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Galaxy morphology and its evolution over the cosmic epoch hold importantclues for understanding the regulation of star formation (SF). However,studying the relationship between morphology and SF has been hindered by theavailability of consistent data at different redshifts. Our sample, combiningCANDELS (0.8 < z < 2.5) and the GALEX-SDSS-WISE Legacy Catalog (GSWLC; z ~ 0),has physical parameters derived using consistent SED fitting with flexible dustattenuation laws. We adopt visual classifications from Kartaltepe et al. 2015and expand them to z ~ 0 using SDSS images matching the physical resolution ofCANDELS rest-frame optical images and deep FUV GALEX images matching thephysical resolution of the CANDELS rest-frame FUV images. Our main finding isthat disks with SF clumps at z ~ 0 make a similar fraction (~15%) ofstar-forming galaxies as at z ~ 2. The clumpy disk contribution to the SFbudget peaks at z ~ 1, rather than z ~ 2, suggesting that the principal epochof disk assembly continues to lower redshifts. Star-forming spheroids ("bluenuggets"), though less centrally concentrated than quenched spheroids,contribute significantly (~15%) to the SF budget at z ~ 1-2, suggesting thatcompaction precedes quenching. Among green valley and quiescent galaxies, thepure spheroid fraction drops since z ~ 1, whereas spheroids with disks(S0-like) become dominant. Mergers at or nearing coalescence are enhanced inSFR relative to the main sequence at all redshifts by a factor of ~2, butcontribute $\lesssim$5% to the SF budget, with their contribution remainingsmall above the main sequence.

CANDELS Meets GSWLC: Evolution of the Relationship Between Morphology and Star Formation Since z = 2