Cosmological Constraints from the Observed Growth of X-ray Luminous Galaxy Clusters

Details Cosmological Constraints from the Observed Growth of X-ray Luminous Galaxy Clusters Cosmological Constraints from the Observed Growth of X-ray Luminous Galaxy Clusters

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008head...10.2507m&link_type=abstract

American Astronomical Society, HEAD meeting #10, #25.07

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We present constraints on the mean matter density, Ωm, normalization of the density fluctuation power spectrum, ▦, and dark energy equation of state parameter, w, obtained from the X-ray luminosity function of the Massive Cluster Survey (MACS) in combination with the local BCS and REFLEX galaxy cluster samples. Our analysis incorporates the mass function predictions of Jenkins et al. (2001), a mass--luminosity relation calibrated using the data of Reiprich and Bohringer (2002), and standard priors on the Hubble constant and mean baryon density. We find Ωm=0.37+0.12-0.08 and ▦=0.70+0.08-0.11 for a spatially flat, cosmological constant model, and Ωm=0.35+0.14-0.09, ▦=0.72+0.10-0.13 and w=-1.5+0.6-0.9 for a flat, constant-w model (marginalized 68 per cent confidence intervals). Our findings constitute the first determination of the dark energy equation of state from measurements of the growth of cosmic structure in galaxy clusters, and the consistency of our result with w=-1 lends additional support to the cosmological constant model. Future work improving our understanding of redshift evolution and X-ray observational biases affecting the mass-luminosity relation have the potential to greatly improve these constraints. Our results compare favorably with those from recent analyses of type Ia supernovae, cosmic microwave background anisotropies, the X-ray gas mass fraction of relaxed galaxy clusters and cosmic shear. Combining the luminosity function data with supernova, cosmic microwave background and cluster gas fraction data yields the improved constraints Ωm=0.271+0.014-0.016, ▦=0.81±0.03 and w=-1.02±0.05. This work was supported by grants from NASA and the U.S. Department of Energy, and by a Stanford Graduate Fellowship.

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