  Hot Dust-Obscured Galaxies (Hot DOGs) are among the most luminous galaxies in
the Universe. Powered by highly obscured, possibly Compton-thick, active
galactic nuclei (AGNs), Hot DOGs are characterized by SEDs that are very red in
the mid-IR yet dominated by the host galaxy stellar emission in the UV and
optical. An earlier study identified a sub-sample of Hot DOGs with
significantly enhanced UV emission. One target, W0204-0506, was studied in
detail and, based on Chandra observations, it was concluded that the enhanced
emission was most likely due to either extreme unobscured star-formation (${\rm
SFR}>1000~M_{\odot}~\rm yr^{-1}$) or to light from the highly obscured AGN
scattered by gas or dust into our line of sight. Here, we present a follow-up
study of W0204-0506 as well as two more Hot DOGs with excess UV emission. For
the two new objects we obtained Chandra/ACIS-S observations, and for all three
targets we obtained HST/WFC3 F555W and F160W imaging. We conclude that the
excess UV emission is primarily dominated by light from the central highly
obscured, hyper-luminous AGN that has been scattered into our line of sight. We
cannot rule out, however, that star-formation may significantly contribute to
the UV excess of W0204-0506.
