Measuring the Three-dimensional Structure of Galaxy Clusters. I. Application to a Sample of 25 Clusters

By E. De Filippis, M. Sereno, M. Bautz, G. Longo. 2005

184 citations recorded by the source corpus.

We discuss a method to constrain the intrinsic shapes of galaxy clusters by combining X-ray and Sunyaev-Zel'dovich observations. The method is applied to a sample of 25 X-ray-selected clusters, with measured Sunyaev-Zel'dovich temperature decrements. The sample turns out to be slightly biased, with strongly elongated clusters preferentially aligned along the line of sight. This result demonstrates that X-ray-selected cluster samples may be affected by morphological and orientation effects, even if a relatively high threshold signal-to-noise ratio is used to select the sample. A large majority of the clusters in our sample exhibit a marked triaxial structure; the spherical hypothesis is strongly rejected for most sample members. Cooling-flow clusters do not show preferentially regular morphologies. We also show that identification of multiple gravitationally lensed images, together with measurements of the Sunyaev-Zel'dovich effect and X-ray surface brightness, can provide a simultaneous determination of the three-dimensional structure of a cluster, of the Hubble constant, and of the cosmological energy density parameters.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/4c5133bfc5687062cb9c03d47223148650ecec1f

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In Astronomy and Astrophysics

1. Richard S. Ellis
2. J. Richard
3. T. Treu
4. E. Jullo
5. A. Newman
6. D. Sand
7. Graham P. Smith
8. S. M. Moran

Citations in the corpus

• THE DENSITY PROFILES OF MASSIVE, RELAXED GALAXY CLUSTERS. I. THE TOTAL DENSITY OVER THREE DECADES IN RADIUS (2012, background): “…SunyaevZel’dovich-based) and nearly spherical (X-ray) mass measures, the l.o.s. shape can be inferred (e.g., Piffaretti et al. 2003; Gavazzi 2005; De Filippis et al. 2005; Sereno et al. 2006; Morandi et al. 2010, 2011; Newman et al. 2011; Morandi & Limousin 2012) assuming that the ICM is near…”
• Searching for cool core clusters at high redshift (2008, background): “2005, Bauer et al. 2005, Reese et al. 2002, De Filippis et al. 2005, Arabadjis et al. 2002, Pratt & Arnaud 2002.”
• TESTING THE DISTANCE–DUALITY RELATION WITH GALAXY CLUSTERS AND TYPE Ia SUPERNOVAE (2010, methodology): “In the case of De Filippis et al. (2005) sample (see Fig.”
• A Wide-Field Survey of Two z ~ 0.5 Galaxy Clusters: Identifying the Physical Processes Responsible for the Observed Transformation of Spirals into S0s (2007, result): “…field is due to cluster-scale rotation, previous analyses of the X-ray and Sunyaev-Zeldovich observations prefer a prolate or triaxial shape for MS 0451 (Donahue et al. 2003; De Filippis et al. 2005), whereas the cluster would necessarily be oblate if the observed velocities are due to rotation.”