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Compact star-forming clumps observed in distant galaxies are often suggestedto play a crucial role in galaxy assembly. In this paper, we use a novelapproach of applying finite resolution deconvolution on ground-based images ofthe COSMOS field to resolve 20,185 star-forming galaxies (SFG) at 0.5<z<2 to anangular resolution of 0.3", and study their clumpy fractions. A comparisonbetween the deconvolved and HST images across four different filters shows goodagreement and validates the deconvolution. We model spectral energydistributions using the deconvolved 14-band images to provide resolved surfacebrightness and stellar mass density maps for these galaxies. We find that thefraction of clumpy galaxies decreases with increasing stellar masses, and withincreasing redshift: from ~30% at z ~ 0.7 to ~50% at z ~ 1.7. Using abundancematching, we also trace the progenitors for galaxies at z ~ 0.7 and measure thefractional mass contribution of clumps toward their total mass budget. Clumpsare observed to have a higher fractional mass contribution toward galaxies athigher redshift: increasing from ~1% at z ~ 0.7 to ~5% at z ~ 1.7. Finally, themajority of clumpy SFGs have higher specific star formation rates (sSFR)compared to the average SFGs at fixed stellar mass. We discuss the implicationof this result to in-situ clump formation due to disk instability.

astrophysical journal/the astrophysical journal

Finite Resolution Deconvolution of Multi-Wavelength Imaging of 20,000  Galaxies in the COSMOS Field: The Evolution of Clumpy Galaxies Over Cosmic  Time