Distribution of rotation periods for the M35 members in our sample. The colour of each symbol indicates the deviation of the EW(Li) obtained for that star from a third order polynomial fit to EW(Li) vs. (BP–RP)₀. Circles indicate the M35 members observed in 1999 December and 2001 February whose Li EWs have been derived as discussed in Sect. 5.2, while triangles are those M35 members whose Li EWs have been taken from Barrado y Navascués et al. (2001a), Anthony-Twarog et al. (2018), or Jeffries et al. (2021). Squares denote those stars observed in 1999 December and 2001 February for which we could only derive upper limits for the Li EWs. Top: our complete set of M35 members with rotation periods. Bottom: only those sources classified as single stars are shown. The four outliers that do not follow the general trend are circled in black.