摘要：Due to an unfortunate error in the computation of distance between clusters, Tables 4 and 5, and Fig. 12 in Sect. 3.3 of the original paper contain incorrect values. Here we present the updated tables and figure. Table 4 gives the list of cluster pairs that differ by less than 100 pc in distance and 5 km s −1 in velocity in our high-quality sample. The closest pairincludes ASCC 16and ASCC 21, which are separated by ∼13 pc, with a velocity difference of 4.5 km s −1 . RSG 7 and RSG 8, as well as ASCC 16 and ASCC 19, are also close pairs separated by ∼24 pc, with velocity differences of 2.3 km s −1 and 3.6 km s −1 respectively, thus good candi- dates to be physically related. Several possibly larger complexes may be found in that table, formed by clusters that appear more than one time. Table 5 gives a list of candidates binaries from the literature. The most famous binary cluster formed by h and χ Persei (NGC 869 and NGC 884, Messow & Schorr 1913) appears to have a separation of 19.5 pc. An excellent candidate binary is the pair Collinder 394 and NGC 6716, which lie at a distance of ∼11 pc from each other. IC 2602 and Platais 8 are also close from each other (∼35 pc) and they are possibly phys- ically related, owing to their common age in DAML and similar velocity (also reported in Table 4). The other pairs in Table 5 have much larger separation and they are more likely to result from a chance alignment than that they are a physical binary system.
关键词：enstars: kinematics and dynamicsGalaxy: kinematics and dynamicsopen clusters and associations: generalerrata, addenda
