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Weak lensing of the cosmic microwave background: Power spectrum covariance

Cooray, Asantha (2002) Weak lensing of the cosmic microwave background: Power spectrum covariance. Physical Review D, 65 (6). Art. No. 063512. ISSN 2470-0010.

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We discuss the non-Gaussian contribution to the power spectrum covariance of cosmic microwave background (CMB) anisotropies resulting through weak gravitational lensing angular deflections and the correlation of deflections with secondary sources of temperature fluctuations generated by the large scale structure, such as the integrated Sachs-Wolfe effect and the Sunyaev-Zel’dovich effect. This additional contribution to the covariance of binned angular power spectrum, beyond the well known cosmic variance and any associated instrumental noise, results from a trispectrum, or a four point correlation function, in temperature anisotropy data. With substantially wide bins in multipole space, the resulting non-Gaussian contribution from lensing to the binned power spectrum variance is insignificant out to multipoles of a few thousand and is not likely to affect the cosmological parameter estimation with acoustic peaks and the damping tail. The non-Gaussian contribution to covariance, however, should be considered when interpreting binned CMB power spectrum measurements at multipoles of a few thousand corresponding to angular scales of few arcminutes and less.

Item Type:Article
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Cooray, Asantha0000-0002-3892-0190
Additional Information:© 2002 The American Physical Society. Received 11 October 2001; published 28 February 2002. We acknowledge support from the Sherman Fairchild Foundation and from the U.S. DOE Grant No. DE-FG03-92-ER40701.
Funding AgencyGrant Number
Sherman Fairchild FoundationUNSPECIFIED
Department of Energy (DOE)DE-FG03-92-ER40701
Issue or Number:6
Record Number:CaltechAUTHORS:COOprd02e
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:10985
Deposited By: Archive Administrator
Deposited On:21 Jun 2008
Last Modified:03 Oct 2019 00:14

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