Speaker
Description
We investigate the formation history of massive disc galaxies in hydrodynamical simulation -- the IllustrisTNG, to study why massive disc galaxies survive through cosmic time. 83 galaxies in the simulation are selected with M$_{*,z=0}$ $>8\times10^{10}$ \Msun and kinematic bulge-to-total ratio less than $0.3$. We find that 8.4 percent of these massive disc galaxies have quiet merger histories and preserve disc morphology since formed. 54.2 percent have a significant increase in bulge components in history, then become discs again till present time. The rest 37.3 percent experience prominent mergers but survive to remain discy. While mergers and even major mergers do not always turn disc galaxies into ellipticals, we study the relations between various properties of mergers and the morphology of merger remnants. We find a strong dependence of remnant morphology on the orbit type of major mergers. Specifically, major mergers with a spiral-in falling orbit mostly lead to disc-dominant remnants, and major mergers of head-on galaxy-galaxy collision mostly form ellipticals. This dependence of remnant morphology on orbit type is much stronger than the dependence on cold gas fraction or orbital configuration of merger system as previously studied.
