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dc.contributor.authorKilbinger, Martin
dc.contributor.authorWraith, Darren
dc.contributor.authorRobert, Christian P.
dc.contributor.authorBenabed, Karim
dc.contributor.authorCappé, Olivier
HAL ID: 1534
ORCID: 0000-0001-7415-8669
dc.contributor.authorCardoso, Jean-François
HAL ID: 742037
ORCID: 0000-0002-3388-6608
dc.contributor.authorFort, Gersende
HAL ID: 739303
ORCID: 0000-0001-5400-1058
dc.contributor.authorPrunet, Simon
HAL ID: 739461
ORCID: 0000-0002-1755-4582
dc.contributor.authorBouchet, François R.
HAL ID: 180816
ORCID: 0000-0002-8051-2924
dc.date.accessioned2011-10-12T13:52:17Z
dc.date.available2011-10-12T13:52:17Z
dc.date.issued2010
dc.identifier.urihttps://basepub.dauphine.fr/handle/123456789/7196
dc.language.isoenen
dc.subjectmethods: statisticalen
dc.subjectcosmological parametersen
dc.subject.ddc519en
dc.titleBayesian model comparison in cosmology with Population Monte Carloen
dc.typeArticle accepté pour publication ou publié
dc.description.abstractenWe use Bayesian model selection techniques to test extensions of the standard flat Λ cold dark matter (ΛCDM) paradigm. Dark-energy and curvature scenarios, and primordial perturbation models are considered. To that end, we calculate the Bayesian evidence in favour of each model using Population Monte Carlo (PMC), a new adaptive sampling technique which was recently applied in a cosmological context. In contrast to the case of other sampling-based inference techniques such as Markov chain Monte Carlo (MCMC), the Bayesian evidence is immediately available from the PMC sample used for parameter estimation without further computational effort, and it comes with an associated error evaluation. Also, it provides an unbiased estimator of the evidence after any fixed number of iterations and it is naturally parallelizable, in contrast with MCMC and nested sampling methods. By comparison with analytical predictions for simulated data, we show that our results obtained with PMC are reliable and robust. The variability in the evidence evaluation and the stability for various cases are estimated both from simulations and from data. For the cases we consider, the log-evidence is calculated with a precision of better than 0.08. Using a combined set of recent cosmic microwave background, type Ia supernovae and baryonic acoustic oscillation data, we find inconclusive evidence between flat ΛCDM and simple dark-energy models. A curved universe is moderately to strongly disfavoured with respect to a flat cosmology. Using physically well-motivated priors within the slow-roll approximation of inflation, we find a weak preference for a running spectral index. A Harrison–Zel'dovich spectrum is weakly disfavoured. With the current data, tensor modes are not detected; the large prior volume on the tensor-to-scalar ratio r results in moderate evidence in favour of r= 0.en
dc.relation.isversionofjnlnameMonthly Notices of the Royal Astronomical Society
dc.relation.isversionofjnlvol405en
dc.relation.isversionofjnlissue4en
dc.relation.isversionofjnldate2010
dc.relation.isversionofjnlpages2381-2390en
dc.relation.isversionofdoihttp://dx.doi.org/10.1111/j.1365-2966.2010.16605.xen
dc.identifier.urlsitehttp://arxiv.org/abs/0912.1614v2en
dc.description.sponsorshipprivateouien
dc.relation.isversionofjnlpublisherWileyen
dc.subject.ddclabelProbabilités et mathématiques appliquéesen


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