Mathematics – Logic
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...201.6706r&link_type=abstract
American Astronomical Society, 201st AAS Meeting, #67.06; Bulletin of the American Astronomical Society, Vol. 34, p.1218
Mathematics
Logic
2
Scientific paper
N-body/hydrodynamical simulations of merging galaxy clusters have shown that a merger can temporarily boost the X-ray luminosity and temperature of the merged cluster above the equilibrium values. The cumulative effect of these ``merger boosts'' will affect the observed X-ray luminosity functions (XLFs) and temperature functions (TFs) of clusters, which provide strong constraints on cosmological parameters. We use N-body/hydrodynamical simulations to derive boosts for individual mergers and Monte Carlo simulations of cluster merger histories (``merger trees'') to determine the cumulative effect of merger boosts. We find that merger boosts can have a significant effect on the XLFs and TFs inferred from X-ray observations. For example, in a Universe with Ω M = 0.3 and Ω Λ = 0.7 at a redshift of z=1, the number of clusters with temperatures T >10 keV is increased by a factor of 9.5, and the number of clusters with luminosities LX > 5 x 1044 h-2 erg s-1 is increased by a factor of 8.9. Merger boosts bias the values of σ 8 and Ω M inferred from cluster XLFs and TFs if virial equilibrium is assumed. Merger boosts cause σ 8 to be overestimated by about 20% and Ω M may be underestimated by about 20%. We are currently using our merger tree code to evaluate the effect that cluster mergers have on non-thermal radio emission from clusters. Since cluster mergers also temporarily boost radio emission, it is possible that merger boosts may explain the observed steep relations between radio luminosity and X-ray luminosity or temperature. We have also shown that EUV emission from clusters of galaxies (due to inverse Compton scattering of the Cosmic Microwave Background) is a negligible component of the diffuse EUV background. This work was supported in part by Chandra Award Numbers GO1-2123X and GO2-3159X and NASA XMM/Newton Grant NAG5-10075.
Randall Scott W.
Ricker Paul M.
Sarazin Craig L.
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