Daniel P. Marrone et al 2009 ApJ 701 L114 doi:10.1088/0004-637X/701/2/L114
Daniel P. Marrone1,2,15, Graham P. Smith3, Johan Richard4,5, Marshall Joy6, Massimiliano Bonamente7, Nicole Hasler7, Victoria Hamilton-Morris3, Jean-Paul Kneib8, Thomas Culverhouse1,2, John E. Carlstrom1,2,9,10, Christopher Greer1,2, David Hawkins11, Ryan Hennessy1,2, James W. Lamb11, Erik M. Leitch1,2, Michael Loh1,8, Amber Miller12,13, Tony Mroczkowski12,14, Stephen Muchovej11,14, Clem Pryke1,2,10, Matthew K. Sharp1,9 and David Woody11
Show affiliationsWe 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
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.
cosmology: observations; galaxies: clusters: general; gravitational lensing
98.62.Sb Gravitational lenses and luminous arcs
98.70.Vc Background radiations
98.62.Ck Masses and mass distribution
98.65.-r Galaxy groups, clusters, and superclusters; large scale structure of the Universe
98.62.Lv Stellar content and populations; radii; morphology and overall structure
Issue 2 (2009 August 20)
Received 2009 April 7, accepted for publication 2009 July 6
Published 2009 August 10
Daniel P. Marrone et al 2009 ApJ 701 L114
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