Abstract
ABSTRACT We present full-sky maps of the Integrated Sachs–Wolfe effect (ISW) for the MICE Grand Challenge lightcone simulation up to redshift 1.4. The maps are constructed in the linear regime using spherical Bessel transforms. We compare and contrast this procedure against analytical approximations found in the literature. By computing the ISW in the linear regime, we remove the substantial computing and storage resources required to calculate the non-linear Rees–Sciama effect. Since the linear ISW at low redshift z ≲ 1, at large angular scales, and after matter domination is ${\sim}10^{2}\, \mathrm{ times}$ larger in ΔT/T, this has a negligible impact on the maps produced and only becomes relevant on scales which are dominated by cosmic microwave background (CMB) anisotropies. The MICE simulation products have been extensively used for studies involving current and future galaxy surveys. The availability of these maps will allow MICE to be used for future galaxy and CMB cross-correlation studies, ISW reconstruction studies, and ISW void-stacking studies probed by galaxy surveys such as Dark Energy Survey, Dark Energy Spectroscopic Instrument, Euclid, and Rubin Legacy Survey of Space and Time. The pipeline developed in this study is provided as a public Python package pyGenISW. This could be used in the future studies for constructing the ISW from existing and future simulation suites probing vast sets of cosmological parameters and models.
Highlights
The Integrated Sachs–Wolfe effect (ISW; Sachs & Wolfe 1967), caused by the evolution of gravitational potentials in large-scale structure (LSS), imprints features on to the cosmic microwave background (CMB)
The paper is organized as follows: in Section 2 we describe the MICE simulation data used and the ISW construction methods implemented in this study; in Section 3 we compare the ISW maps and their statistics to each other, and theoretical expectations; lastly, in Section 4 we discuss the results and the relevance of the data and pipeline produced in this study for future work
The full-sky MICE ISW map for contributions in the range 0 ≤ z ≤ 1.4 is shown in Fig. 1 using the spherical Bessel transform (SBT) with normal boundary conditions
Summary
The Integrated Sachs–Wolfe effect (ISW; Sachs & Wolfe 1967), caused by the evolution of gravitational potentials in large-scale structure (LSS), imprints features on to the cosmic microwave background (CMB). This has been performed on several galaxy surveys to constrain the standard cosmological model cold dark matter ( CDM) and to test expanded or alternative models In order to understand the observational sensitivities and systematics of the ISW to cosmological parameters, we need to be able to construct ISW maps and corresponding galaxy mocks for a wide range of cosmological parameters and models At present, this is computationally expensive as accurate ISW maps require regular snapshots of the gravitational potential. For this reason only a handful of such simulations exist (see Cai et al 2010; Watson et al 2014; Carbone, Petkova & Dolag 2016; Adamek et al 2020) using either the best-fitting Planck cosmology or exploring a limited set of cosmological parameters or models
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