We present BeppoSAX results of a spatially resolved spectral analysis of A3571 , a relaxed nearby cluster of galaxies .
In the central 2′ ( 130 { h _ { 50 } ^ { -1 } } kpc ) radius the metal abundance is 0.49 \pm 0.08 solar and the absorption ( 1.13 \pm 0.28 ) \times 10 ^ { 21 } atom cm ^ { -2 } , whereas elsewhere within an 8′ ( 520 { h _ { 50 } ^ { -1 } } kpc ) radius the abundance is 0.32 \pm 0.05 solar and the absorption consistent with the galactic value of 4.4 \times 10 ^ { 20 } atom cm ^ { -2 } .
The significant central metal abundance enhancement is consistent with the supernova enrichment scenario .
The excess absorption may be attributed to the cooling flow , whose mass flow rate is 80 \pm 40 { M _ { \odot } } yr ^ { -1 } from our spectral fit .
The BeppoSAX and ASCA radial temperature profiles agree over the entire overlapping radial range r < 25′ = 1.6 { h _ { 50 } ^ { -1 } } Mpc .
The combined BeppoSAX and ASCA temperature profile exhibits a constant value out to a radius of \sim 10′ ( 650 { h _ { 50 } ^ { -1 } } kpc ) and a significant decrease ( { T \propto r ^ { -0.55 } } , corresponding to \gamma = 1.28 ) at larger radii .
These temperature data are used to derive the total mass profile .
The best fit NFW dark matter density model results in a temperature profile that is not convectively stable , but the model is acceptable within the uncertainties of the data .
The temperature profile is acceptably modeled with a “ core ” model for the dark matter density , consisting of a core radius with a constant slope at larger radii .
With this model the total mass and formal 90 % confidence errors within the virial radius r _ { 178 } ( 2.5 { h _ { 50 } ^ { -1 } } Mpc ) are { 9.1 ^ { +3.6 } _ { -1.5 } \times 10 ^ { 14 } h _ { 50 } ^ { -1 } M _ { \odot } } , by a factor of 1.4 smaller than the isothermal value .
The gas mass fraction increases with radius , reaching f { { } _ { gas } ( r _ { 178 } ) = 0.26 ^ { +0.05 } _ { -0.10 } \times h _ { 50 } ^ { -3 / 2 } } .
Assuming that the measured gas mass fraction is the lower limit to the primordial baryonic fraction gives { \Omega _ { m } < 0.4 } at 90 % confidence .