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). Avariety of scalings of the stellar mass-to-light ratio Y-star are considered. For each prescription for Y-star, I give fits of the form M-d = AV(f)(x). 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-circle dot km(-4) s(4) and x = 4. This relation holds over five decades in mass. Galaxy color, stellar fraction, and Y-star 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 Y-star similar to 3/4 of the maximum disk value, while low surface brightness galaxies typically attain similar to 1/4 of this amount.