COSMOLOGICAL CONSTRAINTS FROM CLUSTER X-RAY MORPHOLOGIES

Details COSMOLOGICAL CONSTRAINTS FROM CLUSTER X-RAY MORPHOLOGIES COSMOLOGICAL CONSTRAINTS FROM CLUSTER X-RAY MORPHOLOGIES

1995-01-04

arxiv.org/abs/astro-ph/9501011v1

Astrophys.J. 447 (1995) 8

Astronomy and Astrophysics

Astrophysics

uuencoded, compressed postscript, (mohr@cfa.harvard.edu)

Scientific paper

10.1086/175852

We use a representative sample of 65 galaxy clusters observed with the Einstein IPC to constrain the range of cluster X-ray morphologies. We develop and apply quantitative and reproducible measures to constrain the intrinsic distributions of emission weighted centroid variation, axial ratio, orientation, and the radial fall--off. We then use the range of cluster X--ray morphologies to constrain three generic cosmological models (Omega=1, Omega_0=0.2, and Omega_0=0.2 & lambda_0=0.8). For each of these models, we evolve eight sets of Gaussian random initial conditions consistent with an effective power spectrum $P(k)\propto k^{-1}$ on cluster scales. Using this sample of 24 numerical cluster simulations, we compare the X--ray morphologies of the observed and simulated clusters. The comparisons indicate that: (i) cluster centroid variations, axial ratios, and radial fall-offs are sensitive to the underlying cosmological model, and (ii) galaxy clusters with the observed range of X--ray morphologies are very unlikely in low Omega_0 cosmologies. The analysis favors the Omega=1 model, though some discrepancies remain. We discuss the effects of changing the initial conditions and including additional physics in the simulations.

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