Galaxy Clusters at z ≥ 1: Gas Constraints from the Sunyaev–Zel'dovich Array
Creators
- Culverhouse, T. L.1
- Bonamente, M.2, 3
- Bulbul, E.2
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Carlstrom, J. E.1
- Gralla, M. B.1
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Greer, C.1
- Hasler, N.2
- Hawkins, D.4
- Hennessy, R.1
- Jetha, N. N.2, 3
- Joy, M.3
- Lamb, J. W.4
- Leitch, E. M.1
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Marrone, D. P.1
- Miller, A.5
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Mroczkowski, T.5, 6
- Muchovej, S.4, 5
- Pryke, C.1
- Sharp, M.1
- Woody, D. P.4
- Andreon, S.
- Maughan, B.7
- Stanford, S. A.8, 9
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1.
University of Chicago
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2.
University of Alabama in Huntsville
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3.
Marshall Space Flight Center
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4.
California Institute of Technology
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5.
Columbia University
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6.
University of Pennsylvania
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7.
University of Bristol
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8.
University of California, Davis
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9.
Lawrence Livermore National Laboratory
Abstract
We present gas constraints from Sunyaev-Zel'dovich (SZ) effect measurements in a sample of 11 X-ray and infrared (IR) selected galaxy clusters at z ≥ 1, using data from the Sunyaev-Zel'dovich Array (SZA). The cylindrically integrated Compton-y parameter, Y, is calculated by fitting the data to a two-parameter gas pressure profile. Where possible, we also determine the temperature of the hot intracluster plasma from Chandra and XMM-Newton data and constrain the gas mass within the same aperture (r_(2500)) as Y. The SZ effect is detected in the clusters for which the X-ray data indicate gas masses above ~10^(13) M _⊙, including XMMU J2235 – 2557 at redshift z = 1.39, which to date is one of the most distant clusters detected using the SZ effect. None of the IR-selected targets are detected by the SZA measurements, indicating low gas masses for these objects. For these and the four other undetected clusters, we quote upper limits on Y and M_(gas,SZ), with the latter derived from scaling relations calibrated with lower redshift clusters. We compare the constraints on Y and X-ray-derived gas mass M_(gas,X-ray) to self-similar scaling relations between these observables determined from observations of lower redshift clusters, finding consistency given the measurement error.
Additional Information
© 2010 The American Astronomical Society. Received 2010 July 8; accepted 2010 September 8; published 2010 October 13. The operation of the SZA is supported by the NSF through grant AST-0604982 and AST-0838187. Partial support is also provided from grant PHY-0114422 at the University of Chicago, and by the NSF grants AST-0507545 and AST-05-07161 to Columbia University. CARMA operations are supported by the NSF under a cooperative agreement, and by the CARMA partner universities. S.M. acknowledges support from an NSF Astronomy and Astrophysics Fellowship; C.G., S.M., and M.S. from NSF Graduate Research Fellowships; D.P.M. from NASA Hubble Fellowship grant HF-51259.01.Attached Files
Published - Culverhouse2010p12078Astrophys_J_Lett.pdf
Files
Culverhouse2010p12078Astrophys_J_Lett.pdf
Additional details
Identifiers
- Eprint ID
- 21162
- Resolver ID
- CaltechAUTHORS:20101206-092457615
Funding
- NSF Astronomy and Astrophysics Fellowship
- NSF Graduate Research Fellowship
- Hubble Fellowship
- HF-51259.01
Dates
- Created
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2010-12-06Created from EPrint's datestamp field
- Updated
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2021-11-09Created from EPrint's last_modified field
Caltech Custom Metadata
- Caltech groups
- Physics Department