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We study the connection between active galactic nuclei (AGN) and their hostgalaxies through cosmic time in the large-scale cosmological IllustrisTNGsimulations. We first compare BH properties, i.e. the hard X-ray BH luminosityfunction, AGN galaxy occupation fraction, and distribution of Eddington ratios,to available observational constraints. The simulations produce a population ofBHs in good agreement with observations, but we note an excess of faint AGN inhard X-ray (L_x ~ 10^{43-44} erg/s), and a lower number of bright AGN(L_x>10^{44} erg/s), a conclusion that varies quantitatively but notqualitatively with BH luminosity estimation method. The lower Eddington ratiosof the 10^{9} Msun BHs compared to observations suggest that AGN feedback maybe too efficient in this regime. We study galaxy star formation activity andstructural properties, and design sample-dependent criteria to identifydifferent galaxy types (star-forming/quiescent, extended/compact) that we applyboth to the simulations and observations from the candels fields. We analyzehow the simulated and observed galaxies populate the specific star formationrate - stellar mass surface density diagram. A large fraction of the z=0M_{star}>10^{11} Msun quiescent galaxies first experienced a compaction phase(i.e. reduction of galaxy size) while still forming stars, and then a quenchingevent. We measure the dependence of AGN fraction on galaxies' locations in thisdiagram. After correcting the simulations with a redshift and AGNluminosity-dependent model for AGN obscuration, we find good qualitative andquantitative agreement with observations. The AGN fraction is the highest amongcompact star-forming galaxies (16-20% at z~1.5-2), and the lowest among compactquiescent galaxies (6-10% at z~1.5-2).

Linking galaxy structural properties and star formation activity to black hole activity with IllustrisTNG