The Baryonic Tully-Fisher Relation of Galaxies with Extended Rotation Curves and the Stellar Mass of Rotating Galaxies

I investigate the baryonic Tully-Fisher relation for a sample of galaxies with extended 21 cm rotation curves spanning the range 20 km s^-1<~V_f<=300 km s^-1. A variety of scalings of the stellar mass-to-light ratio Υ_* are considered. For each prescription for Υ_*, I give fits of the form M_d=AV^x_f. Presumably, the prescription that comes closest to the correct value will minimize the scatter in the relation. The fit with minimum scatter has A=50 M_solar km^-4 s⁴ and x=4. This relation holds over five decades in mass. Galaxy color, stellar fraction, and Υ_* are correlated with each other and with M_d, in the sense that more massive galaxies tend to be more evolved. There is a systematic dependence of the degree of maximality of disks on surface brightness. High surface brightness galaxies typically have Υ_*~3/4 of the maximum disk value, while low surface brightness galaxies typically attain ~1/4 of this amount.