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We analyze the resolved stellar populations of 473 massive star-forminggalaxies at 0.7 < z < 1.5, with multi-wavelength broad-band imaging fromCANDELS and Halpha surface brightness profiles at the same kiloparsecresolution from 3D-HST. Together, this unique data set sheds light on how theassembled stellar mass is distributed within galaxies, and where new stars arebeing formed. We find the Halpha morphologies to resemble more closely thoseobserved in the ACS I band than in the WFC3 H band, especially for the largersystems. We next derive a novel prescription for Halpha dust corrections, whichaccounts for extra extinction towards HII regions. The prescription leads toconsistent SFR estimates and reproduces the observed relation between theHalpha/UV luminosity ratio and visual extinction, both on a pixel-by-pixel andon a galaxy-integrated level. We find the surface density of star formation tocorrelate with the surface density of assembled stellar mass for spatiallyresolved regions within galaxies, akin to the so-called 'main sequence of starformation' established on a galaxy-integrated level. Deviations from thisrelation towards lower equivalent widths are found in the inner regions ofgalaxies. Clumps and spiral features, on the other hand, are associated withenhanced Halpha equivalent widths, bluer colors, and higher specific starformation rates compared to the underlying disk. Their Halpha/UV luminosityratio is lower than that of the underlying disk, suggesting the ACS clumpselection preferentially picks up those regions of elevated star formationactivity that are the least obscured by dust. Our analysis emphasizes thatmonochromatic studies of galaxy structure can be severely limited bymass-to-light ratio variations due to dust and spatially inhomogeneous starformation histories.

A CANDELS - 3D-HST Synergy: Resolved Star Formation Patterns at 0.7 < z < 1.5