  We investigate the role of the Simba feedback model on the structure of the
Intra-Group Medium (IGrM) in the new Hyenas suite of cutting-edge cosmological
zoom-in simulations. Using 34 high-resolution zooms of halos spanning from
$10^{13}-10^{14}$ $M_\odot$ at $z=0.286$, we follow halos for 700 Myr, over
several major active galactic nuclei (AGN) jet feedback events. We use the
MOXHA package to generate mock Chandra X-ray observations, as well as
predictive mocks for the upcoming LEM mission, identifying many
feedback-generated features such as cavities, shock-fronts, and hot-spots,
closely mimicking real observations. Our sample comprises $105$ snapshots with
identified cavities, $50$ with single bubbles and $55$ with two, and spans
three orders of magnitude in observed cavity enthalpies, from $10^{41}-10^{44}$
erg/s. Comparing semi-major axis length, midpoint radius, and eccentricity to a
matched sample of observations, we find good agreement in cavity dimensions
with real catalogues. We estimate cavity power from our mock maps following
observational procedures, showing that this is typically more than enough to
offset halo cooling, particularly in low-mass halos, where we match the
observed excess in energy relative to cooling. Bubble enthalpy as measured with
the usual midpoint pressure typically exceeds the energy released by the most
recent jet event, hinting that the mechanical work is done predominantly at a
lower pressure against the IGrM. We demonstrate for the first time that X-ray
cavities are observable in a modern large-scale simulation suite and discuss
the use of realistic cavity mock observations as new halo-scale constraints on
feedback models in cosmological simulations.
