  We make an in-depth analysis of different AGN jet models' signatures,
inducing quiescence in galaxies with a halo mass of $10^{12} M_\odot$. Three
jet models, including cosmic ray-dominant, hot thermal, and precessing kinetic
jets, are studied at two energy flux levels each, compared to a jet-free,
stellar feedback-only simulation. We examine the distribution of Mg II, O VI,
and O VIII ions, alongside gas temperature and density profiles. Low-energy
ions, like Mg II, concentrate in the ISM, while higher energy ions, e.g., O
VIII, prevail at the AGN jet cocoon's edge. High-energy flux jets display an
isotropic ion distribution with lower overall density. High-energy thermal or
cosmic ray jets pressurize at smaller radii, significantly suppressing core
density. The cosmic ray jet provides extra pressure support, extending cool and
warm gas distribution. A break in the ion-to-mass ratio slope in O VI and O
VIII is demonstrated in the ISM-to-CGM transition (between 10-30 kpc), growing
smoothly towards the CGM at greater distances.
