The Stellar Mass Tully-Fisher Relation to z = 1.2 from AEGIS

We combine newly measured rotation velocities, velocity dispersions, and stellar masses to construct stellar mass Tully-Fisher relations (M sub(*)TFRs) for 544 galaxies with strong emission lines at 0.1 z 1.2 from the All-Wavelength Extended Groth Strip International Survey (AEGIS) and the Deep Extragalactic Evolutionary Probe 2 (DEEP2) survey. The conventional M sub(*)TFR using only rotation velocity (V sub(rot)) shows large scatter (61.5 dex in velocity). The scatter and residuals are correlated with morphology in the sense that disturbed, compact, and major merger galaxies have lower velocities for their masses. We construct an M sub(*)TFR using the kinematic estimator S sub(0.5), which is defined as (0.5V super(2) sub(rot) + s super(2) sub(g)) super(1/2) and accounts for disordered or noncircular motions through the gas velocity dispersion (s sub(g)). The new M sub(*)TFR, termed S sub(0.5)/M sub(*)TFR, is remarkably tight over 0.1 < z < 1.2, with no detectable evolution of its intercept or slope with redshift. The average best-fit relation has 0.47 dex scatter in stellar mass, corresponding to 61.2 "magnitudes," assuming a constant mass-to-light ratio. Interestingly, the S sub(0.5)/M sub(*)TFR is consistent with the absorption-line-based stellar mass Faber-Jackson relation for nearby elliptical galaxies in terms of slope and intercept, which might suggest a physical connection between the two relations.