Boxy H$α$ Emission Profiles in Star-Forming Galaxies

We assemble a sample of disk star-forming galaxies from the Sloan Digital Sky Survey Data Release 7, studying the structure of H$α$ emission lines, finding a large fraction of this sample contains boxy H$α$ line profiles. This fraction depends on galaxy physical and geometric parameters in the following way: (1) it increases monotonically with star formation rate per unit area ($Σ_{\rm SFR}$), and stellar mass ($M_*$), with the trend being much stronger with $M_*$, from $\sim$0% at $M_*=10^{10}M_{\odot}$ to about 50% at $M_*=10^{11}M_\odot$; (2) the fraction is much smaller in face-on systems than in edge-on systems. It increases with galaxy inclination ($i$) while $i < 60\,^{\circ}$ and is roughly a constant of 25% beyond this range; (3) for the sources which can be modeled well with two velocity components, blueshifted and redshifted from the systemic velocity, these is a positive correlation between the velocity difference of these two components and the stellar mass, with a slope similar to the Tully-Fisher relation; (4) the two components are very symmetric in the mean, both in velocity and in amplitude. The four findings listed above can be understood as a natural result of a rotating galaxy disk with a kpc-scale ring-like H$α$ emission region.

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