Lithium in V505 Per

We determined the surface lithium abundance of the eclipsing binary components in V 505 Per (HIP 10961) to be $A(Li)$=2.65$\pm$0.07 and 2.35$\pm$0.1, which supports the rather unexpected conclusion that their surface Li abundances differ. We find effective temperatures of 6600 K + 6550 K ($\sim$150 K higher than previously reported), which places the stars at the hot limit of the Lithium Dip, thus alleviating the previously suggested discrepancy with cluster stars of similar ages and temperatures. These temperatures are also more consistent with the system's {\it Gaia} spectral energy distribution. Our iron abundances, $[Fe/H]=-0.15\pm 0.07$ and $-0.25\pm 0.1$, agree with the predictions of the higher temperatures deduced from our spectra and from the evolutionary tracks. The rotation rate implied by our line profiles, 12.5$\pm$1 km\,s$^{-1}$, is smaller than the synchronous rotation rate, which is a curious result given the circular orbit and the age of the system.