Scaling relations from Sunyaev-Zel'dovich effect and Chandra X-ray measurements of high-redshift galaxy clusters
Abstract
We present Sunyaev-Zel'dovich Effect (SZE) scaling relations for 38 massive galaxy clusters at redshifts 0.14 ≤ z≤ 0.89, observed with both the Chandra X-ray Observatory and the centimeter-wave SZE imaging system at the BIMA and OVRO interferometric arrays. An isothermal β-model with the central 100 kpc excluded from the X-ray data is used to model the intracluster medium and to measure global cluster properties. For each cluster, we measure the X-ray spectroscopic temperature, SZE gas mass, total mass, and integrated Compton y-parameters within r2500. Our measurements are in agreement with the expectations based on a simple self-similar model of cluster formation and evolution. We compare the cluster properties derived from our SZE observations with and without Chandra spatial and spectral information and find them to be in good agreement. We compare our results with cosmological numerical simulations and find that simulations that include radiative cooling, star formation, and feedback match well both the slope and normalization of our SZE scaling relations.
Additional Information
© 2008. The American Astronomical Society. Received 2007 August 3; accepted 2007 November 2. This work was made possible by the skill and dedication of Leon van Speybroeck and his colleagues on the Chandra project, who constructed an exceptional observatory and obtained deep X-ray observations for a large sample of galaxy clusters. We thank E. Leitch and the anonymous referee for excellent suggestions on the manuscript. The support of the BIMA and OVRO staff over many years is also gratefully acknowledged, including J. R. Forster, C. Giovanine, R. Lawrence, S. Padin, R. Plambeck, S. Scott, and D. Woody. We thank C. Alexander, K. Coble, A. Cooray, K. Dawson, L. Grego, G. Holder, W. Holzapfel, A. Miller, J. Mohr, S. Patel, E. Reese, and P. Whitehouse for their outstanding contributions to the SZE instrumentation, observations, and analysis. This work was supported in part by NSF grants AST 00-96913 and AST 06-04982 and by the KICP NSF Physics Frontier Center grant PHY 01-14422. Research at the Owens Valley Radio Observatory and the Berkeley-Illinois-Maryland Array was supported by National Science Foundation grants AST 99-81546 and 02-28963. Calculations were performed at the Space Plasma Interactive Data Analysis and Simulation Laboratory at the Center for Space Plasma and Aeronomy Research of the University of Alabama at Huntsville. D. N. is supported by the Sherman Fairchild Postdoctoral Fellowship at Caltech. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.Attached Files
Published - BONapj08.pdf
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Additional details
- Eprint ID
- 13867
- Resolver ID
- CaltechAUTHORS:20090407-101728774
- AST 00-96913
- NSF
- AST 06-04982
- NSF
- AST 99-81546
- NSF
- AST 02-28963
- NSF
- PHY 01-14422
- NSF
- Sherman Fairchild Foundation
- Created
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2009-07-16Created from EPrint's datestamp field
- Updated
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2021-11-08Created from EPrint's last_modified field