We present gas and total mass profiles for 13 low-redshift , relaxed clusters spanning a temperature range 0.7–9 keV , derived from all available Chandra data of sufficient quality .
In all clusters , gas temperature profiles are measured to large radii ( Vikhlinin et al . )
so that direct hydrostatic mass estimates are possible to nearly r _ { 500 } or beyond .
The gas density was accurately traced to larger radii ; its profile is not described well by a beta-model , showing continuous steepening with radius .
The derived \rho _ { \text { tot } } profiles and their scaling with mass generally follow the Navarro-Frenk-White model with concentration expected for dark matter halos in \Lambda CDM cosmology .
However , in three cool clusters , we detect a central mass component in excess of the NFW profile , apparently associated with their cD galaxies .
In the inner region ( r < 0.1 ~ { } r _ { 500 } ) , the gas density and temperature profiles exhibit significant scatter and trends with mass , but they become nearly self-similar at larger radii .
Correspondingly , we find that the slope of the mass-temperature relation for these relaxed clusters is in good agreement with the simple self-similar behavior , M _ { 500 } \propto T ^ { \alpha } where \alpha = ( 1.5 - 1.6 ) \pm 0.1 , if the gas temperatures are measured excluding the central cool cores .
The normalization of this M - T relation is significantly , by \approx 30 \% , higher than most previous X-ray determinations .
We derive accurate gas mass fraction profiles , which show increase both with radius and cluster mass .
The enclosed f _ { \text { gas } } profiles within r _ { 2500 } \simeq 0.4 r _ { 500 } have not yet reached any asymptotic value and are still far ( by a factor of 1.5 - 2 ) from the Universal baryon fraction according to the CMB observations .
The f _ { \text { gas } } trends become weaker and its values closer to Universal at larger radii , in particular , in spherical shells r _ { 2500 } < r < r _ { 500 } .