X-ray Cluster Evolution and Projection Effects in a CHDM Universe

Details X-ray Cluster Evolution and Projection Effects in a CHDM Universe X-ray Cluster Evolution and Projection Effects in a CHDM Universe

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aas...185.7415l&link_type=abstract

American Astronomical Society, 185th AAS Meeting, #74.15; Bulletin of the American Astronomical Society, Vol. 26, p.1429

Astronomy and Astrophysics

Astronomy

Scientific paper

We have generated surface-brightness projections of large-scale structure simulations (at different epochs) in the Einstein and ROSAT bandpasses in order to calculate the probabilities of misidentifying filaments and projected groups as rich clusters. Cluster masses are tracked as a function of time in order to estimate cluster merger and mass accretion rates. We also show how cluster profiles vary with time and fit King models to the cold, hot and baryonic components in order to estimate core radii and slopes. The particular simulations used for this analysis self-consistently evolve both baryons (gas) and dark matter in a CHDM universe. The X-ray properties of the resulting clusters have already been shown to agree well with observational results(Bryan et. al 1994).

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