Higher resolution figure for Kassin et al. 2007, astro-ph/0702643:

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

Caption: The S_0.5 and Vrot stellar mass Tully-Fisher relations (M*TFRs) for 0.1 < z < 1.2 in bins of z. Galaxies are plotted as different symbols according to their quantitative morphologies, and if a morphology is unobtainable, it is placed into the `none' category. Symbols are outlined in black if the galaxies were considered to be disturbed or compact via a separate visual classification. If Vrot is not inclination corrected, open symbols are used; all galaxies in the `none'category are inclination-corrected as their symbol does not have an open form. Using S_0.5, which combines the dynamical support from ordered motion with that from disordered motions, results in an M*TFR that is much tighter and non-evolving to z=1.2. For S_0.5, a fit to data in the lowest z bin is plotted as a solid line that is repeated in the other z bins as dashed lines. Fits are labeled in each box, where "a" is the intercept at 10^10 solar masses, "b" the slope, "c" the intrinsic scatter in S_0.5, and "rms" the rms scatter in S_0.5. In the lowest z bin for Vrot, the M*TFRs from local and z~1 studies (Bell & de Jong 2001 and Conselice et al. 2005, respectively) are plotted as two dot-dashed and dotted lines, respectively, to delineate rms scatter. In the lowest z bin for S_0.5, the local M* Faber-Jackson relation (Gallazzi et al. 2006) is plotted as two dotted lines to delineate rms scatter. All relations from the literature have been converted to a Chabrier initial mass function when necessary. An estimate of the S0.5/MbaryonTFR (Section 9) is plotted as a long dashed blue line in the lowest z bin.