Volume 487, Number 1, August III 2008
|Page(s)||75 - 87|
|Section||Cosmology (including clusters of galaxies)|
|Published online||04 June 2008|
Cluster geometry and inclinations from deprojection uncertainties
Cluster geometry and inclination
School of Physics & Astronomy, University of Nottingham, Nottingham NG7 2RD, UK e-mail: dalia.chakrabarty$@$nottingham.ac.uk
2 Department of Physical Sciences, University of Napoli Federico II, via Cintia 6, 80126 Napoli, Italy e-mail: email@example.com
3 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK e-mail: firstname.lastname@example.org
Accepted: 30 May 2008
Context. The determination of cluster masses is a complex problem that would be aided by information about the cluster shape and orientation (with respect to the line-of-sight).
Aims. It is in this context, that we have developed a scheme for identifying the intrinsic morphology and inclination of a cluster, by looking for the signature of the true cluster characteristics in the inter-comparison of the different deprojected emissivity profiles (that all project to the same X-ray brightness distribution) and complimenting this with SZe data when available.
Methods. We deproject the cluster X-ray surface brightness profile under assumptions about geometry and inclination that correspond to four extreme scenarios; the deprojection is performed by the non-parametric algorithm DOPING. The formalism is tested with model clusters and is then applied to a sample of 24 clusters. While the shape determination is possible by implementing the X-ray brightness alone, the estimation of the inclination is usually markedly improved upon by the usage of SZe data that is available for the considered sample.
Results. We spot 8 prolate systems, 1 oblate and 15 of the clusters in our sample as triaxial. In fact, for systems identified as triaxial, we are able to discern how the three semi-axis lengths compare with each other. This, when compounded by the information about the line-of-sight extent, allows us to constrain the intrinsic axial ratios and the inclination quite tightly.
Key words: methods: analytical / galaxies: clusters: general
© ESO, 2008
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