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CFHTLenS: combined probe cosmological model comparison using 2D weak gravitational lensing

Kilbinger, Martin and Fu, Liping and Heymans, Catherine and Simpson, Fergus and Benjamin, Jonathan and Erben, Thomas and Harnois-Déraps, Joachim and Hoekstra, Henk and Hilderbrandt, Hendrik and Kitching, Thomas D. and Mellier, Yannick and Miller, Lance and Van Waerbeke, Ludovic and Benabed, Karim and Bonnett, Christopher and Coupon, Jean and Hudson, Michael J. and Kuijken, Konrad and Rowe, Barnaby and Schrabback, Tim and Semboloni, Elisabetta and Vafaei, Sanaz and Velander, Malin (2013) CFHTLenS: combined probe cosmological model comparison using 2D weak gravitational lensing. Monthly Notices of the Royal Astronomical Society, 430 (3). pp. 2200-2220. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20130627-095852442

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Abstract

We present cosmological constraints from 2D weak gravitational lensing by the large-scale structure in the Canada–France–Hawaii Telescope Lensing Survey (CFHTLenS) which spans 154 deg^2 in five optical bands. Using accurate photometric redshifts and measured shapes for 4.2 million galaxies between redshifts of 0.2 and 1.3, we compute the 2D cosmic shear correlation function over angular scales ranging between 0.8 and 350 arcmin. Using non-linear models of the dark-matter power spectrum, we constrain cosmological parameters by exploring the parameter space with Population Monte Carlo sampling. The best constraints from lensing alone are obtained for the small-scale density-fluctuations amplitude σ_8 scaled with the total matter density Ωm. For a flat Λcold dark matter (ΛCDM) model we obtain σ_8(Ω_m/0.27)0.6 = 0.79 ± 0.03. We combine the CFHTLenS data with 7-year Wilkinson Microwave Anisotropy Probe (WMAP7), baryonic acoustic oscillations (BAO): SDSS-III (BOSS) and a Hubble Space Telescope distance-ladder prior on the Hubble constant to get joint constraints. For a flat ΛCDM model, we find Ω_m = 0.283 ± 0.010 and σ_8 = 0.813 ± 0.014. In the case of a curved wCDM universe, we obtain Ω_m = 0.27 ± 0.03, σ_8 = 0.83 ± 0.04, w0 = −1.10 ± 0.15 and Ω_K = 0.006^(+0.006)_(− 0.004). We calculate the Bayesian evidence to compare flat and curved ΛCDM and dark-energy CDM models. From the combination of all four probes, we find models with curvature to be at moderately disfavoured with respect to the flat case. A simple dark-energy model is indistinguishable from ΛCDM. Our results therefore do not necessitate any deviations from the standard cosmological model.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1093/mnras/stt041DOIUNSPECIFIED
http://mnras.oxfordjournals.org/content/430/3/2200PublisherUNSPECIFIED
Additional Information:© 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2013 January 7. Received 2013 January 7; in original form 2012 October 9. First published online: February 12, 2013. We would like to thank the anonymous referee for useful suggestions which helped to improve the paper. Further, we thank P. Schneider for insightful comments and discussions. This work is based on observations obtained with MegaPrime/MegaCam, a joint project of the Canada–France–Hawaii Telescope (CFHT) and CEA/Irfu, at CFHT which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l’Univers (INSU) at the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This research used the facilities of the Canadian Astronomy Data Centre operated by the NRC of Canada with the support of the Canadian Space Agency. We thank the CFHT staff, in particular J.-C. Cuillandre and E. Magnier, for the observations, data processing and continuous improvement of the instrument calibration. We also thank TERAPIX for quality assessment, and E. Bertin for developing some of the software used in this study. CFHTLenS data processing was made possible thanks to the support from the Natural Sciences and Engineering Research Council of Canada (NSERC) and HPC specialist O. Toader. The N-body simulations were performed on the TCS supercomputer at the SciNet HPC Consortium. The early stages of the CFHTLenS project were made possible thanks to the European Commissions Marie Curie Research Training Network DUEL (MRTN-CT-2006-036133) and its support of CFHTLenS team members LF, HHi and BR. MK is supported in parts by the Deutsche Forschungsgemeinschaft (DFG) cluster of excellence ‘Origin and Structure of the Universe’. LF acknowledges support from NSFC grants 11103012 and 10878003, Innovation Program 12ZZ134 and Chen Guang project 10CG46 of SMEC, and STCSM grant 11290706600 & Pujiang Program 12PJ1406700. CH and FS acknowledge support from the European Research Council (ERC) through grant 240185. TE is supported by the DFG through project ER 327/3-1 and the Transregional Collaborative Research Centre TR 33. HHo acknowledges support fromMarie Curie IRG grant 230924, the Netherlands Organization for Scientific Research (NWO) through grant 639.042.814 and from the ERC through grant 279396. HHi is supported by the Marie Curie IOF 252760 and by a CITA National Fellowship. TDK is supported by a Royal Society University Research Fellowship. YM acknowledges support from CNRS/INSU and the Programme National Galaxies et Cosmologie (PNCG). LVW and MJH acknowledge support from NSERC. LVW also acknowledges support from the Canadian Institute for Advanced Research (CIfAR; Cosmology and Gravity program). BR acknowledges support from the ERC through grant 24067, and the Jet Propulsion Laboratory, California Institute of Technology (NASA). TS acknowledges support from NSF through grant AST-0444059-001, SAO through grant GO0-11147A, andNWO. ES acknowledges support from th NWO grant 639.042.814 and support from ERC under grant 279396. MV acknowledges support from NWO and from the Beecroft Institute for Particle Astrophysics and Cosmology. Author Contribution: All authors contributed to the development and writing of this paper. The authorship list reflects the lead authors of this paper (MK, LF, CH and FS) followed by two alphabetical groups. The first group includes key contributers to the science analysis and interpretation in this paper, the founding core team and those whose long-term significant effort produced the final CFHTLenS data product. The second group covers members of the CFHTLenS team who made a significant contribution to either the project, this paper or both, and external authors. JHD, SV and LVW produced the numerical simulations and, with CH, created the clone. The CFHTLenS collaboration was co-led by CH and LVW, and the CFHTLenS Cosmology Working Group was led by TDK.
Funders:
Funding AgencyGrant Number
European Commissions Marie Curie Research Training Network DUELMRTN-CT-2006- 036133
Deutsche Forschungsgemeinschaft (DFG)UNSPECIFIED
NSFC11103012
NSFC10878003
SMEC Innovation Program12ZZ134
SMEC Chen Guang project 10CG46
STCSM11290706600
Pujiang Program12PJ1406700
European Research Council (ERC)240185
Deutsche Forschungsgemeinschaft (DFG)ER 327/3-1
Transregional Collaborative Research CentreTR 33
Marie Curie IRG grant230924
Netherlands Organization for Scientific Research (NWO)639.042.814
European Research Council (ERC)279396
Marie Curie IOF252760
CITA National FellowshipUNSPECIFIED
Royal Society University Research FellowshipUNSPECIFIED
CNRS/INSUUNSPECIFIED
Programme National Galaxies et Cosmologie (PNCG)UNSPECIFIED
NSERCUNSPECIFIED
Canadian Institute for Advanced Research (CIfAR)UNSPECIFIED
European Research Council (ERC)24067
JPL/CaltechUNSPECIFIED
NASAUNSPECIFIED
NSFAST-0444059-001
SAOGO0-11147A
Beecroft Institute for Particle Astrophysics and CosmologyUNSPECIFIED
Subject Keywords:methods: statistical; cosmological parameters
Record Number:CaltechAUTHORS:20130627-095852442
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20130627-095852442
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:39121
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:01 Jul 2013 20:45
Last Modified:01 Jul 2013 20:45

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