期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 441, 期 3, 页码 2725-2743出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stu754
关键词
methods: statistical; cosmological parameters
资金
- NSFC [11103012, 11333001]
- Innovation Program of SMEC [12ZZ134]
- STCSM [11290706600]
- Pujiang Program [12PJ1406700]
- Shanghai Research grant [13JC1404400]
- Natural Sciences and Engineering Research Council of Canada (NSERC)
- DFG cluster of excellence 'Origin and Structure of the Universe'
- European Research Council under the EC FP7 [240185, 279396]
- Royal Society University Research Fellowship
- Canadian Institute for Advanced Research (CIfAR, Cosmology and Gravity program)
- Deutsche Forschungsgemeinschaft [ER 327/3-1]
- Transregional Collaborative Research Centre TR 33 - 'The Dark Universe'
- Marie Curie IOF [252760]
- CITA National Fellowship
- DFG [Hi 1495/2-1]
- Marie Curie IRG [230924]
- Netherlands Organization for Scientific Research (NWO) [639.042.814]
- CNRS/INSU (Institut National des Sciences de l'Univers)
- Programme National Galaxies et Cosmologie (PNCG)
- European Research Council [240672]
- NSF [AST-0444059-001]
- SAO [GO0-11147A]
- NWO
- Beecroft Institute for Particle Astrophysics and Cosmology
- Canada Foundation for Innovation under Compute Canada
- Government of Ontario
- Ontario Research Fund - Research Excellence
- University of Toronto
- STFC [ST/H002456/1, ST/K000977/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/K000977/1, ST/H002456/1] Funding Source: researchfish
Higher order, non-Gaussian aspects of the large-scale structure carry valuable information on structure formation and cosmology, which is complementary to second-order statistics. In this work, we measure second- and third-order weak-lensing aperture-mass moments from the Canada-France-Hawaii Lensing Survey (CFHTLenS) and combine those with cosmic microwave background (CMB) anisotropy probes. The third moment is measured with a significance of 2 sigma. The combined constraint on I (8) pound = sigma(8)(Omega(m)/0.27)(alpha) is improved by 10 per cent, in comparison to the second-order only, and the allowed ranges for Omega(m) and sigma(8) are substantially reduced. Including general triangles of the lensing bispectrum yields tighter constraints compared to probing mainly equilateral triangles. Second- and third-order CFHTLenS lensing measurements improve Planck CMB constraints on Omega(m) and sigma(8) by 26 per cent for flat I > cold dark matter. For a model with free curvature, the joint CFHTLenS-Planck result is Omega(m) = 0.28 +/- 0.02 (68 per cent confidence), which is an improvement of 43 per cent compared to Planck alone. We test how our results are potentially subject to three astrophysical sources of contamination: source-lens clustering, the intrinsic alignment of galaxy shapes, and baryonic effects. We explore future limitations of the cosmological use of third-order weak lensing, such as the non-linear model and the Gaussianity of the likelihood function.
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