Chandra Cluster Cosmology Project III: Cosmological Parameter Constraints

Publication: Research - peer-reviewJournal article – Annual report year: 2009

Standard

Chandra Cluster Cosmology Project III: Cosmological Parameter Constraints. / Vikhlinin, A.; Kravtsov, A. V.; Burenin, R. A.; Ebeling, H.; Forman, W. R.; Hornstrup, Allan; Jones, C.; Murray, S. S.; Nagai, D.; Quintana, H.; Voevodkin, A.

In: Astrophysical Journal, Vol. 692, No. 2, 2009, p. 1060-1074.

Publication: Research - peer-reviewJournal article – Annual report year: 2009

Harvard

Vikhlinin, A, Kravtsov, AV, Burenin, RA, Ebeling, H, Forman, WR, Hornstrup, A, Jones, C, Murray, SS, Nagai, D, Quintana, H & Voevodkin, A 2009, 'Chandra Cluster Cosmology Project III: Cosmological Parameter Constraints' Astrophysical Journal, vol 692, no. 2, pp. 1060-1074., 10.1088/0004-637X/692/2/1060

APA

Vikhlinin, A., Kravtsov, A. V., Burenin, R. A., Ebeling, H., Forman, W. R., Hornstrup, A., ... Voevodkin, A. (2009). Chandra Cluster Cosmology Project III: Cosmological Parameter Constraints. Astrophysical Journal, 692(2), 1060-1074. 10.1088/0004-637X/692/2/1060

CBE

Vikhlinin A, Kravtsov AV, Burenin RA, Ebeling H, Forman WR, Hornstrup A, Jones C, Murray SS, Nagai D, Quintana H, Voevodkin A. 2009. Chandra Cluster Cosmology Project III: Cosmological Parameter Constraints. Astrophysical Journal. 692(2):1060-1074. Available from: 10.1088/0004-637X/692/2/1060

MLA

Vancouver

Vikhlinin A, Kravtsov AV, Burenin RA, Ebeling H, Forman WR, Hornstrup A et al. Chandra Cluster Cosmology Project III: Cosmological Parameter Constraints. Astrophysical Journal. 2009;692(2):1060-1074. Available from: 10.1088/0004-637X/692/2/1060

Author

Vikhlinin, A.; Kravtsov, A. V.; Burenin, R. A.; Ebeling, H.; Forman, W. R.; Hornstrup, Allan; Jones, C.; Murray, S. S.; Nagai, D.; Quintana, H.; Voevodkin, A. / Chandra Cluster Cosmology Project III: Cosmological Parameter Constraints.

In: Astrophysical Journal, Vol. 692, No. 2, 2009, p. 1060-1074.

Publication: Research - peer-reviewJournal article – Annual report year: 2009

Bibtex

@article{8e92bab38c2d4067a57e5220a2b88ac6,
title = "Chandra Cluster Cosmology Project III: Cosmological Parameter Constraints",
keywords = "galaxies: clusters: general, dark matter, cosmology: observations, cosmological parameters, surveys",
publisher = "Institute of Physics Publishing, Inc",
author = "A. Vikhlinin and Kravtsov, {A. V.} and Burenin, {R. A.} and H. Ebeling and Forman, {W. R.} and Allan Hornstrup and C. Jones and Murray, {S. S.} and D. Nagai and H. Quintana and A. Voevodkin",
year = "2009",
doi = "10.1088/0004-637X/692/2/1060",
volume = "692",
number = "2",
pages = "1060--1074",
journal = "Astrophysical Journal",
issn = "0004-637X",

}

RIS

TY - JOUR

T1 - Chandra Cluster Cosmology Project III: Cosmological Parameter Constraints

A1 - Vikhlinin,A.

A1 - Kravtsov,A. V.

A1 - Burenin,R. A.

A1 - Ebeling,H.

A1 - Forman,W. R.

A1 - Hornstrup,Allan

A1 - Jones,C.

A1 - Murray,S. S.

A1 - Nagai,D.

A1 - Quintana,H.

A1 - Voevodkin,A.

AU - Vikhlinin,A.

AU - Kravtsov,A. V.

AU - Burenin,R. A.

AU - Ebeling,H.

AU - Forman,W. R.

AU - Hornstrup,Allan

AU - Jones,C.

AU - Murray,S. S.

AU - Nagai,D.

AU - Quintana,H.

AU - Voevodkin,A.

PB - Institute of Physics Publishing, Inc

PY - 2009

Y1 - 2009

N2 - Chandra observations of large samples of galaxy clusters detected in X-rays by ROSAT provide a new, robust determination of the cluster mass functions at low and high redshifts. Statistical and systematic errors are now sufficiently small, and the redshift leverage sufficiently large for the mass function evolution to be used as a useful growth of a structure-based dark energy probe. In this paper, we present cosmological parameter constraints obtained from Chandra observations of 37 clusters with langzrang = 0.55 derived from 400 deg2 ROSAT serendipitous survey and 49 brightest z ≈ 0.05 clusters detected in the All-Sky Survey. Evolution of the mass function between these redshifts requires ΩΛ > 0 with a ~5σ significance, and constrains the dark energy equation-of-state parameter to w 0 = –1.14 ± 0.21, assuming a constant w and a flat universe. Cluster information also significantly improves constraints when combined with other methods. Fitting our cluster data jointly with the latest supernovae, Wilkinson Microwave Anisotropy Probe, and baryonic acoustic oscillation measurements, we obtain w 0 = –0.991 ± 0.045 (stat) ±0.039 (sys), a factor of 1.5 reduction in statistical uncertainties, and nearly a factor of 2 improvement in systematics compared with constraints that can be obtained without clusters. The joint analysis of these four data sets puts a conservative upper limit on the masses of light neutrinos ∑m ν <0.33 eV at 95% CL. We also present updated measurements of ΩM h and σ8 from the low-redshift cluster mass function.

AB - Chandra observations of large samples of galaxy clusters detected in X-rays by ROSAT provide a new, robust determination of the cluster mass functions at low and high redshifts. Statistical and systematic errors are now sufficiently small, and the redshift leverage sufficiently large for the mass function evolution to be used as a useful growth of a structure-based dark energy probe. In this paper, we present cosmological parameter constraints obtained from Chandra observations of 37 clusters with langzrang = 0.55 derived from 400 deg2 ROSAT serendipitous survey and 49 brightest z ≈ 0.05 clusters detected in the All-Sky Survey. Evolution of the mass function between these redshifts requires ΩΛ > 0 with a ~5σ significance, and constrains the dark energy equation-of-state parameter to w 0 = –1.14 ± 0.21, assuming a constant w and a flat universe. Cluster information also significantly improves constraints when combined with other methods. Fitting our cluster data jointly with the latest supernovae, Wilkinson Microwave Anisotropy Probe, and baryonic acoustic oscillation measurements, we obtain w 0 = –0.991 ± 0.045 (stat) ±0.039 (sys), a factor of 1.5 reduction in statistical uncertainties, and nearly a factor of 2 improvement in systematics compared with constraints that can be obtained without clusters. The joint analysis of these four data sets puts a conservative upper limit on the masses of light neutrinos ∑m ν <0.33 eV at 95% CL. We also present updated measurements of ΩM h and σ8 from the low-redshift cluster mass function.

KW - galaxies: clusters: general

KW - dark matter

KW - cosmology: observations

KW - cosmological parameters

KW - surveys

UR - http://lanl.arxiv.org/PS_cache/arxiv/pdf/0812/0812.2720v1.pdf

U2 - 10.1088/0004-637X/692/2/1060

DO - 10.1088/0004-637X/692/2/1060

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

VL - 692

SP - 1060

EP - 1074

ER -