A Transition Mass in the Local Tully-Fisher Relation

Abstract

We study the stellar mass Tully-Fisher relation (TFR, stellar mass versus rotation velocity) for a morphologically blind selection of emission line galaxies in the field at redshifts 0.1 $<$ z $<$ 0.375. Kinematics (${\sigma }_g$, V${}_{rot}$) are measured from emission lines in Keck/DEIMOS spectra and quantitative morphology is measured from V- and I-band Hubble images. We find a transition stellar mass in the TFR, $\log$ M${}_{\ast }$ = 9.5 M${}_{\odot }$. Above this mass, nearly all galaxies are rotation-dominated, on average more morphologically disk-like according to quantitative morphology, and lie on a relatively tight TFR. Below this mass, the TFR has significant scatter to low rotation velocity and galaxies can either be rotation-dominated disks on the TFR or asymmetric or compact galaxies which scatter off. We refer to this transition mass as the "mass of disk formation", M${}_{\mathrm{df}}$ because above it all star-forming galaxies form disks (except for a small number of major mergers and highly star-forming systems), whereas below it a galaxy may or may not form a disk.

Accepted to MNRAS. 14 pages, 7 figures

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