Galaxy cluster correlation function to z∼1.5 in the IRAC shallow cluster survey

被引：38

作者：

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

Gonzalez, A. H. ^{[3
]}

Moustakas, L. A. ^{[1
]}

Eisenhardt, P. R. ^{[1
]}

Stanford, S. A. ^{[4
,5
]}

Stern, D.

Brown, M. J. I. ^{[6
]}

机构：

[1] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA

[2] Natl Opt Astron Observ, Tucson, AZ 85726 USA

[3] Univ Florida, Dept Astron, Gainesville, FL 32611 USA

[4] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA

[5] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA

[6] Monash Univ, Sch Phys, Clayton, Vic 3168, Australia

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2007年 / 671卷 / 02期

关键词：

cosmology : observations; galaxies : clusters : general; large-scale structure of universe;

D O I：

10.1086/525558

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the galaxy cluster autocorrelation function of 277 galaxy cluster candidates with in 0.25 <= z <= 1.5 a 7 deg(2) area of the IRAC Shallow Cluster Survey. We find strong clustering throughout our galaxy cluster sample, as expected for these massive structures. Specifically, at < z >=0.5 we find a correlation length of r(0)=17.40(-3.10)(+3.98) h(-1)Mpc, in excellent agreement with the Las Campanas Distant Cluster Survey, the only other nonlocal measurement. At higher redshift,, we find that strong clustering persists, with a correlation AzS p 1 length of r(0)=19.14(-4.56)(+5.65) h(-1) Mpc. A comparison with high-resolution cosmological simulations indicates these are clusters with halo masses of similar to 10(14) M-circle dot, a result supported by estimates of dynamical mass for a subset of the sample. In a stable clustering picture, these clusters will evolve into massive (10(15) M-circle dot) clusters by the present day.

引用

页码：L93 / L96

页数：4

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