X-ray total mass estimate for the nearby relaxed cluster A3571

2); (2) Observatory; 3); (3) Space Research Institute; Cambridge; Finland; J. Nevalainen (1; M. Markevitch (1; Russia); Russian Acad. of Sci.

X-ray total mass estimate for the nearby relaxed cluster A3571

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arxiv astro-ph/0001162 v1 pith:UBLULQFV submitted 2000-01-10 astro-ph

X-ray total mass estimate for the nearby relaxed cluster A3571

J. Nevalainen (1 , 2) , M. Markevitch (1 , 3) , W.R. Forman (1) ((1) Harvard Smithsonian Center for Astrophysics , Cambridge , USA , (2) Observatory

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University of Helsinki Finland (3) Space Research Institute Russian Acad. of Sci. Russia)

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We constrain the total mass distribution in the cluster A3571, combining spatially resolved ASCA temperature data with ROSAT imaging data with the assumption that the cluster is in hydrostatic equilibrium. The total mass within r_500 (1.7/h_50 Mpc) is M_500 = 7.8[+1.4,-2.2] 10^14/ h_50 Msun at 90% confidence, 1.1 times smaller than the isothermal estimate. The Navarro, Frenk & White ``universal profile'' is a good description of the dark matter density distribution in A3571. The gas density profile is shallower than the dark matter profile, scaling as r^{-2.1} at large radii, leading to a monotonically increasing gas mass fraction with radius. Within r_500 the gas mass fraction reaches a value of f_gas = 0.19[+0.06,-0.03] h_50^{-3/2} (90% confidence errors). Assuming that this value of f_gas is a lower limit for the the universal value of the baryon fraction, we estimate the 90% confidence upper limit of the cosmological matter density to be Omega_m < 0.4.

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Kinematics of Weak Cool-Core Cluster A3571 Observed with XRISM: Low Cooling Rate Balanced by Low Heating Rate
astro-ph.GA 2026-06 unverdicted novelty 4.0

XRISM kinematics measurements in A3571 find low uniform velocity dispersion whose implied turbulent heating offsets cooling, with sloshing as a major contributor.