The clump stellar mass function (cSMF) tells you the abundance of clumps as a function of their mass. Here, we compare the cSMF of young clumps to old clumps. We find that the older clump population has a flatter cSMF slope, suggestive of a higher abundance of more massive clumps relative to lower-mass ones. This could imply mechanisms that preferentially disrupt clumps based on their mass as clumps evolve!
Wouldn't it be nice if we could get HST-like images from the ground? Here we show examples of deconvolved galaxies in multiple filters. Each row shows a different galaxy, and each panel compares the rest-frame UV, the rest-frame optical, and the composite. Within each panel we show the ground-based image, its deconvolved counterpart, and the space-based image for reference. Together these panels illustrate that image deconvolution can recover real structure that is all but invisible in the original ground-based data.