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hal.structure.identifierInstitut d'Astrophysique de Paris [IAP]
dc.contributor.authorKilbinger, Martin*
hal.structure.identifierInstitut d'Astrophysique de Paris [IAP]
dc.contributor.authorBenabed, Karim*
hal.structure.identifierLaboratoire de Physique Nucléaire et de Hautes Énergies [LPNHE (UMR_7585)]
dc.contributor.authorGuy, J.*
hal.structure.identifierLaboratoire de Physique Nucléaire et de Hautes Énergies [LPNHE (UMR_7585)]
dc.contributor.authorAstier, P.*
hal.structure.identifierInstitut d'Astrophysique de Paris [IAP]
dc.contributor.authorTereno, I.*
hal.structure.identifierInstitut d'Astrophysique de Paris [IAP]
hal.structure.identifier
dc.contributor.authorFu, Liangliang*
hal.structure.identifierInstitut d'Astrophysique de Paris [IAP]
hal.structure.identifierCEntre de REcherches en MAthématiques de la DEcision [CEREMADE]
dc.contributor.authorWraith, Darren*
hal.structure.identifierInstitut d'Astrophysique de Paris [IAP]
dc.contributor.authorCoupon, J.*
hal.structure.identifierInstitut d'Astrophysique de Paris [IAP]
dc.contributor.authorMellier, Y.*
hal.structure.identifierLaboratoire de Physique Nucléaire et de Hautes Énergies [LPNHE (UMR_7585)]
dc.contributor.authorBalland, C.
HAL ID: 19982
ORCID: 0000-0002-3487-7308
*
hal.structure.identifierInstitut d'Astrophysique de Paris [IAP]
dc.contributor.authorBouchet, F.R.
HAL ID: 21788
ORCID: 0000-0002-4040-2253
*
hal.structure.identifier
dc.contributor.authorHamana, T.*
hal.structure.identifier
dc.contributor.authorHardin, D.*
hal.structure.identifier
dc.contributor.authorMcCracken, H.J.*
hal.structure.identifier
dc.contributor.authorPain, R.
HAL ID: 742459
ORCID: 0000-0003-4016-6067
*
hal.structure.identifier
dc.contributor.authorRegnault, N.*
hal.structure.identifier
dc.contributor.authorSchultheis, M.*
hal.structure.identifier
dc.contributor.authorYahagi, H.*
dc.date.accessioned2014-02-11T15:05:29Z
dc.date.available2014-02-11T15:05:29Z
dc.date.issued2009
dc.identifier.urihttps://basepub.dauphine.fr/handle/123456789/12637
dc.language.isoenen
dc.subjectcosmology: observationsen
dc.subjectcosmology: cosmological parametersen
dc.subjectmethods: statisticalen
dc.subject.ddc520en
dc.titleDark energy constraints and correlations with systematics from CFHTLS weak lensing, SNLS supernovae Ia and WMAP5en
dc.typeArticle accepté pour publication ou publié
dc.description.abstractenAims. We combine measurements of weak gravitational lensing from the CFHTLS-Wide survey, supernovae Ia from CFHT SNLS and CMB anisotropies from WMAP5 to obtain joint constraints on cosmological parameters, in particular, the dark-energy equation-of-state parameter w. We assess the influence of systematics in the data on the results and look for possible correlations with cosmological parameters. Methods. We implemented an MCMC algorithm to sample the parameter space of a flat CDM model with a dark-energy component of constant w. Systematics in the data are parametrised and included in the analysis. We determine the influence of photometric calibration of SNIa data on cosmological results by calculating the response of the distance modulus to photometric zero-point variations. The weak lensing data set is tested for anomalous field-to-field variations and a systematic shape measurement bias for high-redshift galaxies. Results. Ignoring photometric uncertainties for SNLS biases cosmological parameters by at most 20% of the statistical errors, using supernovae alone; the parameter uncertainties are underestimated by 10%. The weak-lensing field-to-field variance between 1 deg2-MegaCam pointings is 5-15% higher than predicted from N-body simulations. We find no bias in the lensing signal at high redshift, within the framework of a simple model, and marginalising over cosmological parameters. Assuming a systematic underestimation of the lensing signal, the normalisation $\sigma_8$ increases by up to 8%. Combining all three probes we obtain -0.10 < 1 + w < 0.06 at 68% confidence ( -0.18 < 1 + w < 0.12 at 95%), including systematic errors. Our results are therefore consistent with the cosmological constant $\Lambda$. Systematics in the data increase the error bars by up to 35%; the best-fit values change by less than 0.15$\sigma$.en
dc.relation.isversionofjnlnameAstronomy & Astrophysics
dc.relation.isversionofjnlvol497en
dc.relation.isversionofjnlissue3en
dc.relation.isversionofjnldate2009
dc.relation.isversionofjnlpages677-688en
dc.relation.isversionofdoihttp://dx.doi.org/10.1051/0004-6361/200811247en
dc.identifier.urlsitehttp://arxiv.org/abs/0810.5129v2en
dc.relation.isversionofjnlpublisherEDP Sciencesen
dc.subject.ddclabelSciences connexes (physique, astrophysique)en
dc.relation.forthcomingnonen
dc.relation.forthcomingprintnonen
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