Abstract
The late integrated Sachs-Wolfe (ISW) effect correlates the Cosmic Microwave Background (CMB) temperature anisotropies with foreground cosmic large-scale structures. As the correlation depends crucially on the growth history in the era of dark energy, it is a key observational probe for constraining the cosmological model. Here we present a detailed study based on full-sky and deep light cones generated from very large volume numerical N-body simulations, which allow us to avoid the use of standard replica techniques, while capturing the entirety of the late ISW effect on the large scales. We post-process the light cones using an accurate ray-tracing method and construct full-sky maps of the ISW temperature anisotropy for three different dark energy models. We quantify in detail the extent to which the ISW effect can be used to discriminate between different dark energy scenarios when cross-correlated with the matter distribution or the CMB lensing potential. We also investigate the onset of non-linearities, the so-called Rees-Sciama effect which provides a complementary probe of the dark sector. We find the signal of the lensing-lensing and ISW-lensing correlation of the three dark energy models to be consistent with measurements from the Planck satellite. Future surveys of the large-scale structures may provide cross-correlation measurements that are sufficiently precise to distinguish the signal of these models. Our methodology is very general and can be applied to any dark energy or modified gravity scenario as long as the metric seen by photons can still be characterized by a Weyl potential.
Highlights
In a flat Friedmann-Lemaître-Robertson-Walker (FLRW) universe, the presence of dark energy (DE) generates a distinct imprint on the cosmic microwave background radiation through the late integrated Sachs-Wolfe effect [1]
We present a detailed study based on full-sky and deep light cones generated from very large volume numerical N-body simulations, which allow us to avoid the use of standard replica techniques, while capturing the entirety of the late integrated Sachs-Wolfe (ISW) effect on the large scales
From the dependence of the signal on zÃ, we can see that the differences among the various model predictions correlate with the differences in the redshift evolution of the linear growth rate shown in Overall, we find a good agreement with the linear theory for multipoles l ≲ 50 where the linear ISW effect is expected to dominate over the nonlinear RS effect
Summary
In a flat Friedmann-Lemaître-Robertson-Walker (FLRW) universe, the presence of dark energy (DE) generates a distinct imprint on the cosmic microwave background radiation through the late integrated Sachs-Wolfe effect [1]. This effect originates in the decay of the gravitational potentials associated with large-scale structure whose growth rate is altered by the increasingly fast expansion driven by the DE component. CMB photons traveling through the structures gain a small energy variation that generates temperature anisotropies at large angular scales This is not the case in a matter dominated universe where the cosmic expansion exactly compensates the growth rate of structures, rendering the gravitational potentials constant in time. This signal needs to be disentangled from that of other effects contributing to the CMB
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