Feedback from active galactic nuclei (AGN) plays a critical role in shaping
the matter distribution on scales comparable to and larger than individual
galaxies. Upcoming surveys such as
Euclid and LSST aim to precisely
quantify the matter distribution on cosmological scales, making a detailed
understanding of AGN feedback effects essential. Hydrodynamical simulations
provide an informative framework for studying these effects, in particular by
allowing us to vary the parameters that determine the strength of these
feedback processes and, consequently, to predict their corresponding impact on
the large-scale matter distribution. We use the EAGLE simulations to explore
how changes in subgrid viscosity and AGN heating temperature affect the matter
distribution, quantified via 2- and 3-point correlation functions, as well as
higher order cumulants of the matter distribution. We find that varying
viscosity has a small impact (
≈10%) on scales larger than
1h−1
Mpc, while changes to the AGN heating temperature lead to substantial
differences, with up to
70% variation in gas clustering on small scales
(
≲1h−1 Mpc). By examining the suppression of the power spectrum
as a function of time, we identify the redshift range
z=1.5−1 as a key
epoch where AGN feedback begins to dominate in these simulations. The 3-point
function provides complementary insight to the more familiar 2-point
statistics, and shows more pronounced variations between models on the scale of
individual haloes. On the other hand, we find that effects on even larger
scales are largely comparable.