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We present a targeted follow-up Hubble Space Telescope WFC3 F160W imagingstudy of very massive galaxies $(\log(M_{\rm{star}}/M_{\odot})> 11.2)$ selectedfrom a combination of ground-based near-infrared galaxy surveys (UltraVISTA,NMBS-II, UKIDSS UDS) at $1.5<z<3$. We find that these galaxies are diverse intheir structures, with $\sim1/3$ of the targets being composed of close pairs,and span a wide range in sizes. At $1.5<z<2.5$, the sizes of both star-formingand quiescent galaxies are consistent with the extrapolation of the stellarmass-size relations determined at lower stellar masses. At $2.5<z<3.0$,however, we find evidence that quiescent galaxies are systematically largerthan expected based on the extrapolation of the relation derived using lowerstellar mass galaxies. We used the observed light profiles of the blendedsystems to decompose their stellar masses and investigate the effect of theclose pairs on the measured number densities of very massive galaxies in theearly universe. We estimate correction factors to account for close-pair blendsand apply them to the observed stellar mass functions measured usingground-based surveys. Given the large uncertainties associated with thisextreme population of galaxies, there is currently little tension between the(blending-corrected) number density estimates and predictions from theoreticalmodels. Although we currently lack the statistics to robustly correct forclose-pair blends, we show that this is a systematic effect which can reducethe observed number density of very massive galaxies by up to a factor of$\sim1.5$, and should be accounted for in future studies of stellar massfunctions.

HST F160W Imaging of Very Massive Galaxies at $1.5