Notes. The numbers in Cols. 2 and 3 give the deviation of the space velocity of each star from the mean space velocity of Her-Lyr in Sect. 6 in units of σ. The criteria defined in Sect. 6 are applied to each single candidate. A discrepancy of more than two σ in UV velocity and age disqualifies a star as a probable member. For lithium, a more qualitative argument (EW(Li)_UMa < EW(Li)_{Her − Lyr} ≲ EW(Li)_Pleiades) is given. A Her-Lyr candidate is assigned a X if the equivalent width fits that of the canonical members, a if the star is lithium-depleted, and a ? if no information was found or if the criterion is not applicable to this particular object. Similarly, a X is given if a candidate displays significant chromospheric activity , otherwise or ? if unknown. The ≳ and ≲ signs in Col. 6 indicate that the age was derived based on an upper limit of the rotational period, i.e., vsini. Based on these criteria, the membership probability is qualitatively indicated by a + for a high membership probability and a o for doubtful membership. Improbable members do not fulfill at least one of the criteria and are indicated by –. In case of unavailable information or upper limits, the candidate is kept as a possible member and marked by ? (Col. 7). For comparison, results by Fuhrmann (2004) and López-Santiago et al. (2006) are given in the last two columns. In cases of resolved multiple systems where common proper motion is confirmed (see Sects. 3 and 7), similar UVW velocity is assumed and the membership is assessed as for the primary. Canonical members are written in bold face.