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The mass-loss mechanism for stripped-envelope supernovae (SESNe) remains debated comma but indirect evidence is mounting in support of binary stars. It wasn.t until 2014 comma however comma that the community obtained the first direct post-explosion detection of a surviving companion to a SESN (Type IIb SN 1993J). Since then comma there have been four more comma including the first fully stripped Type Ib-c SN 2013ge this past year. The field is now past the point of targeting individual systems one at a time. A statistically complete companion-mass distribution (including deep upper limits) can provide important constraints on the underlying physics used in binary evolution models (e.g. comma winds comma rotation comma metallicity comma nuclear burning instabilities) comma which in turn has far-reaching implications in all of astrophysics comma including merger sources for gravitational waves. Building the proper dataset is a slow process given the small number of viable candidates each year (considering distance comma extinction comma etc.). Here we propose optical+UV observations at the sites of the two most viable SESNe targets of this year to detect (or place meaningful limits on) any surviving companion. NUV (F275W-F336W) imaging offers an optimum detection strategy for the expected hot comma blue stellar companions comma while optical imaging can rule out shock interaction contributions and probe less likely comma but possible comma cooler star companions. We also propose ongoing monitoring of SN 2013ge. Given HST.s time horizon comma the degrading UV response on WFC3 comma and the requisite waiting period to allow the SN to fade before conducting a companion search comma now is the time to take full advantage of HST.s unique UV capabilities.