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Title:
LoCuSS: A Comparison of Sunyaev-Zel'dovich Effect and Gravitational-Lensing Measurements of Galaxy Clusters
Authors:
Marrone, Daniel P.; Smith, Graham P.; Richard, Johan; Joy, Marshall; Bonamente, Massimiliano; Hasler, Nicole; Hamilton-Morris, Victoria; Kneib, Jean-Paul; Culverhouse, Thomas; Carlstrom, John E.; Greer, Christopher; Hawkins, David; Hennessy, Ryan; Lamb, James W.; Leitch, Erik M.; Loh, Michael; Miller, Amber; Mroczkowski, Tony; Muchovej, Stephen; Pryke, Clem; Sharp, Matthew K.; Woody, David
Affiliation:
AA(Kavli Institute for Cosmological Physics, Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA ; Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA ; Jansky Fellow, National Radio Astronomy Observatory.), AB(School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham, B15 2TT, UK ), AC(California Institute of Technology, Mail Code 105-24, Pasadena, CA 91125, USA ; Department of Physics, Durham University, South Road, Durham, DH1 3LE, UK ), AD(Space Science Office, VP62, NASA/Marshall Space Flight Center, Huntsville, AL 35812, USA ), AE(Department of Physics, University of Alabama, Huntsville, AL 35812, USA ), AF(Department of Physics, University of Alabama, Huntsville, AL 35812, USA ), AG(School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham, B15 2TT, UK ), AH(Laboratoire d'Astrophysique de Marseilles, OAMP, CNRS-Université Aix-Marseilles, 38 rue Frédéric Joliot-Curie, 13388 Marseilles Cedex 13, France ), AI(Kavli Institute for Cosmological Physics, Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA ; Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA ), AJ(Kavli Institute for Cosmological Physics, Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA ; Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA ; Department of Physics, University of Chicago, Chicago, IL 60637, USA ; Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA ), AK(Kavli Institute for Cosmological Physics, Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA ; Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA ), AL(Owens Valley Radio Observatory, California Institute of Technology, Big Pine, CA 93513, USA ), AM(Kavli Institute for Cosmological Physics, Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA ; Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA ), AN(Owens Valley Radio Observatory, California Institute of Technology, Big Pine, CA 93513, USA ), AO(Kavli Institute for Cosmological Physics, Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA ; Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA ), AP(Kavli Institute for Cosmological Physics, Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA ; Laboratoire d'Astrophysique de Marseilles, OAMP, CNRS-Université Aix-Marseilles, 38 rue Frédéric Joliot-Curie, 13388 Marseilles Cedex 13, France ), AQ(Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA ; Department of Physics, Columbia University, New York, NY 10027, USA ), AR(Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA ; Department of Astronomy, Columbia University, New York, NY 10027, USA ), AS(Owens Valley Radio Observatory, California Institute of Technology, Big Pine, CA 93513, USA ; Department of Astronomy, Columbia University, New York, NY 10027, USA ), AT(Kavli Institute for Cosmological Physics, Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA ; Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA ; Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA ), AU(Kavli Institute for Cosmological Physics, Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA ; Department of Physics, University of Chicago, Chicago, IL 60637, USA ), AV(Owens Valley Radio Observatory, California Institute of Technology, Big Pine, CA 93513, USA )
Publication:
The Astrophysical Journal Letters, Volume 701, Issue 2, pp. L114-L118 (2009). (ApJL Homepage)
Publication Date:
08/2009
Origin:
IOP
ApJ Keywords:
cosmology: observations, galaxies: clusters: general, gravitational lensing
DOI:
10.1088/0004-637X/701/2/L114
Bibliographic Code:
2009ApJ...701L.114M

Abstract

We present the first measurement of the relationship between the Sunyaev-Zel'dovich effect (SZE) signal and the mass of galaxy clusters that uses gravitational lensing to measure cluster mass, based on 14 X-ray luminous clusters at z sime 0.2 from the Local Cluster Substructure Survey. We measure the integrated Compton y-parameter, Y, and total projected mass of the clusters (M GL) within a projected clustercentric radius of 350 kpc, corresponding to mean overdensities of 4000-8000 relative to the critical density. We find self-similar scaling between M GL and Y, with a scatter in mass at fixed Y of 32%. This scatter exceeds that predicted from numerical cluster simulations, however, it is smaller than comparable measurements of the scatter in mass at fixed TX . We also find no evidence of segregation in Y between disturbed and undisturbed clusters, as had been seen with TX on the same physical scales. We compare our scaling relation to the Bonamente et al. relation based on mass measurements that assume hydrostatic equilibrium, finding no evidence for a hydrostatic mass bias in cluster cores (M GL = 0.98 ± 0.13 M HSE), consistent with both predictions from numerical simulations and lensing/X-ray-based measurements of mass-observable scaling relations at larger radii. Overall our results suggest that the SZE may be less sensitive than X-ray observations to the details of cluster physics in cluster cores.
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