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Parameter estimation biases due to contributions from the Rees-Sciama effect to the integrated Sachs-Wolfe spectrum

Schäfer, Björn Malte ; Kalovidouris, Angelos Fotios ; Heisenberg, Lavinia

In: Monthly Notices of the Royal Astronomical Society, 2011, vol. 416, no. 2, p. 1302-1310

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    Titre
    • Parameter estimation biases due to contributions from the Rees-Sciama effect to the integrated Sachs-Wolfe spectrum
    Auteur
    • Schäfer, Björn Malte. Institut d'Astrophysique Spatiale, Université Paris XI, bâtiment 120-121, Centre universitaire d'Orsay, 91440 Orsay Cedex, France
    • Kalovidouris, Angelos Fotios. Astronomisches Recheninstitut, Zentrum für Astronomie, Universität Heidelberg, Mönchhofstraße 12, 69120 Heidelberg, Germany
    • Heisenberg, Lavinia. Institut für theoretische Astrophysik, Zentrum für Astronomie, Universität Heidelberg, Albert-Ueberle-Straße 2, 69120 Heidelberg, Germany
    Type de document
    • Postprint
    Langue
    • Anglais
    Publié dans
    • Monthly Notices of the Royal Astronomical Society, 2011, vol. 416, no. 2, p. 1302-1310. Blackwell Publishing Ltd
    Autre version électronique
    Identifiant OAI-PMH
    • oai:doc.rero.ch:303629
    Summary
    The subject of this paper is an investigation of the non-linear contributions to the spectrum of the integrated Sachs-Wolfe (iSW) effect. We derive the corrections to the iSW autospectrum and the iSW-tracer cross-spectrum consistently to third order in perturbation theory and analyse the cumulative signal-to-noise ratio for a cross-correlation between the Planck and Euclid data sets as a function of multipole order. We quantify the parameter sensitivity and the statistical error bounds on the cosmological parameters Ωm, σ8, h, ns and w from the linear iSW effect and the systematical parameter estimation bias due to the non-linear corrections in a Fisher formalism, analysing the error budget in its dependence on multipole order. Our results include the following: (i) the spectrum of the non-linear iSW effect can be measured with 0.8σ statistical significance, (ii) non-linear corrections dominate the spectrum starting from ℓ≃ 102, (iii) an anticorrelation of the CMB temperature with tracer density on high multipoles in the non-linear regime, (iv) a much weaker dependence of the non-linear effect on the dark energy model compared to the linear iSW effect and (v) parameter estimation biases amount to less than 0.1σ and weaker than other systematics