Quenching time-scales in the IllustrisTNG simulation

ABSTRACT The time-scales for galaxy quenching offer clues to its underlying physical drivers. We investigate central in the IllustrisTNG 100-1 simulation, their evolution over time, and pre-quenching properties of galaxies that predict time-scales. Defining duration ?q as time between crossing specific star formation rate (sSFR) thresholds, we find ${\sim} 40{{\ \rm per\ cent}}$ quench rapidly with < 1 Gyr, but a substantial tail can take up 10 Gyr quench. Furthermore, 29 per cent left star-forming main sequence (SFMS) more than 2 ago never fully by z = 0. While median is fairly constant epoch, leaving SFMS increases steadily cosmic slow quenchers being dominant around ? 2–0.7. Compared fast (?q Gyr), slow-quenching > Gyr) were massive, had massive black holes, larger stellar radii, accreted gas higher angular momentum (AM) prior quenching. These evolve little 0, except accreting AM quenchers, which reaches same high quenchers. By also have residual extended rings. Using expected relationship age gradient inside-out agreement Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) integral field unit (IFU) observations. Our results suggest potential well depth determine time-scale.