The structure of disc galaxies

The bars, spiral arms and outer disc breaks


Bars and central star formation

In this paper, we found that the fraction of galaxies hosting bars tend to be highest, when the galaxies have either significant enhanced central star formation, or strongly suppressed central star formation. It suggests that bars may play role in the quenching of central star formation, or mechanisms that quenched the star formation also enhanced the formation or maintenance of bars.

In this paper, we found that, at least in the highly disk-dominated barred galaxies, the strengths of spiral arms are likely the key parameter that determines whether the barred galaxies have centrally enhanced or suppressed SFR.

Bulge and disk

The growth of bulges and discs with HI

This paper find that at fixed stellar mass, disc colours are correlated with the HI mass fraction, while bulge colours are not. The lack of a correlation between the bulge colour and the Hi mass fraction is regardless whether the bulges are pseudo, or whether the galaxies host bars or are interacting with a neighbour. There is no strong correlation between the colours of the discs and bulges either. These results suggest that the current total amount of Hi is closely related to the formation of discs, but does not necessarily fuel the formation of (pseudo) bulges in an efficient way.

Disc breaks

Up-bending breaks and gas accretion

This paper found that HI-rich and low-spin galaxies tend to have high fraction of hosting up-bending (type III) outer discs (~75%), which is significantly higher than control galaxies. The high and excess type III fraction is independent of the existence of strong bars and environment. The result supports the in-situ star formation fueld by gas accretion to be an important way of building the up-bending outer discs.