First Measurements of the 3D Morphology of a Sample of Galaxy Clusters

Details First Measurements of the 3D Morphology of a Sample of Galaxy Clusters First Measurements of the 3D Morphology of a Sample of Galaxy Clusters

Aug 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004head....8.0202d&link_type=abstract

American Astronomical Society, HEAD meeting #8, #02.02; Bulletin of the American Astronomical Society, Vol. 36, p.903

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For many years SZ and X-ray data of galaxy clusters have been used in conjunction in order to infer fundamental cosmological informations. Results from WMAP, combined with other astronomical data, have recently enabled accurate testing of cosmological models and constrained the geometry of the universe.
Using the cosmology implied from WMAP, we are using a combined X-ray and SZ analysis to obtain detailed informations on cluster morphologies: we are able to measure their shapes, elongation along the line of sight and inclination respect to it. If also strong lensing data are available, the need for a preassumption on cosmology ceases and both cosmology and detailed morphology can be computed for a cluster at the same time. In the last years Chandra has provided unprecedented detailed images of the 2D projected appearance of galaxy clusters, but we still know so little on how and how much this is affected by projection effects. Detailed informations on the three dimensional geometry of galaxy clusters, are of fundamental importance for a better understanding of their dynamical state, which will allow a more correct determination of the spectral parameters and mass distribution. We are applying this procedure to a sample of clusters spanning a large redshift range (0.02

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