Integrated Sachs-Wolfe tomography with orthogonal polynomials
  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 of PLANCK
and EUCLID. The signal to noise ratio has also been studied for other
contemporary galaxy surveys, such as SDSS, NVSS and 2MASS. For the
cross-spectra our tomographic method provides a 16% increase in the signal to
noise ratio and an improvement of up to 30% in conditional errors on
parameters. Including all spectra, the marginalised errors approach an inverse
square-root dependence with increasing cumulative polynomial order which
underlines the statistical independence of the weighted signal spectra.
