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We propose a snapshot program to determine the occurrence rate of interaction between circumstellar material (CSM) and the ejecta of stripped supernovae (SNe IIb comma Ib comma Ic comma SLSNe-I) using NUV imaging at >1 year after explosion. Large amounts of CSM must have been ejected by the progenitors to these SNe comma so the potential for significant CSM interaction is present. However comma only in very few cases have interaction signatures been identified using ground-based observations. In these cases we see H emission in late-time spectra created by the ejecta crashing into H-rich material. The reason interaction signatures are rare could be because the bulk of envelope material is ejected a very long time before explosion comma or because it is V1.0 how or if CSM interaction with H-poor material would appear in the optical. A systematic survey in the NUV will be able to identify NUV excess from interaction regardless of the CSM composition. NUV emission from CSM has been identified in SNe Ia comma but no late-time NUV survey has been carried out for stripped SNe. This NUV snapshot program targets an untargeted sample of 163 stripped SNe comma and requires on average only a 30 minute duration visit per target. NUV imaging will constrain the prevalence comma radius comma mass and composition of CSM around stripped SNe comma and will offer novel constraints on both single- and binary-star models for stripped SNe.