用

页码：317 / 323

页数：7

共 36 条

[21] Gas, iron, and gravitational mass in galaxy clusters:: The general lack of cluster evolution at z < 1.0 [J].

Matsumoto, H ;

Tsuru, TG ;

Fukazawa, Y ;

Hattori, M ;

Davis, DS .

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, 2000, 52 (01) :153-160

[22]

MATTEUCCI F, 1988, ASTRON ASTROPHYS, V202, P21

[23] Images, structural properties, and metal abundances of galaxy clusters observed with Chandra ACIS-I at 0.1 < z < 1.3 [J].

Maughan, B. J. ;

Jones, C. ;

Forman, W. ;

Van Speybroeck, L. .

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 2008, 174 (01) :117-135

[24] The evolution of the cluster X-ray scaling relations in the Wide Angle ROSAT Pointed Survey sample at 0.6<z<1.0 [J].

Maughan, BJ ;

Jones, LR ;

Ebeling, H ;

Scharf, C .

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2006, 365 (02) :509-529

[25]

MCCAMMON D, 1990, ANNU REV ASTRON ASTR, V28, P657

[26] Lack of evolution in the iron abundance in clusters of galaxies and implications for the global star formation rate at high redshift [J].

Mushotzky, RF ;

Loewenstein, M .

ASTROPHYSICAL JOURNAL, 1997, 481 (02) :L63-L66

[27] The metal enrichment of the intracluster medium in hierarchical galaxy formation models [J].

Nagashima, M ;

Lacey, CG ;

Baugh, CM ;

Frenk, CS ;

Cole, S .

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2005, 358 (04) :1247-1266

[28] The evolution of the galaxy cluster luminosity-temperature relation [J].

Novicki, MC ;

Sornig, M ;

Henry, JP .

ASTRONOMICAL JOURNAL, 2002, 124 (05) :2413-2424

[29] SNe heating and the chemical evolution of the intra-cluster medium [J].

Pipino, A ;

Matteucci, F ;

Borgani, S ;

Biviano, A .

NEW ASTRONOMY, 2002, 7 (05) :227-247

[30] Structure and scaling of the entropy in nearby galaxy clusters [J].

Pratt, GW ;

Arnaud, M ;

Pointecouteau, E .

ASTRONOMY & ASTROPHYSICS, 2006, 446 (02) :429-438

← 1 2 3 4 →