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Article: Constraining a spatially dependent rotation of the cosmic microwave background polarization
Title  Constraining a spatially dependent rotation of the cosmic microwave background polarization 

Authors  
Issue Date  2009 
Citation  Physical Review D  Particles, Fields, Gravitation and Cosmology, 2009, v. 79, n. 12 How to Cite? 
Abstract  Following Kamionkowski (2008), a quadratic estimator of the rotation of the plane of polarization of the cosmic microwave background (CMB) is constructed. This statistic can estimate a spatially varying rotation angle α(n). We use this estimator to quantify the prospects of detecting such a rotation field with forthcoming experiments. For PLANCK and CMBPol experiments, we find that the estimator containing the product of the E and B components of the polarization field is the most sensitive. The variance of this EB estimator N(L) is roughly independent of the multipole L and is only weakly dependent on the instrumental beam. For FWHM of the beam size Θfwhm∼5′50′ and instrument noise Δp∼550μKarcmin, the scaling of variance N(L) can be fitted by a power law N(L)=3.3×107Δp2Θfwhm1.3deg 2. For small instrumental noise Δp≤5μKarcmin, the lensing B modes become important, saturating the variance to ∼106deg 2 even for an ideal experiment. Upcoming experiments like PLANCK will be able to detect a power spectrum of the rotation angle, Cαα(L), as small as 0.01deg 2, while futuristic experiments like CMBPol will be able to detect rotation angle power spectrum as small as 2.5×105deg 2. We discuss the implications of such constraints, both for the various physical effects that can rotate the polarization as photons travel from the last scattering surface as well as for constraints on instrumental systematics that can also lead to a spurious rotation signal. Rotation of the CMB polarization generates B modes which will act as contamination for the primordial Bmode detection. We discuss an application of our estimator to derotate the CMB to increase the sensitivity for the primordial B modes. © 2009 The American Physical Society. 
Persistent Identifier  http://hdl.handle.net/10722/226687 
ISSN  2014 Impact Factor: 4.643 2015 SCImago Journal Rankings: 1.882 
DC Field  Value  Language 

dc.contributor.author  Yadav, Amit P S   
dc.contributor.author  Biswas, Rahul   
dc.contributor.author  Su, Meng   
dc.contributor.author  Zaldarriaga, Matias   
dc.date.accessioned  20160629T01:58:18Z   
dc.date.available  20160629T01:58:18Z   
dc.date.issued  2009   
dc.identifier.citation  Physical Review D  Particles, Fields, Gravitation and Cosmology, 2009, v. 79, n. 12   
dc.identifier.issn  15507998   
dc.identifier.uri  http://hdl.handle.net/10722/226687   
dc.description.abstract  Following Kamionkowski (2008), a quadratic estimator of the rotation of the plane of polarization of the cosmic microwave background (CMB) is constructed. This statistic can estimate a spatially varying rotation angle α(n). We use this estimator to quantify the prospects of detecting such a rotation field with forthcoming experiments. For PLANCK and CMBPol experiments, we find that the estimator containing the product of the E and B components of the polarization field is the most sensitive. The variance of this EB estimator N(L) is roughly independent of the multipole L and is only weakly dependent on the instrumental beam. For FWHM of the beam size Θfwhm∼5′50′ and instrument noise Δp∼550μKarcmin, the scaling of variance N(L) can be fitted by a power law N(L)=3.3×107Δp2Θfwhm1.3deg 2. For small instrumental noise Δp≤5μKarcmin, the lensing B modes become important, saturating the variance to ∼106deg 2 even for an ideal experiment. Upcoming experiments like PLANCK will be able to detect a power spectrum of the rotation angle, Cαα(L), as small as 0.01deg 2, while futuristic experiments like CMBPol will be able to detect rotation angle power spectrum as small as 2.5×105deg 2. We discuss the implications of such constraints, both for the various physical effects that can rotate the polarization as photons travel from the last scattering surface as well as for constraints on instrumental systematics that can also lead to a spurious rotation signal. Rotation of the CMB polarization generates B modes which will act as contamination for the primordial Bmode detection. We discuss an application of our estimator to derotate the CMB to increase the sensitivity for the primordial B modes. © 2009 The American Physical Society.   
dc.language  eng   
dc.relation.ispartof  Physical Review D  Particles, Fields, Gravitation and Cosmology   
dc.title  Constraining a spatially dependent rotation of the cosmic microwave background polarization   
dc.type  Article   
dc.description.nature  Link_to_subscribed_fulltext   
dc.identifier.doi  10.1103/PhysRevD.79.123009   
dc.identifier.scopus  eid_2s2.067649870089   
dc.identifier.volume  79   
dc.identifier.issue  12   
dc.identifier.spage  null   
dc.identifier.epage  null   
dc.identifier.eissn  15502368   