THE STAR FORMATION MASS SEQUENCE OUT TO z=2.5

We study the star formation rate (SFR)-stellarmass (M-star) relation in a self-consistent manner from 0 < z < 2.5 with 22,816 star-forming galaxies selected from the NEWFIRM Medium-Band Survey. We find a significant nonlinear slope of the relation, SFR proportional to M-star(0.6), and a constant observed scatter of 0.34 dex, independent of redshift and M-star. However, if we select only blue galaxies we find a linear relation SFR proportional to M-star, similar to previous results at z = 0 by Peng et al. This selection excludes red, dusty, star-forming galaxies with higher masses, which brings down the slope. By selecting on L-IR/L-UV (a proxy for dust obscuration) and the rest-frame U - V colors, we show that star-forming galaxies fall in three distinct regions of the log(SFR)-log(M-star) plane: (1) actively star-forming galaxies with normal dust obscuration and associated colors (54% for log(M-star) > 10 at 1 < z < 1.5), (2) red star-forming galaxies with low levels of dust obscuration and low-specific SFRs (11%), and (3) dusty, blue star-forming galaxies with high-specific SFRs (7%). The remaining 28% comprises quiescent galaxies. Galaxies on the normal star formation sequence show strong trends of increasing dust attenuation with stellar mass and a decreasing specific SFR, with an observed scatter of 0.25 dex. The dusty, blue galaxies reside in the upper envelope of the star formation sequence with remarkably similar spectral shapes at all masses, suggesting that the same physical process is dominating the stellar light. The red, low-dust star-forming galaxies may be in the process of shutting off and migrating to the quiescent population.