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We present Ha maps at 1kpc spatial resolution for star-forming galaxies atz~1, made possible by the WFC3 grism on HST. Employing this capability over allfive 3D-HST/CANDELS fields provides a sample of 2676 galaxies. By creating deepstacked Halpha (Ha) images, we reach surface brightness limits of1x10^-18\erg\s\cm^2\arcsec^2, allowing us to map the distribution of ionizedgas out to >10kpc for typical L* galaxies at this epoch. We find that thespatial extent of the Ha distribution increases with stellar mass asr(Ha)[kpc]=1.5(Mstars/10^10Msun)^0.23. Furthermore, the Ha emission is moreextended than the stellar continuum emission, consistent with inside-outassembly of galactic disks. This effect, however, is mass dependent withr(Ha)/r(stars)=1.1(M/10^10Msun)^0.054, such that at low masses r(Ha)~r(stars).We map the Ha distribution as a function of SFR(IR+UV) and find evidence for`coherent star formation' across the SFR-M plane: above the main sequence, Hais enhanced at all radii; below the main sequence, Ha is depressed at allradii. This suggests that at all masses the physical processes driving theenhancement or suppression of star formation act throughout the disks ofgalaxies. It also confirms that the scatter in the star forming main sequenceis real and caused by variations in the star formation rate at fixed mass. Athigh masses (10^10.5<M/Msun<10^11), above the main sequence, Ha is particularlyenhanced in the center, plausibly building bulges and/or supermassive blackholes. Below the main sequence, the star forming disks are more compact and astrong central dip in the EW(Ha), and the inferred specific star formationrate, appears. Importantly though, across the entirety of the SFR-M plane, theabsolute star formation rate as traced by Ha is always centrally peaked, evenin galaxies below the main sequence.

Where stars form: inside-out growth and coherent star formation from HST Halpha maps of 2676 galaxies across the main sequence at z~1