UBV light curves obtained in 1975 for both components of ADS 9537 are presented. These light curves and the light curve of BV Dra by Yamasaki have been solved for geometrical parameters using the synthesis method under two hypotheses explaining theW-subclass light curves: (1) temperature excess of the less massive components; (2) spots on the more massive components; the results are very similar. Because of the poor determinacy of the solutions, mass-ratios have been assumed:q=0.8 for BV Dra and a range inq for BW Dra; our solutions suggest preference for smallerq in the latter system. We compare both variables and conclude that they follow the Main Sequence dependences. We give also a bried discussion of the existing information on other contact binaries in multiple (visual) systems: the contact binaries seem to follow the same statistical distributions for occurrence in multiples as found for detached binaries but severe selection effects limit detectability for multiple systems with ‘wide’ orbits having semi-axes below 100 a.u.