2012
DOI: 10.1111/j.1365-2966.2012.21125.x
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Integrated Sachs-Wolfe tomography with orthogonal polynomials

Abstract: Topic of this article are tomographic measurements of the integrated Sachs-Wolfe effect with specifically designed, orthogonal polynomials which project out statistically independent modes of the galaxy distribution. The polynomials are contructed using the Gram-Schmidt orthogonalisation method. To quantify the power of the iSW-effect in contraining cosmological parameters we perfom a combined Fisher matrix analysis for the iSW-, galaxy- and cross-spectra for wCDM cosmologies using the survey characteristics o… Show more

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Cited by 4 publications
(2 citation statements)
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“…We show how information from both effects can be combined in a single formalism, tying into the three-dimensional treatment of weak lensing. The 3d-method presented here combines iSW-lensing correlations (Nishizawa et al 2008;Lee 2015) in a redshift-resolved way, improving over tomographic methods (Ho et al 2008;Jürgens & Schäfer 2012).…”
Section: Introductionmentioning
confidence: 99%
“…We show how information from both effects can be combined in a single formalism, tying into the three-dimensional treatment of weak lensing. The 3d-method presented here combines iSW-lensing correlations (Nishizawa et al 2008;Lee 2015) in a redshift-resolved way, improving over tomographic methods (Ho et al 2008;Jürgens & Schäfer 2012).…”
Section: Introductionmentioning
confidence: 99%
“…Although one might naively think that statistically independent measurements should be best at constraining a model, it is rather the fact that the additional information in the crosscorrelation with its parameter constraining power is advantageous to exploit: Firstly, on large scales there is a non-vanishing correlation of observed galaxy shapes and the CMB temperature due to the integrated Sachs Wolfe (iSW) effect, which has been investigated in a three-dimensional analysis by Zieser & Merkel (2016), as a generalization of tomographic measurements (e.g. Ho et al 2008;Jürgens & Schäfer 2012). Secondly, both weak lensing of the CMB and of galaxies are caused by the very same large scale structure.…”
mentioning
confidence: 99%