NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-07-22 T23:02:35 PDT
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For refcode 2013A&A...555A..66L:
Retrieve 124 NED objects in this reference.
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Copyright by European Southern Observatory (ESO). Reproduced by permission
2013A&A...555A..66L A comprehensive picture of baryons in groups and clusters of galaxies Lagana, T. F.; Martinet, N.; Durret, F.; Lima Neto, G. B.; Maughan, B.; Zhang, Y.-Y. Abstract. Aims: Based on XMM-Newton, Chandra, and SDSS data, we investigate the baryon distribution in groups and clusters and its use as a cosmological constraint. For this, we considered a sample of 123 systems with temperatures kT_500_ = 1.0-9.0 keV, total masses in the mass range M_500_ = (~10^13^-4 x 10^15^)h_70_^-1^ M_sun_, and redshifts 0.02 < z < 1.3. Methods: The gas masses and total masses are derived from X-ray data under the assumption of hydrostatic equilibrium and spherical symmetry. The stellar masses are based on SDSS-DR8 optical photometric data. For the 37 systems out of 123 that had both optical and X-ray data available, we investigated the gas, stellar, and total baryon mass fractions inside r_2500_ and r_500_ and the differential gas mass fraction within the spherical annulus between r_2500_ and r_500_, as a function of total mass. For the other objects, we investigated the gas mass fraction only. Results: We find that the gas mass fraction inside r_2500_ and r_500_ depends on the total mass. However, the differential gas mass fraction does not show any dependence on total mass for systems with M_500_ > 10^14^ M_sun_. The stellar mass fraction inside r_2500_ and r_500_ increases towards low-mass systems more steeply than the f_gas_ decrease with total mass. Adding the gas and stellar mass fractions to obtain the total baryonic content, we find it to increase with cluster mass, reaching the WMAP-7 value for clusters with M_500_ ~ 10^14^ M_sun_. This led us to investigate the contribution of the intracluster light to the total baryon budget for lower mass systems, but we find that it cannot account for the difference observed. Conclusions: The gas mass fraction dependence on total mass observed for groups and clusters could be due to the difficulty of low-mass systems to retain gas inside the inner region (r < r_2500_). Because of their shallower potential well, non-thermal processes are more effective in expelling the gas from their central regions outwards. Since the differential gas mass fraction is nearly constant, it provides better constraints for cosmology. Moreover, we find that the gas mass fraction does not depend on redshift at a 2sigma level. Using our total f_b_ estimates, our results imply Omega_m_ < 0.55, and taking the highest significant estimates for f_b_, Omega_m_ > 0.22. Table 1 and Appendices are available in electronic form at http://www.aanda.org Key words: galaxies: clusters: general, cosmological parameters, galaxies: clusters: intracluster medium
Retrieve 124 NED objects in this reference.
Please click here for ADS abstract

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