The impact of feedback and cosmology on Cosmic Infrared Background cross-correlations

We study the evolution and clustering properties of the star formation rate density (SFR) ${\rho }_{\mathrm{S}\mathrm{F}\mathrm{R}}$ in the FLAMINGO suite of hydrodynamical simulations, with the aim of exploring the possibility of constraining AGN and stellar feedback prescription, as well as the effect of cosmology, using cross-correlations between the Cosmic Infrared Background (CIB) and other tracers of the large-scale structure. Specifically, we consider tomographic measurements of the bias-weighted SFR-density $⟨b{\rho }_{\mathrm{S}\mathrm{F}\mathrm{R}}⟩$, as well as cross-correlations between the CIB and cosmic shear as a probe of the ${\rho }_{\mathrm{S}\mathrm{F}\mathrm{R}}$-matter correlation. Most of the FLAMINGO models calibrated against the $z=0$ galaxy stellar mass function (SMF) yield similar predictions for the distribution and clustering of star-forming systems, and thus it is difficult to derive clean conclusions regarding the impact of AGN feedback or cosmology on CIB statistics. However, we show that current measurements of $⟨b{\rho }_{\mathrm{S}\mathrm{F}\mathrm{R}}⟩$, as well as CIB-shear cross-correlations clearly disfavour models with strong stellar feedback, as well as simulations with strong kinetic (jet-driven) AGN feedback, even under the fiducial SMF calibration. This study demonstrates the potential of CIB cross-correlations to study aspects of the physics of star and galaxy formation in a cosmological setting.