Abstract
12 W~UMa-type systems were observed at 3.6 cm with a goal to compare their radio luminosities with those of non-contact, rapidly rotating, late-type stars. Only 3 systems, all of spectral type K, have been detected. The detections and (low) upper limits for remaining systems confirm the strong under-luminosity of W~UMa-type systems. VW~Cep, which was been detected several times before, has been analyzed in terms of the temporal cumulative flux distribution. Apparently, VW~Cep spends most of the time in radio quiescence with flare-like events taking less than 20\% of time.
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