  We use the Simba suite of cosmological hydrodynamical simulations to
investigate the importance of various stellar and AGN feedback mechanisms in
partitioning the cosmic baryons between the intergalactic (IGM) and
circumgalactic (CGM) media in the $z\leq 1$ Universe. We identify the AGN jets
as the most prominent mechanism for the redistribution of baryons between the
IGM and CGM. In contrast to the full feedback models, deactivating AGN jets
results in $\approx20$ per cent drop in fraction of baryons residing in the IGM
and a consequent increase of CGM baryon fraction by $\approx 50$ per cent. We
find that stellar feedback modifies the partition of baryons on a $10$ per cent
level. We further examine the physical properties of simulated haloes in
different mass bins, and their response to various feedback models. On average,
a sixfold decrease in the CGM mass fraction due to the inclusion of feedback
from AGN jets is detected in $10^{12}M_{\odot} \leq M_{\rm 200} \leq
10^{14}M_{\odot}$ haloes. Examination of the average radial gas density
profiles of $M_{200} > 10^{12}M_{\odot}$ haloes reveals up to an order of
magnitude decrease in gas densities due to the AGN jet feedback. We compare gas
density profiles from Simba simulations to the predictions of the modified NFW
model, and show that the latter provides a reasonable approximation within the
virial radii of the full range of halo masses, but only when rescaled by the
appropriate mass-dependent CGM fraction of the halo. The relative partitioning
of cosmic baryons and, subsequently, the feedback models can be constrained
observationally with fast radio bursts (FRBs) in upcoming surveys.
