Modeling Cosmological Evolution of Jetted Seyfert Galaxies for <i>z</i>  ≲ 10

Abstract We use high-resolution cosmological zoom-in simulations to model mechanical and thermal feedback from active galactic nuclei onto the evolution of Seyfert-type galaxies, studying the morphology of central galaxies growing within dark matter (DM) halos with masses log M / M ⊙ ∼ 11.8 at z = 0. In Paper I, we focused on the end products at z = 0; here, we analyze evolution for z ≲ 10. Black holes (SMBHs) of ∼10 6 M ⊙ were seeded at z ∼ 9.1 and z ∼ 3.7, producing jets along their spin axes. Obtained SMBH accretion rates vary in the range ∼0.3–10 −4 of the Eddington rate. We compared the basic properties of galaxies, such as star formation rate, masses, gas and stellar fractions, bulge-to-disk mass ratios, SMBH masses, etc., over the range of redshifts. Our results indicate that jets and associated overpressured bubbles have substantial effects on Seyfert galaxy evolution, including properties of the interstellar medium and circumgalactic medium (CGM), and even beyond. This feedback can suppress and even quench star formation, reduce stellar mass and gas fraction, modify the bulge-to-disk ratios, drive outflows from galaxies and host DM halos, and metal-enrich the CGM. The jets are largely but not exclusively contained within galaxies. However, overpressured bubbles cross and modify the composition of the CGM and intergalactic medium, their thermodynamic and dynamic state, and generate vorticity. The CGM emerges as a complex region, where the action of galactic outflows and jet-formed bubbles combines with the influx from cosmological filaments and diffuse accretion. Ultimately, the above processes affect the gas balance within the galaxy, its morphology, and gas supply to the SMBH, limiting its growth.