New Lessons from the HI Size-Mass Relation of Galaxies

Abstract

We revisit the HI size-mass (D${}_{\mathrm{HI}}$-M${}_{\mathrm{HI}}$) relation of galaxies with a sample of more than 500 nearby galaxies covering over five orders of magnitude in HI mass and more than ten $B$-band magnitudes. The relation is remarkably tight with a scatter $\sigma \sim$0.06 dex, or 14%. The scatter does not change as a function of galaxy luminosity, HI richness or morphological type. The relation is linked to the fact that dwarf and spiral galaxies have a homogenous radial profile of HI surface density in the outer regions when the radius is normalised by D${}_{\mathrm{HI}}$. The early-type disk galaxies typically have shallower HI radial profiles, indicating a different gas accretion history. We argue that the process of atomic-to-molecular gas conversion or star formation cannot explain the tightness of the D${}_{\mathrm{HI}}$-M${}_{\mathrm{HI}}$ relation. This simple relation puts strong constraints on simulation models for galaxy formation.

9 pages, 6 figures, accepted for publication at MNRAS

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