Campanelli, Leonardo and Fogli, Gianluigi and Kahniashvili, Tina and Marone, Antonio and Ratra, Bharat (2012) Galaxy cluster number count data constraints on cosmological parameters. The European Physical Journal C, 72.

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Abstract
We use data on massive galaxy clusters ( M cluster>8×1014 h 1 M ⊙ within a comoving radius of R cluster=1.5 h 1 Mpc) in the redshift range 0.05≲ z≲0.83 to place constraints, simultaneously, on the nonrelativistic matter density parameter Ω m , on the amplitude of mass fluctuations σ 8, on the index n of the powerlaw spectrum of the density perturbations, and on the Hubble constant H 0, as well as on the equationofstate parameters ( w 0, w a ) of a smooth dark energy component. For the first time, we properly take into account the dependence on redshift and cosmology of the quantities related to cluster physics: the critical density contrast, the growth factor, the mass conversion factor, the virial overdensity, the virial radius and, most importantly, the cluster number count derived from the observational temperature data. We show that, contrary to previous analyses, cluster data alone prefer low values of the amplitude of mass fluctuations, σ 8≤0.69 (1 σ C.L.), and large amounts of nonrelativistic matter, Ω m ≥0.38 (1 σ C.L.), in slight tension with the ΛCDM concordance cosmological model, though the results are compatible with ΛCDM at 2 σ. In addition, we derive a σ 8 normalization relation, σ8 \varOmegam^{1/3} = 0.49 ± 0.06 (2 σ C.L.). Combining cluster data with σ 8independent baryon acoustic oscillation observations, cosmic microwave background data, Hubble constant measurements, Hubble parameter determination from passively evolving red galaxies, and magnituderedshift data of type Ia supernovae, we find \varOmegam = 0.28^{+0.03}_{0.02} and σ8 = 0.73^{+0.03}_{0.03}, the former in agreement and the latter being slightly lower than the corresponding values in the concordance cosmological model. We also find H0 = 69.1^{+1.3}_{1.5} mbox {km}/mbox {s}/mbox {Mpc}, the fit to the data being almost independent on n in the adopted range [0.90,1.05]. Concerning the dark energy equationofstate parameters, we show that the present data on massive clusters weakly constrain ( w 0, w a ) around the values corresponding to a cosmological constant, i.e. ( w 0, w a )=(1,0). The global analysis gives w0 = 1.14^{+0.14}_{0.16} and wa = 0.85^{+0.42}_{0.60} (1 σ C.L. errors). Very similar results are found in the case of timeevolving dark energy with a constant equationofstate parameter w=const (the XCDM parametrization). Finally, we show that the impact of bounds on ( w 0, w a ) is to favor topdown phantom models of evolving dark energy.
Item Type:  Article 

Subjects:  Q Science > QB Astronomy Q Science > QC Physics 
Depositing User:  Prof. Tina Kahniashvili 
Date Deposited:  30 Jan 2014 12:53 
Last Modified:  27 Mar 2015 07:08 
URI:  http://eprints.iliauni.edu.ge/id/eprint/777 
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