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A Weak Lensing Study of X-ray Groups in the Cosmos Survey: Form and Evolution of the Mass-Luminosity Relation

Leauthaud, Alexei and Finoguenov, Alexis and Kneib, Jean-Paul and Taylor, James E. and Massey, Richard and Rhodes, Jason and Ilbert, Olivier and Bundy, Kevin and Tinker, Jeremy and George, Matthew R. and Capak, Peter and Koekemoer, Anton M. and Johnston, David E. and Zhang, Yu-Ying and Cappelutti, Nico and Ellis, Richard S. and Elvis, Martin and Giodini, Stefania and Heymans, Catherine and Le Fèvre, Olivier and Lilly, Simon and McCracken, Henry J. and Mellier, Yannick and Réfrégier, Alexandre and Salvato, Mara and Scoville, Nick and Smoot, George and Tanaka, Masayuki and Van Waerbeke, Ludovic and Wolk, Melody (2010) A Weak Lensing Study of X-ray Groups in the Cosmos Survey: Form and Evolution of the Mass-Luminosity Relation. Astrophysical Journal, 709 (1). pp. 97-114. ISSN 0004-637X. doi:10.1088/0004-637X/709/1/97.

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Measurements of X-ray scaling laws are critical for improving cosmological constraints derived with the halo mass function and for understanding the physical processes that govern the heating and cooling of the intracluster medium. In this paper, we use a sample of 206 X-ray-selected galaxy groups to investigate the scaling relation between X-ray luminosity (L_X) and halo mass (M_(200)) where M_(200) is derived via stacked weak gravitational lensing. This work draws upon a broad array of multi-wavelength COSMOS observations including 1.64 degrees^2 of contiguous imaging with the Advanced Camera for Surveys to a limiting magnitude of I_(F814W) = 26.5 and deep XMM-Newton/Chandra imaging to a limiting flux of 1.0 × 10^(–15) erg cm6(–2) s^(–1) in the 0.5-2 keV band. The combined depth of these two data sets allows us to probe the lensing signals of X-ray-detected structures at both higher redshifts and lower masses than previously explored. Weak lensing profiles and halo masses are derived for nine sub-samples, narrowly binned in luminosity and redshift. The COSMOS data alone are well fit by a power law, M_(200) (L_X)^α, with a slope of α = 0.66 ± 0.14. These results significantly extend the dynamic range for which the halo masses of X-ray-selected structures have been measured with weak gravitational lensing. As a result, tight constraints are obtained for the slope of the M-L_X relation. The combination of our group data with previously published cluster data demonstrates that the M-L_X relation is well described by a single power law, α = 0.64 ± 0.03, over two decades in mass, M_(200) ~ 10^(13.5)-10^(15.5) h^(–1)_72 M_☉. These results are inconsistent at the 3.7σ level with the self-similar prediction of α = 0.75. We examine the redshift dependence of the M-L_X relation and find little evidence for evolution beyond the rate predicted by self-similarity from z ~ 0.25 to z ~ 0.

Item Type:Article
Related URLs:
URLURL TypeDescription
Leauthaud, Alexei0000-0002-3677-3617
Finoguenov, Alexis0000-0002-4606-5403
Kneib, Jean-Paul0000-0002-4616-4989
Massey, Richard0000-0002-6085-3780
Rhodes, Jason0000-0002-4485-8549
Ilbert, Olivier0000-0002-7303-4397
Bundy, Kevin0000-0001-9742-3138
Capak, Peter0000-0003-3578-6843
Koekemoer, Anton M.0000-0002-6610-2048
Ellis, Richard S.0000-0001-7782-7071
Le Fèvre, Olivier0000-0001-5891-2596
Lilly, Simon0000-0002-6423-3597
McCracken, Henry J.0000-0002-9489-7765
Salvato, Mara0000-0001-7116-9303
Scoville, Nick0000-0002-0438-3323
Tanaka, Masayuki0000-0002-5011-5178
Additional Information:© 2010 American Astronomical Society. Print publication: Issue 1 (2010 January 20); received 2009 May 9; accepted for publication 2009 November 12; published 2009 December 29. We thank Uros Seljak, Reiko Nakajima, Henk Hoekstra, Rachel Mandelbaum, Chris Hirata, Masahiro Takada, and Satoshi Miyazaki for useful discussions. We thank Florian Pacaud for providing X-ray data for this analysis. We are also grateful to Eduardo Rozo and to Joel Berg´e for providing comments on the manuscript and to an anonymous referee for insightful comments. A.L. acknowledges support from the Chamberlain Fellowship at LBNL and from the Berkeley Center for Cosmological Physics. J.P.K. acknowledges CNRS and CNES for support. J.P.K. and H.J.M.C.C. acknowledge support from the research grant ANR-07-BLAN-0228. The HST COSMOS Treasury program was supported through NASA grant HST-GO-09822. We thank Tony Roman, Denise Taylor, and David Soderblom for their assistance in planning and scheduling of the extensive COSMOS observations. We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. More information on the COSMOS survey is available at It is a pleasure to acknowledge the excellent services provided by the NASA IPAC/IRSA staff (Anastasia Laity, Anastasia Alexov, Bruce Berriman, and John Good) in providing online archive and server capabilities for the COSMOS data sets.
Group:COSMOS, Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Chamberlain FellowshipUNSPECIFIED
Berkeley Center for Cosmological PhysicsUNSPECIFIED
Centre National d'Études Spatiales (CNES)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)ANR-07-BLAN-0228
Subject Keywords:cosmology: observations; gravitational lensing; large-scale structure of universe
Issue or Number:1
Record Number:CaltechAUTHORS:20100201-100414082
Persistent URL:
Official Citation:A Weak Lensing Study of X-ray Groups in the Cosmos Survey: Form and Evolution of the Mass-Luminosity Relation Alexie Leauthaud, Alexis Finoguenov, Jean-Paul Kneib, James E. Taylor, Richard Massey, Jason Rhodes, Olivier Ilbert, Kevin Bundy, Jeremy Tinker, Matthew R. George, Peter Capak, Anton M. Koekemoer, David E. Johnston, Yu-Ying Zhang, Nico Cappelluti, Richard S. Ellis, Martin Elvis, Stefania Giodini, Catherine Heymans, Oliver Le Fèvre, Simon Lilly, Henry J. McCracken, Yannick Mellier, Alexandre Réfrégier, Mara Salvato, Nick Scoville, George Smoot, Masayuki Tanaka, Ludovic Van Waerbeke, and Melody Wolk 2010 ApJ 709 97-114 doi: 10.1088/0004-637X/709/1/97
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:17361
Deposited On:01 Feb 2010 19:31
Last Modified:08 Nov 2021 23:35

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