Table 1 shows data for the 176 SMC objects which form 75 star cluster pairs and multiplets (Bica & Dutra 2000), considering that the pair BS63/B67 in the latter study is possibly a triplet with NGC 294 (ODB98). By columns: (1) object cross-identification in the different catalogues: N (Henize 1956), K (Kron 1956), L (Lindsay 1958), H (Hodge 1960), SL (Shapley & Lindsay 1963), B (Brück 1976), DEM (Davies et al. 1976), ESO (Lauberts 1982), H86- (Hodge 1986), MA (Meyssonier & Azzopardi 1993), BS (Bica & Schmitt 1995), OGLE (Pietrzynski et al. 1998). Note that some are embedded objects, named after the corresponding HII region; (2) and (3) right ascension and declination for the epoch J2000, respectively; (4) object type following BS95: C for star cluster, NC for small HII regions with embedded star clusters, CN for clusters which show some traces of emission, A for associations, CA and/or AC for star clusters of low density and objects with intermediate properties, AN for associations which show some traces of emission and NA for HII regions with embedded associations; (5) and (6) major and minor sizes, respectively; (7) position angle of major axis ( = N, = E); (8) centre-to-centre angular separation (1 arcsec = 0.28 pc assuming an absolute distance modulus (m-M) = 18.9 for the SMC, Westerlund 1990). For triplets and multiplets we measured the separation between the two main members, as indicated in the corresponding object line in the table; (9) remarks: m6, m5, m4, mT and mP indicate groups with six, five and four members, triplets and pairs, respectively. A running number identifies each candidate system. Abbreviations "br*'' indicates that a bright star is present; "att'' means attached to. A hierarchical indication is given for objects embedded in or superimposed on larger ones: "in'' suggests a possible physical connection while "sup'' suggests a projection. There are 56 pairs, 15 triplets, 2 quadruplets, 1 quintuplet and 1 sextuplet. The quintuplet is located in the star forming region NGC 395 with dimensions 25 pc 18 pc which in turn is embedded in the HII complex SMC-DEM126 with 66 pc 35 pc according to angular sizes in BS95. The sextuplet is mostly contained in the OB association H-A35 (Hodge 1985) with dimensions 57 pc 47 pc. One quadruplet is located in H-A60 with 44 pc 24 pc. Note that dimensions (Cols. 5 and 6) and position angle (Col. 7) are from Bica & Dutra (2000) and were measured on plates. The dimensions are in general larger than the isophotal sizes in the subsequent analyses.
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