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Date and Time of the Query: 2019-04-19 T17:53:34 PDT
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For refcode 2010A&A...524A..68E:
Retrieve 44 NED objects in this reference.
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Copyright by European Southern Observatory (ESO). Reproduced by permission
2010A&A...524A..68E Mass profiles and c-M_DM_ relation in X-ray luminous galaxy clusters Ettori, S.; Gastaldello, F.; Leccardi, A.; Molendi, S.; Rossetti, M.; Buote, D.; Meneghetti, M. Abstract. Context. Galaxy clusters represent valuable cosmological probes using tests that mainly rely on measurements of cluster masses and baryon fractions. X-ray observations represent one of the main tools for uncovering these quantities. Aims: We aim to constrain the cosmological parameters {OMEGA}_m_ and {sigma}_8_ using the observed distribution of the both values of the concentrations and dark mass within R_200_ and of the gas mass fraction within R_500_. Methods: We applied two different techniques to recover the profiles the gas and dark mass, described according to the Navarro, Frenk & White (1997, ApJ, 490, 493) functional form, of a sample of 44 X-ray luminous galaxy clusters observed with XMM-Newton in the redshift range 0.1-0.3. We made use of the spatially resolved spectroscopic data and of the PSF-deconvolved surface brightness and assumed that hydrostatic equilibrium holds between the intracluster medium and the gravitational potential. We evaluated several systematic uncertainties that affect our reconstruction of the X-ray masses. Results: We measured the concentration c_200_, the dark mass M_200_ and the gas mass fraction in all the objects of our sample, providing the largest dataset of mass parameters for galaxy clusters in the redshift range 0.1-0.3. We confirm that a tight correlation between c_200_ and M_200_ is present and in good agreement with the predictions from numerical simulations and previous observations. When we consider a subsample of relaxed clusters that host a low entropy core, we measure a flatter c - M relation with a total scatter that is lower by 40 per cent. We conclude, however, that the slope of the c - M relation cannot be reliably determined from the fitting over a narrow mass range as the one considered in the present work. From the distribution of the estimates of c_200_ and M_200_, with associated statistical (15-25%) and systematic (5-15%) errors, we used the predicted values from semi-analytic prescriptions calibrated through N-body numerical runs and obtain {sigma}_8_ {OMEGA}_m^0.60 +/- 0.03^ = 0.45 +/- 0.01 (at 2 {sigma} level, statistical only) for the subsample of the clusters where the mass reconstruction has been obtained more robustly and {sigma}_8_ {OMEGA}_m^0.56 +/- 0.04^ = 0.39 +/- 0.02 for the subsample of the 11 more relaxed LEC objects. With the further constraint from the gas mass fraction distribution in our sample, we break the degeneracy in the {sigma}_8_ - {OMEGA}_m_ plane and obtain the best-fit values {sigma}_8_ ~ 1.0 +/- 0.2 (0.83 +/- 0.1 when the subsample of the more relaxed objects is considered) and {OMEGA}_m_ = 0.26 +/- 0.02. Conclusions: Analysis of the distribution of the c_200_ - M_200_ - f_gas_ values represents a mature and competitive technique in the present era of precision cosmology, even though it needs more detailed analysis of the output of larger sets of cosmological numerical simulations to provide definitive and robust results. Key words: galaxies: cluster: general, intergalactic medium, X-ray: galaxies: clusters, cosmology: observations, dark matter
Retrieve 44 NED objects in this reference.
Please click here for ADS abstract

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