X-ray Constraints on the Intrinsic Shapes and Baryon Fractions of Five Abell Clusters

Details X-ray Constraints on the Intrinsic Shapes and Baryon Fractions of Five Abell Clusters X-ray Constraints on the Intrinsic Shapes and Baryon Fractions of Five Abell Clusters

1995-04-15

arxiv.org/abs/astro-ph/9504049v3

Astrophys.J. 457 (1996) 565

Astronomy and Astrophysics

Astrophysics

29 pages (2 figures), PostScript, to appear in ApJ on February 1, 1996. No changes to the text -- the publication date given b

Scientific paper

10.1086/176753

We analyzed ROSAT PSPC images of the bright, nearby $(z<0.1)$ galaxy clusters A401, A1656 (Coma), A2029, A2199, and A2256 to constrain their intrinsic shapes and baryon fractions. Following Buote & Tsai we probed the aggregate structure of the clusters on scales $\sim 1.5h^{-1}_{80}$ Mpc to reduce effects of possible substructure on smaller scales ($\lesssim$ a few hundred kpc). The ellipticities of the X-ray isophotes are typically $\epsilon\approx 0.15 - 0.25$ and display negative radial gradients significant (except Coma). By assuming hydrostatic equilibrium and a variety of mass models we obtain ellipticities $\epsilon_{mass} \approx 0.40-0.55$ for isothermal models of the total gravitating matter of the clusters; the $\epsilon_{mass}$ constraints change by $<10%$ upon consideration of the small temperature gradients shown by ASCA to be typical for rich clusters; the observed X-ray ellipticity gradients require that mass models with constant ellipticity have steep density profiles, $\rho\propto r^{-4}$. Estimates of the gas masses are highly insensitive to the ellipticities of the X-ray isophotes. The clusters in our sample have increasing fractions of gas mass to total mass with radius and have $M_{gas}/M_{tot} = (4% - 11%)h^{-3/2}_{80}$ within a radius $1.5h^{-1}_{80}$ Mpc, in excellent agreement with the results of White & Fabian and the Baryon Catastrophe proposed by White et al. (1993). Finally, the ellipticities of the dark matter distributions are essentially identical to $\epsilon_{mass}$ and are consistent with the shapes of dark halos predicted by N-body simulations and the shapes of the galaxy isopleths in the clusters in contrast to our previous conclusions using {\it Einstein} data.

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