Abstract
As of today, the cross-correlation of galaxy surveys with the CMB, extensively discussed in the previous chapter, is still considered as the standard way to probe the iSW effect.
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- 1.
This is true as far as we can discern for now, since the current constraints on the presence of primordial non-Gaussianities in the CMB are compatible with zero (see [16]).
- 2.
Which is quite expected from the nature of the CMB fluctuations.
- 3.
To be more precise, in order to bring the maps to a common resolution we need to smooth each one of them by a Gaussian kernel with a FWHM equal to \(\sqrt{30'^2-R^2}\) with \(R\) the original resolution of the considered map.
- 4.
This was done in anticipation of a potentially large scale of the stacked signal, especially in the light of the “non-rescaled” results from the Gr08 clusters in Sect. 3.2.3.
- 5.
It should be noted that these results differ slightly from those reported my published paper [10], the reason being that I made a mistake in the calculation of the physical radius of the Gr08 voids (by a factor of \(\sim \)0.7). The purple points in Fig. 3.13 were affected as well. This does not alter fundamentally my conclusions and I intend to submit an erratum to the editor of the paper very shortly.
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Ilić, S. (2014). The Impact of Identified Superstructures in the CMB. In: The Large Scale Structures. Springer Theses. Springer, Cham. https://doi.org/10.1007/978-3-319-07746-8_3
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