Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/6726
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dc.contributor.authorVidhya, G-
dc.contributor.authorPravabati, C-
dc.contributor.authorYogendran, K. P-
dc.contributor.authorPark, C-
dc.date.accessioned2020-11-10T02:28:42Z-
dc.date.available2020-11-10T02:28:42Z-
dc.date.issued2015-02-
dc.identifier.citationJournal of Cosmology and Astroparticle Physics, Vol. 2015, No. 2, 28en_US
dc.identifier.issn1475-7516-
dc.identifier.urihttp://prints.iiap.res.in/handle/2248/6726-
dc.descriptionRestricted Access © IOP Publishing http://dx.doi.org/10.1088/1475-7516/2015/02/028en_US
dc.description.abstractWe study the signatures of local type primordial non-Gaussianity, parametrized by fNL, of scalar perturbations in CMB polarization using the probability distribution functions, Minkowski Functionals and Betti numbers. We show that the lowest order non-Gaussian deviation of the PDF of the total polarization intensity is at order (fNLσ)2. We calculate the non-Gaussian deviations of Minkowski Functionals and Betti numbers from simulated polarization maps. If observational issues such as instrumental noise are ignored, we find that E mode polarization provides independent and equally strong constraint on fNL as temperature fluctuations. The constraint is expected to weaken when observational issues are included since the signal-to-noise ratio of polarization data is lower than that of temperature. The non-Gaussian signal in the total polarization intensity, however, is much weaker and has a relatively large cosmic variance and hence may not be useful for detecting local type non-Gaussianity.en_US
dc.language.isoenen_US
dc.publisherIOP Publishingen_US
dc.subjectNon-gaussianityen_US
dc.subjectCMBR polarization parametersen_US
dc.titlePrimordial non-Gaussian signatures in CMB polarizationen_US
dc.typeArticleen_US
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