Berkeley 12 Only straggler candidates inside a radius of 2' around the centre Berkeley 12 of coordinates have been considered. Berkeley 14 Only straggler candidates inside a radius of 3' around the centre Berkeley 14 of coordinates have been considered. The red limit of the blue Berkeley 14 straggler area is (B-V)=0.74. Berkeley 18 Only straggler candidates inside a radius of 3' around the centre Berkeley 18 of coordinates have been considered. The red limit of the blue Berkeley 18 straggler area is (B-V)=0.88. Berkeley 19 The cleaned colour-magnitude diagram in (65) was examined. Berkeley 20 In the VI CCD photometry (261), 16 straggler candidates are Berkeley 20 identified inside a radius of 1.5' around the cluster centre: Berkeley 20 they show the same central concentration as the red giants, Berkeley 20 like in M67. Berkeley 21 The red limit of the blue straggler area is (B-V)=0.97. Berkeley 22 The red limit of the blue straggler area is (B-V)=1.06. In (210) Berkeley 22 it is remarked that most of the straggler candidates are near Berkeley 22 the cluster centre; however, if the apparent diameter given in Berkeley 22 (259), which is the one listed in Table 1, is taken as correct, Berkeley 22 the stragglers do not appear so central. It is possible that Berkeley 22 this diameter is still too small. Berkeley 23 Only straggler candidates inside a radius of 4' around the centre Berkeley 23 of coordinates have been considered. The red limit of the blue Berkeley 23 straggler area is (B-V)=0.53. Berkeley 30 Only straggler candidates inside a radius of 3' around the centre Berkeley 30 of coordinates have been considered. Berkeley 31 The red limit of the blue straggler area is (B-V)=0.50. Berkeley 32 The red limit of the blue straggler area is (B-V)=0.55. Stars Berkeley 32 30, 31, and 40 are cited as blue stragglers in (213). Adopted Berkeley 32 cluster centre: star 16 of (213). Berkeley 33 Only straggler candidates inside a radius of 3' around the centre Berkeley 33 of coordinates have been considered. Berkeley 39 Only straggler candidates inside a radius of 6' around the centre Berkeley 39 of coordinates have been considered. The red limit of the blue Berkeley 39 straggler area is (B-V)=0.64. Four probable members, short- Berkeley 39 period, eclipsing binaries are identified among the stragglers Berkeley 39 by (215). Another Delta Scuti straggler is found by (272). Berkeley 42 Adopted cluster centre: star 329 of (22). Berkeley 58 The diagram of stars up to a radius of 3' around the cluster Berkeley 58 centre has been examined. Berkeley 60 Only straggler candidates inside a radius of 2' around the centre Berkeley 60 of coordinates have been considered. Berkeley 62 The diagram of stars inside a radius of 3' around the centre of Berkeley 62 coordinates has been examined. Berkeley 64 Only straggler candidates inside a radius of 3' around the centre Berkeley 64 of coordinates have been considered. Berkeley 66 The blue straggler area is heavily contaminated by field stars. Berkeley 66 Only straggler candidates inside a radius of 2' around the Berkeley 66 centre of coordinates have been considered. Berkeley 69 The identification chart was not available. Berkeley 70 Only straggler candidates inside a radius of 4' around the centre Berkeley 70 of coordinates have been considered. The red limit of the blue Berkeley 70 straggler area is (B-V)=0.71. Berkeley 81 Only straggler candidates inside a radius of 5' around the centre Berkeley 81 of coordinates have been considered. The red limit of the blue Berkeley 81 straggler area is (B-V)=1.15. Berkeley 86 The dereddened diagram of possible members in (147) was examined. Berkeley 87 The dereddened diagram of possible members in (400) was examined. Berkeley 99 The red limit of the blue straggler area is (B-V)=0.75. Berkeley 104 Only straggler candidates inside a radius of 2' around the centre Berkeley 104 of coordinates have been considered. Blanco 1 Zeta Sculptoris=HD 224990. The identification chart is in the Blanco 1 ubvy photometry (431), where the star Zeta Scl is cited as a Blanco 1 blue straggler and is given the following: (b-y)=-0.064, (u-b)= Blanco 1 0.518, m1=0.101, c1=0.441, and spectrum B6III-B5V. Bochum 1 Apparent cluster diameter from (291). Collinder 97 Cluster reddening from (27). Collinder 135 Selected cluster angular diameter from (259). Collinder 223 Stars 35 and 80 are cited as blue stragglers in (80). Star 2, Collinder 223 which also appears as a blue straggler, is at 3.5 cluster Collinder 223 radii from the centre, which has been set on star 84 (ref. 80). Collinder 223 Star 35=HD 305295, star 80=HD 305218. Collinder 261 The red limit of the blue straggler area above the turnoff is Collinder 261 (B-V)=0.86. In (271) 10 short-period eclipsing variables are Collinder 261 found among the 178 straggler candidates identified by the Collinder 261 authors from their VI CCD photometry. Among our candidates, Collinder 261 the variables are: star 772 (EW), star 1030 (EA/EB), star 1327 Collinder 261 (EW), star 2287 (EB/EW), star 2290 (EA/EB). Collinder 394 The dereddened colour-magnitude diagram in (402) was examined. Haffner 17 All the cluster parameters are from (8). The diagram of stars Haffner 17 up to 3' of the centre was examined. Harvard 5 = Collinder 258. The apparent cluster diameter was taken from Harvard 5 (366). Star 2=HD 108295 has a spectrum B2(V)N (184). Harvard 8 = Collinder 268. Star 2 is cited as a blue straggler in (293). Harvard 8 Adopted cluster centre: star 12 of (293). Hogg 10 The apparent cluster diameter was taken from (71). Hogg 17 Star 1 appears as a straggler but is a non-member according Hogg 17 to (248). Hyades Star 56 is a cluster member acording to the proper motion and Hyades radial velocity study (409). Adopted cluster centre: star 57 Hyades of the same reference. References (1) and (281) cite star 56 Hyades as a blue straggler. Star 56=68 Tauri=HD 27962 has a spectrum Hyades A3V and an optical companion of magnitude 9 (55). The blue Hyades straggler does not show anomalous lithium abundances (50). Hyades In (1) this star is given a spectrum Am(K/H/M=A2/A3:/A5) and Hyades a projected velocity v.sin i=18km/s. It has been suggested Hyades (303) that the white dwarf component of the binary V471 Tauri Hyades in this cluster descends from a blue straggler. The selected Hyades angular diameter in (259) is listed. IC 166 The cluster is given E(B-V)=0.80 and an age between those of IC 166 NGC 752 and NGC 7789 in (51). Star 459 could not be identified IC 166 in the chart. IC 1311 Several possible blue and red stragglers are pointed out in (10). IC 1369 Adopted cluster centre: star 57 (ref. 160). All the blue IC 1369 stragglers lie on the periphery of the cluster, but they are IC 1369 members according to (169). In particular, note the close IC 1369 group of stars 155-156-157. IC 1805 The dereddened colour-magnitude diagram of (188) was examined. IC 2488 Diagrams in (311) were also examined. Adopted cluster centre: IC 2488 star 28 in (311). Star 99=HD 302225(B8) is cited as a blue IC 2488 straggler in (311), and is a probable cluster member (85). IC 2581 The dereddened colour-magnitude diagram in (392) was examined. IC 2602 Star 18=Theta Carinae=HD 93030 is a well known blue straggler. IC 2602 In (177) this star is given the following: v=2.78, (b-y)=-0.094, IC 2602 m1=0.063, c1=-0.078, beta=2.603, spectrum: B0Vp. Reference IC 2602 (281) gives it a projected velocity v.sin i=195km/s. Theta Car IC 2602 is a spectroscopic binary of period 1.77 days and eccentricity IC 2602 0.446 (423), thought to be the result of a mass transfer event IC 2602 in a close binary: an account of this interpretation can be IC 2602 found in (117). IC 2714 Star 98, which also appears as a blue straggler, is a non-member IC 2714 according to (83). IC 2944 Star 21=HD 101545 has a spectrum B0III (184). IC 4651 The colour-magnitude diagrams in (18) and (111) were examined. IC 4651 In the CCD photometric study (18) stars 9 and 46 are considered IC 4651 as probable binaries; the presence of many binaries in the turn- IC 4651 off area is also suggested. Stars 9, 40, 46, and 75 are cited IC 4651 as blue stragglers in (111). Star 46 has a spectrum A5IV, and IC 4651 stars 9 and 75 are non-members according to (253). Membership IC 4651 probabilities based on radial velocities (280): star 11, 23%, IC 4651 star 75, 61%. The DDO photometry of the cluster giants (372) IC 4651 finds CN overabundance in the stragglers, and draws attention to IC 4651 the possible relation between this fact and the blue straggler IC 4651 phenomenon. Other clusters with blue stragglers and CN-strong IC 4651 giants (372): Melotte 66, NGC 2204, NGC 2420, NGC 2682, and IC 4651 NGC 7789. According to (35), star 46 is an X-ray source, a IC 4651 probable cluster member, and a probable binary. IC 4725 Spectra: Star 1=HD 170475, B8III/IV (184); star 50=HD 170682, IC 4725 B6V (121); star 91=HD 170719, B9V (121); star 163=HD 170835, IC 4725 B2.5Vne (149); star 167=HD 170836, B8II (184). IC 4756 Probabilities of membership by (173): Star 104=HD 172012, 67%; IC 4756 star 120, 93%; star 1142, 62%. Stars 5 and 58 (ref. 173) appear IC 4756 as stragglers but they are non-members according to the same IC 4756 reference. Spectra from (159): star 104, A0III+; star 279= IC 4756 HD 172248, B8IV; star 280=HD 172271, kB9 A2 IIIp SiSr ((shell)). IC 4756 Star 104 is cited as a probable blue straggler in (359). It is IC 4756 suggested in (12) that the cluster member and supergiant IC 4756 HD 172365 is a post-blue straggler resulting from the merger of IC 4756 a close binary system. IC 5146 The cluster is given an age of 3 Myr in (431). The dereddened IC 5146 diagram of (429) was examined: star 42=BD+46 3474 has a heavily IC 5146 reddened B1V spectrum. King 2 Only candidates inside r/R=1 were considered. Adopted cluster King 2 centre: star 419 of (21). King 8 Star 105 (sp. F3V) belongs to the field according to (67). Star King 8 8 could not be identified in the chart. King 15 Only straggler candidates inside a radius of 2' around the centre King 15 of coordinates have been considered. Lynga 1 Star 2=DM-61 04247. Markarian 18 The dereddened colour-magnitude diagram of (422) was examined. Melotte 20 = Alpha Persei cluster. The cluster parameters are from (259). Melotte 20 Star HD 22928 = Delta Persei (sp. B6n) is a cluster member Melotte 20 according to its radial velocity (320). Melotte 66 The red limit of the straggler area is (V-I)=0.76. In (237) it Melotte 66 is suggested that a spread in the metal abundances may account Melotte 66 for the observed dispersion around the turnoff in the colour- Melotte 66 magnitude diagram. In that case, several stars that appear as Melotte 66 blue stragglers would not be such. Melotte 101 All the cluster parameters except the apparent diameter were Melotte 101 taken from (8). Melotte 105 All the cluster parameters except the apparent diameter were Melotte 105 taken from (8). Melotte 111 = Coma cluster. Adopted cluster centre: star 91 in (389). Star Melotte 111 146 = 17 Comae = HD 108662 = AI Comae is a cluster member (389) Melotte 111 and an Alpha Canum Venaticorum variable (281). It is cited Melotte 111 as a blue straggler by (1), (185), and (281). Reference (1) Melotte 111 gives this star a projected velocity v.sin i=15km/s and a Melotte 111 spectrum A0Vp(Sr,Cr,Si,Eu). NGC 103 Star 29 appears as a blue straggler in the diagrams of (164), NGC 103 but it is located at about five cluster radii from the centre NGC 103 to the west. NGC 129 Adopted cluster centre: star 100 in chart of (24). Star 10 has NGC 129 a spectrum B9V (231) and a membership probability of 10% (438). NGC 129 Star 6 (sp. A05V) also appears as a straggler, but has a prob- NGC 129 ability of 7% (438). Star 8 (ref. 181) = 196 (WEBDA) is given NGC 129 0% in the same proper motion study. Star 173 (WEBDA) is star D NGC 129 in (24) and star 14 in (181): it appears mildly as a straggler NGC 129 in (181), but as a main-sequence star in (24). NGC 136 Cluster parameters are from (164). NGC 188 Membership probabilities according to (331) and (407): NGC 188 star 1003, 90%; 1032, 98%; 1043, 98%; 1050, 97%; 1093, NGC 188 98%; 1102, 98%; 2008, 97%; 2020, 97%; 2024, 97%; 2031, 93%; NGC 188 2046, 99%; 2069, 98%; 2074, 92%; 2082, 98%; 2105, 98%; 2119, NGC 188 93%; 2127, 98%; 2138, 94%; 2151, 97%; 3074, 95%; 3115, 98%; NGC 188 3135, 93%; 3151, 98%. Star 2189 is given 90% in (407) but NGC 188 0% in (331). In the photometric study (119) the following NGC 188 stars are cited as blue stragglers: 1003, 1005, 1032, NGC 188 1033, 1043, 1093, 1102, 1103, 1112, and 2046. Star 2127 NGC 188 is a W Ursae Majoris eclipsing binary (205). An hyphothetical NGC 188 relation between the blue stragglers and the apparent NGC 188 lack of bright giants in the cluster nucleus is discussed in NGC 188 (208). In (404) and (407) it is suggested that the cluster is NGC 188 somewhat younger than is usually agreed, so several stars that NGC 188 appear as blue stragglers would not be such. In the proper NGC 188 motion study (102) it is found that the stragglers are not more NGC 188 centrally concentrated than the red giants. In the CCD study NGC 188 (208) the discovery of a probable FK Comae variable (star V8) NGC 188 is reported; this star may be a `red straggler' candidate. NGC 366 The diagram of stars inside a radius of 2' around the centre of NGC 366 coordinates was examined. NGC 381 Star 207 (ref. 91)= star 2287 (WEBDA) appears as a blue straggler NGC 381 in the V vs. (B-V) diagram of (91), but it is located more than NGC 381 a degree towards the NE of star 79 of (91). NGC 433 The colour-magnitude diagram of stars inside a radius of 3' NGC 433 around the centre of coordinates was examined. NGC 436 The colour-magnitude diagram of stars inside a radius of 3' NGC 436 around the centre of coordinates was examined. Stars 282 and NGC 436 320 have spectra A0 (41). NGC 457 Only the photoelectric data of (181) were examined. Adopted NGC 457 cluster centre: star 23011 of ref. (290). Star 5 = DM+57 00247 NGC 457 has a spectrum O9.5IV (180), is cited as a blue straggler in NGC 457 (143) and (281), and is a probable cluster member (26). Star 7 NGC 457 (ref. 181) = 0038 (WEBDA) = 23094 (ref. 290) appears as a blue NGC 457 straggler in (181), but it is a non-member according to (26). NGC 559 Star 85 is cited as a blue straggler in (185). In the diagrams NGC 559 of the photoelectric study (54) it appears closer to the main NGC 559 sequence; this star, however, is a probable non-member according NGC 559 to its colour and spectrum (162). NGC 654 The dereddened colour-magnitude diagram in (316) was examined. NGC 744 Star 7 has a spectrum A05 (180). NGC 752 The membership study (330) gives star 209=BD+36 367 a probab- NGC 752 ility of 99%. The ubvy study (403) gives star 209 the folowing: NGC 752 v=9.74, (b-y)=0.028, m1=0.153, c1=1.002. Reference (117) cites NGC 752 star 209 as a blue straggler and star 110 as a `red straggler.' NGC 752 References (179), (185), and (283) also cite star 209 (spectrum NGC 752 B9.5p?) as a blue straggler. Star 209 is an X-ray source (36), NGC 752 and it is not a photometric variable (411). Stars 32, 271, 309, NGC 752 and 1496 also appear as blue stragglers in the colour-magnitude NGC 752 diagrams of (107), (148), and (197), but they are non-members NGC 752 according to (330). NGC 884 = Chi Persei cluster. Star 17=HD 14434 is cited as a blue NGC 884 straggler in (281). According to (201), star 17 has a spectrum NGC 884 O5.5Vnp, a projected velocity v.sin i=400km/s, and it is a NGC 884 possible variable. The reference (371) gives stars 17 and 20 NGC 884 spectra O6.5V and A0I. In (117) the star 2296 (WEBDA) = 19 NGC 884 (ref. 371) = BD+56 574 (sp. B1III) is also cited as a straggler. NGC 1193 Adopted cluster centre: star 310 in ref. (207). In the same NGC 1193 reference, stars 190, 245, 295, 335, and 424 are cited as blue NGC 1193 stragglers. NGC 1252 Adopted cluster centre: star 10 in ref. (42). Star 4=HD 20286 NGC 1252 (sp. B9.5V) is a cluster member according to the same reference, NGC 1252 where the cluster is given an age of 0.5 Gyr. NGC 1342 Only the photoelectric data of (181) were examined. References NGC 1342 (1) and (281) cite star 2=HD 21728 as a blue straggler. In (1) NGC 1342 this star is given a spectrum A0II-IIIp(Si(st),Mg(wk)) and a NGC 1342 projected velocity v.sin i<40km/s. Star 4=HD 275501 has a NGC 1342 spectrum G8II according to (381). Both stars have a membership NGC 1342 probability of 99% (ref. 148). NGC 1348 Only straggler candidates inside a radius of 4' around the centre NGC 1348 of coordinates have been considered. NGC 1444 The apparent cluster diameter was taken from (162). Star 3 has NGC 1444 a spectrum A5V according to (180). NGC 1528 Diagrams in (148) were also examined. References (1) and (281) NGC 1528 cite star 1 (WEBDA)=HD 26603 as a blue straggler, but in (148) NGC 1528 it is assigned a membership probability of 0% according to its NGC 1528 proper motion. Star 209 (WEBDA) also appears as a straggler in NGC 1528 (148), but it is not a proper-motion member. NGC 1545 Only the photoelectric data of (181) were examined. NGC 1647 The dereddened colour-magnitude diagram in (398) was examined. NGC 1664 Only the photoelectric data of (181) were examined. The apparent NGC 1664 cluster diameter was taken from (162). Star 1=HD 30650 has a NGC 1664 membership probability of 91% according to (218), and a spectrum NGC 1664 B3V according to (180). Star 4 (ref. 181) = 578 (WEBDA) also NGC 1664 appears as a blue straggler, but it is not a cluster member NGC 1664 according to (218). NGC 1778 Only the photoelectric data of (181) were examined. NGC 1798 The cluster parameters are from (309). NGC 1817 Each one of the five blue stragglers has a membership probability NGC 1817 of 99% according to (29). Stars 2020, 2072, 2090, and 2110 are NGC 1817 cited as blue stragglers in (165). NGC 1893 The colour-magnitude diagrams in (267) were also examined. Star NGC 1893 301005=HD 242935 has a spectrum O8V((f)) (ref. 267). NGC 1901 Star 4=HD 35094 has a spectrum A5V (184), appears to belong to a NGC 1901 subgroup of bright stars at about 18' from the cluster centre, NGC 1901 and is a cluster member (301). NGC 1907 The diagrams in (181), (334), and (379) were examined. Stars G NGC 1907 and 4 have spectra B9V and B3V (180). Star B is HD 281143. NGC 1907 Stars 10, 51, 116, and 132 (WEBDA numbers) appear as stragglers NGC 1907 in some diagrams, but as main-sequence stars in others. NGC 1912 Only the photoelectric data of (181) were examined. NGC 1976 = Trapezium. The apparent cluster diameter was taken from (162). NGC 1976 The colour-magnitude diagram of (367) was dereddened using the NGC 1976 reddenings for each star listed in the reference. Star 1891 NGC 1976 (WEBDA) = Theta1 Orionis A = HD 37022 (sp. O7Vp,v.sin i=140km/s, NGC 1976 var?), appears blueward the ZAMS in the dereddened diagram, but NGC 1976 it is a non-member according to (276). NGC 2099 Star 56=HD 248599. Membership probabilities (439): star 9, 86%, NGC 2099 star 56, 12%, and star 342, 27%. Star 204, which also appears NGC 2099 as a straggler, has a probability of 9% (439). NGC 2129 Only the photoelectric data of (181) were examined. NGC 2158 The apparent cluster diameter was taken from (162). Only stars NGC 2158 inside a radius of 3' were considered. Some membership NGC 2158 probabilities from (219): star 3, 73%, star 14, 32%, star 25, NGC 2158 43%, star 414, 86%. Star 117 (=3347) has a 6% and star 228 NGC 2158 (=3142) is not a cluster member (219). NGC 2168 Star 218=HD 41940 has a membership probability of 72% (ref. 278) NGC 2168 and a spectrum B2V (180). It is cited as a straggler en (278). NGC 2175 The dereddened colour-magnitude diagram of (158) was examined. NGC 2192 The cluster parameters are from (309). NGC 2204 All the cluster parameters except the apparent diameter are from NGC 2204 (8). Reference (171) draws attention to the strong central NGC 2204 concentration of the blue stragglers, also observed in M67 and NGC 2204 Melotte 66. NGC 2251 Stars 1=HD 259954, 4 (pg)=HD 259989, and 4 (pe)=HD 260022 are NGC 2251 cited as blue stragglers in (1) and (281). Reference (1) gives: NGC 2251 star 1 (sp. B2IV, v.sin i<40km/s); star 34 (sp. B9.5V, v.sin i= NGC 2251 200km/s (approx)); star 4 (sp. A0p(Si)). NGC 2259 Only straggler candidates inside a radius of 2' around the centre NGC 2259 of coordinates have been considered. NGC 2266 Adopted cluster centre: star 14 (ref. 214). Star 10 is cited as NGC 2266 a blue straggler in the same reference. NGC 2281 This cluster shows mass segregation (436); in particular, the NGC 2281 binaries appear concentrated. Star 62=HD 49010 is cited as a NGC 2281 blue straggler in (1) and (281). In (1) this star is given a NGC 2281 spectrum A2:Vp (Si(st),Ca(wk)), and a projected velocity NGC 2281 v.sin i=40,100 km/s, while in (414) it is given a membership NGC 2281 probability of 91%. NGC 2287 Adopted cluster centre: star 102 (123). Reference (246) gives the NGC 2287 spectra: star 109 = HD 49333, B9IV/B7IIIn(He(wk)); star 116 = NGC 2287 HD 49024, B9IIIp(Hg-Mn). The proper motion study (187) gives NGC 2287 star 116 a membership probability of 6%. Stars 109 and 116 are NGC 2287 cited as blue stragglers in (123) and (114), respectively. Star NGC 2287 109 is also cited as a blue straggler in (281), where it is NGC 2287 given a spectrum B4p(He(wk)). NGC 2311 All the cluster parameters are from (8). NGC 2324 Star 168 (ref. 34) = 2668 (WEBDA), which appears as a straggler NGC 2324 in the diagrams of (34), has a membership probability of 0% NGC 2324 according to (265). The same reference gives star 59 a 75%. NGC 2324 Star 6=HD 53206, star 127=HD 289581 NGC 2345 The dereddened colour-magnitude diagram in (287) was examined. NGC 2353 Star 71=HD 55879 has a spectrum O9II(He(wk)) and may be a blue NGC 2353 straggler if it is a cluster member, but it is probable that NGC 2353 it belongs to the CMa OB1 association (135). NGC 2354 Adopted cluster centre: star 157 (ref. 104). Star 266 is an NGC 2354 eclipsing binary (241). NGC 2360 Stars 51 and 100 are cited as blue stragglers in (108) and (283). NGC 2360 The last reference also considers stars 1, 69, and 82 (WEBDA NGC 2360 numbers) as stragglers. Adopted cluster centre: star 46 (108). NGC 2383 Star 1=BD-20 1913 has a spectrum B0III (139). NGC 2420 Star 17 (WEBDA number) appears as a straggler in the diagrams of NGC 2420 (17) but is a non-member according to (408). Other membership NGC 2420 probabilities from the same reference: star R, 77%, star g, 90%, NGC 2420 star 2206a, 87%. Stars 1116, 2206a, and g are cited as blue NGC 2420 stragglers by (283) based on the photometry (34). NGC 2422 Reference (281) cites star 1=HD 60855 as a blue straggler of NGC 2422 spectrum B2IVe and projected velocity v.sin i=320km/s. The ubvy- NGC 2422 beta photometry (370) gives star 1 the following: v=5.684, NGC 2422 (b-y)=0.004, m1=0.042, c1=0.152, beta=2.554. Adopted cluster NGC 2422 centre: star 81 (373). NGC 2437 Diagrams from (257) and (373) were examined. Star 10 = NGC 2437 HD 61954, star 1 = HD 62000, star 2 = HD 62129. Spectra from NGC 2437 (184): A1II/III (star 1), B8IV/V (star 2), and B6Ib (star 10). NGC 2439 Adopted cluster centre: star 205 (432). Star 2=CD-31 4911 has a NGC 2439 spectrum B1.5Ib and is cited as a blue straggler in (281). This NGC 2439 may not be a true cluster (WEBDA). NGC 2447 Star 35=ADS 6339 is a binary (delta=0.5 mag, rho=0.7"). NGC 2451 The diagrams in (100) and (433) were examined. Star 175 is NGC 2451 HD 61831, star 283 is HD 63465. Adopted cluster centre: star NGC 2451 962 (433). The ubvy-beta study (115) casts doubt on the NGC 2451 physical reality of this cluster. Star 283 is cited as a blue NGC 2451 straggler in (230). Reference (184) gives the spectra B3V (star NGC 2451 175), and B2IV/V (star 283). NGC 2467 The dereddened colour-magnitude diagram in (129) was examined; NGC 2467 the authors suggest that this is a superposition of early-type NGC 2467 stars rather than a cluster. NGC 2477 The apparent cluster diameter is from (162). NGC 2506 The following membership probabilities are from (64): star 441, NGC 2506 42%, star 447, 94%, star 462, 71%, star 467, 91%, star 510, 88%, NGC 2506 star 571, 42%, star 691, 88%, star 769, 91%. Star 589 (264) = NGC 2506 3129 (WEBDA), which also appears as a straggler, is a non-member NGC 2506 according to (64). NGC 2516 Adopted cluster centre: star d in (90). Star A = HD 66194 = NGC 2516 V374 Carinae has a membership probability of 99% (223), and NGC 2516 a spectrum B2Vne/B3ne (127). This star is cited as a blue NGC 2516 straggler in (281) and (420), and is considered to be an NGC 2516 analogue of the straggler Theta Carinae in IC 2602 by (112) and NGC 2516 (423). According to (156), both components of this binary are NGC 2516 main-sequence stars, and would experience mass transfer before NGC 2516 abandoning this stage. NGC 2527 Star 213=HD 67097 has a spectrum A0V (254). NGC 2533 Star 52 (sp. B3) is a probable non-member according to (249). NGC 2533 The UBV photoelectric study (202) gives this star (B-V)=0.06. NGC 2539 Stars 423, 610, and 653 appear as stragglers but they are not NGC 2539 cluster members according to (242). NGC 2546 Star 544=HD 69067 (Ap), 682=HD 68450 (B0III), spectra from (184). NGC 2627 All cluster data except the apparent diameter are from (7). NGC 2632 = Praesepe. References (1) and (281) cite star 265 = HD 73666 = NGC 2632 40 Cancri as a blue straggler. Star 265 is a Si star (spectrum NGC 2632 A1IIIp(Si)s) according to (2), but this is not confirmed by NGC 2632 (11). Star 300=HD 73731=Epsilon Cnc has an spectrum Am(K/H/M= NGC 2632 A5/A6/F0) (2), and is a binary (5). Both stars are cluster NGC 2632 members (228). A spectroscopic study of the four straggler NGC 2632 candidates listed in (9) is presented in (11): besides star 265, NGC 2632 the other three stars are not included in the present catalogue, NGC 2632 since they rather seem located on the `blue hook.' According to NGC 2632 (11), stars 224 = HD 73618 and 265 are Am, star 348 = HD 73819 NGC 2632 is Ba-deficient, and star 50 = HD 73210 es metal-deficient. NGC 2632 Internal mixing does not seem to be here a plausible mechanism NGC 2632 to explain the stragglers (11). NGC 2658 All the cluster parameters except the apparent diameter are from NGC 2658 (6). NGC 2669 Star 24 = HD 75067 (sp. B8/9IV/V(n)) (184). Adopted cluster NGC 2669 centre: star 8 (422). Star 2 appears as a straggler but is a NGC 2669 non-member according to (224). NGC 2682 = M67. This cluster has a number of well-known blue stragglers, NGC 2682 a detailed spectral analysis of which can be found in (269). The NGC 2682 photometry listed in (352) was used; it includes all the stars NGC 2682 with a membership probability greater than 50% according to the NGC 2682 proper motion study (351). The adopted cluster centre is star NGC 2682 1023 of (351). All the stars with probability greater than 80% NGC 2682 are listed in our catalogue. Note that the WEBDA numbers are NGC 2682 the often-quoted Fagerholm numbers (e.g.: star 1284 = F190). NGC 2682 The following are the membership probabilities: star 145(94%), NGC 2682 277(93%), 740(87%), 751(96%), 752(95%), 821(89%), 856(90%), NGC 2682 968(95%), 975(90%), 977(93%), 984(95%), 997(93%), 1005(95%), NGC 2682 1031(91%), 1036(91%), 1066(90%), 1072(95%), 1082(99%), 1165 NGC 2682 (93%), 1183(95%), 1195(96%), 1263(89%), 1267(93%), 1273(91%), NGC 2682 1280(93%), 1284(95%), 1434(91%), 1440(94%), 1947(86%), 2204 NGC 2682 (83%). Most of these stars are also NGC 2682 catalogued as stragglers by (283). A possible relation between NGC 2682 the blue stragglers and the `clump' stars is discussed in (113). NGC 2682 In the IR study (319) of the five bluest stragglers, two of them NGC 2682 (1284 and 1434) are found to show infrared excesses that are NGC 2682 interpreted as signs of the presence of evolved companions (i.e. NGC 2682 they may be Algol-type binaries). In the case of 1284, the NGC 2682 binary character has received support from the discovery of NGC 2682 radial velocity variations, which have been interpreted (282) as NGC 2682 manifestations of a binary of period 4.18 days and eccentricity NGC 2682 0.205. This star is a good example in support of the mass NGC 2682 transfer theory to explain some stragglers (282). However, star NGC 2682 977 is above the magnitude limit that the same theory predicts, NGC 2682 although its membership is under discussion (269). Stars 1280 NGC 2682 and 1284 are small-amplitude pulsating variables of Delta Sct NGC 2682 type (153). In (268) it is shown that the spatial distribution NGC 2682 of the blue stragglers (strong central concentration) is similar NGC 2682 to that of the cluster binaries;an evolutionary relation between NGC 2682 the two populations is suggested (268). Stars 997 (410) and 1082 NGC 2682 (37) are X-ray sources; star 1082 is also a triple star, two NGC 2682 components of which would be blue stragglers (354). Several `red NGC 2682 stragglers' are pointed out in (118), and in (268) star F136 is NGC 2682 associated with an evolutionary stage related to the blue strag- NGC 2682 glers (it is a binary star).Through the determination of lithium NGC 2682 abundances on some stragglers, a form of mixing affecting their NGC 2682 external layers has been proposed (113). Star 984 would not be NGC 2682 an unresolved pair,but a single, `genuine' blue straggler (369). NGC 2682 These authors analyse high-resolution spectra of stragglers and NGC 2682 main-sequence turnoff stars, and find that their metallicities NGC 2682 and abundance ratios are not significantly different. Based on NGC 2682 arguments from hydrodynamical models of stellar collisions, they NGC 2682 claim that the upper limits for the lithium abundances of all NGC 2682 blue stragglers are consistent with a formation process without NGC 2682 mixing. In reference (239) is made a detailed analysis of the NGC 2682 spectroscopic binary and `red straggler' 1040 (ref. 352), and NGC 2682 it is proposed that it originated as a short-period binary and NGC 2682 evolved through a blue straggler phase to its present state. NGC 2682 According to (240), stars 975 and 1082 have hot subluminous NGC 2682 companions; this is confirmed for star 1082 in (412). NGC 2849 All cluster parameters are from (6). Only stars up to 2' from NGC 2849 the cluster centre were considered. From their colour-colour NGC 2849 diagrams, (236) conclude that stars 4 and 19 must be foreground NGC 2849 stars. NGC 3105 The dereddened colour-magnitude diagram of suspected members in NGC 3105 (137) was examined. NGC 3114 The apparent cluster diameter was taken from (363). In the NGC 3114 ubvy-beta photometric study (360) stars 8 (= 108 WEBDA), 9 (= NGC 3114 23), 14 (= 210), 15 (= 196), 16 (= 25), 18 (= 211), 61 (= 234), NGC 3114 and 124 (= 256) are considered to be blue straggler candidates NGC 3114 according to their position in the beta-c diagram: five of them NGC 3114 show peculiarities. The following spectra and membership NGC 3114 probabilities are from (155): star 23, B3V, 99%; star 33, B2.5V, NGC 3114 96%; star 149, B3III, 81%; star 180, B2Ve, 93%; star 196, B6V, NGC 3114 95%. Star 108, which also appears as a straggler, is not a NGC 3114 cluster member (155). NGC 3247 All the cluster parameters are from (6). NGC 3293 The dereddened colour-magnitude diagram in (401) was examined. NGC 3293 The adopted apparent diameter is from (401), and the adopted NGC 3293 centre is star 31. Star 1=HD 91824 (O7V(f)) is a probable NGC 3293 member of the Car OB1 association (401). NGC 3324 The dereddened colour-magnitude diagram in (73) was examined. NGC 3324 The apparent cluster diameter is also from (73). NGC 3496 Reference (13) observes spectroscopically three of the straggler NGC 3496 candidates listed in the earlier version of the catalogue (9): NGC 3496 stars 43, 115, and 117. They show low projected rotational NGC 3496 velocities and no specific spectral peculiarities. NGC 3532 Only the photoelectric colour-magnitude diagram of (133) was NGC 3532 examined. The cluster shows a remarkable concentration of its NGC 3532 more massive stars (133).The following membership probabilities NGC 3532 are from (222): star 105, 90%; star 420=HD 96059, 60%; star 449= NGC 3532 HD 96729, 91%; star 471=HD 96012, 35%; star 566=HD 96879, 62%. NGC 3532 Stars 115 and 409, which appear as stragglers in (133), are NGC 3532 non-members according to (222). Spectra: star 420, B9III (184); NGC 3532 star 449, B9IIIp (167); star 471, B8IV/V (184). References (1) NGC 3532 and (281) cite star 155 as a blue straggler. NGC 3680 Adopted cluster centre: star 31 (109). The ubvy study (116) NGC 3680 cites stars 3, 29, 33 and 56 as blue stragglers and stars 20 and NGC 3680 34 as `red stragglers,' although stars 3, 29 and 56 are probable NGC 3680 non-members. The CCD photometry (16) considers stars 29 and 33 NGC 3680 as probable cluster members, and stars 53 and 56 as likely non- NGC 3680 members. An important number of binaries around the turnoff NGC 3680 is thought to be present (16). NGC 3766 Adopted cluster centre: star 20 (368). In (281) star 2 = NGC 3766 HD 100856 (sp. B1.5III) is cited as a blue straggler. NGC 3960 Only the photoelectric colour-magnitude diagram of (192) was NGC 3960 examined. NGC 4103 All cluster parameters are from (8). NGC 4349 Adopted cluster centre: star 151 (256). The apparent cluster NGC 4349 diameter is from (162). In (281) star 131 = DM-61 3143 is cited NGC 4349 as a blue straggler. NGC 4439 The apparent cluster diameter is from (288). NGC 4755 = Kappa Crucis cluster. The colour-magnitude diagram with NGC 4755 probable members in (94) was examined. The apparent cluster NGC 4755 diameter is from (162). Star F = CPD-59 4564 = BW Crucis has a NGC 4755 spectrum B2III (358), a membership probability of 92% (225), and NGC 4755 is a beta Cephei variable (191). NGC 4815 Only straggler candidates inside a radius of 3' around the centre NGC 4815 of coordinates have been considered. NGC 5168 Star 1=CPD-60 4735 has a luminosity class III (288). NGC 5281 Star 1 is cited as a blue straggler in (281). NGC 5460 Star 66, which appears as a straggler, is a non-member (82). NGC 5617 All cluster data except the apparent diameter are from (7). NGC 5822 The following spectra are from (184): star 2115=HD 133136 (B8II), NGC 5822 star 2222=HD 133279 (A2IV/V), star 2261=HD 133181 (A0II/IV), NGC 5822 star 3249=HD 132922 (B9IV/V). NGC 5823 Adopted cluster centre: star 37 (48). Only the photoelectric NGC 5823 data in (48) were taken into account. NGC 5999 All the cluster parameters except the apparent diameter are from NGC 5999 (8). The diagram up to 2.5' from the cluster centre was NGC 5999 examined. NGC 6025 Star 1=HD 143348 (B3IVe) is cited as a blue straggler in (281). NGC 6067 Only the photoelectric colour-magnitude diagram of (385) was NGC 6067 examined. Star 264=DM-53 07347, star 267=DM-53 07353, NGC 6067 star 286=DM-53 07384. The following spectra are from (237): NGC 6067 264(B5V/III), 266(B2III), 286(B8IV). Star 267 is cited as a NGC 6067 blue straggler in (281). NGC 6124 Star 8 is a cluster member according to (312). NGC 6134 All the cluster parameters except the apparent diameter were NGC 6134 taken from (8). NGC 6167 The apparent cluster diameter is from (293). NGC 6192 The dereddened colour-magnitude diagram of (226) was examined. NGC 6200 The dereddened V vs. (U-B) diagram of (138) was examined. NGC 6231 Star 858 (WEBDA) = HD 152233 (sp. O6IIIfp,variable?) is cited as NGC 6231 a blue straggler in (281). NGC 6242 The apparent cluster diameter was taken from (288). NGC 6268 Selected angular diameter from (259). NGC 6281 Selected angular diameter from (259). Star 9 (WEBDA) is cited as NGC 6281 a straggler in (1), (281), and (302), but it is a non-member NGC 6281 according to (124). NGC 6404 Only straggler candidates inside a radius of 2' around the centre NGC 6404 of coordinates have been considered. NGC 6416 Star 367=HD 160826 has spectrum B9V (184). NGC 6425 Adopted cluster centre: star 54 (ref. 386). Star 50=HD 318301 is NGC 6425 a Be star (260). NGC 6475 Only the colour-magnitude diagram based on the photoelectric data NGC 6475 of (229) was examined. Adopted cluster centre: star 65 (229). NGC 6475 Star 26=HD 162374 is cited as a blue straggler in (112), where NGC 6475 it is found to be similar to Theta Carinae. In (1) and (281) NGC 6475 stars 26 and 56=HD 162586 are also cited as blue stragglers. NGC 6475 In (3) these stars are given the spectra B6V and B8V. Membership NGC 6475 probabilities based on proper motions (88): star 26, 53%; star NGC 6475 56, 57%. Probability based on radial velocities (152): star 56, NGC 6475 92%. This star is also a visual binary (delta=0.0 mag,rho=0.3") NGC 6475 (179). The stragglers of this cluster were studied spectro- NGC 6475 scopically by (13). NGC 6494 Only the photoelectric data of (181) were examined. Stars 1= NGC 6494 HD 163245 and 12 have spectra A4V (89) and A0V (180). The proper NGC 6494 motion study (353) assigns these stars the membership probabil- NGC 6494 ities 88% and 98%. NGC 6514 Selected angular diameter from (259). NGC 6530 Selected angular diameter from (259). NGC 6583 Only straggler candidates inside a radius of 2.5' around the NGC 6583 centre of coordinates have been considered. NGC 6611 Selected angular diameter from (259). The dereddened colour- NGC 6611 magnitude diagram in (430) was examined. NGC 6631 Only straggler candidates inside a radius of 1' around the centre NGC 6631 of coordinates have been considered. NGC 6633 According to the proper motion study (350), star 32=HD 169959 has NGC 6633 a probability membership of 90%, and star 66=HD 170054 has 70%. NGC 6633 Star 159=HD 170563 is a cluster member according to (178). NGC 6633 References (1), (179), (185), and (277) cite stars 32 and 159 as NGC 6633 blue stragglers. In (1) the following spectra and projected NGC 6633 velocities are given: star 32, A0III, v.sin i<40km/s; 159, NGC 6633 B6IVp(Si), v.sin i<20km/s. Star 66 has a spectrum B6IV (245). NGC 6633 Star 155 is HD 170472. Reference (13) also studies spectro- NGC 6633 scopically the stragglers 32 and 66. NGC 6664 The Stromgren photometry (361) cites stars 53 and 61 as blue NGC 6664 stragglers. NGC 6705 The colour-magnitude diagram in (374) was examined. It displays NGC 6705 stars with p>=90% according to the proper motion study (277). NGC 6705 Star 1095 is given in (277) a membership probability of 61%. NGC 6705 Adopted cluster centre: star 1066 (ref. 277). The apparent NGC 6705 diameter is from (374). References (1) and (281) cite star 1095 NGC 6705 as a blue straggler; in (1) this star is given a spectrum B3p. NGC 6709 Stars 235 and 293 appear on the main sequence rather than in the NGC 6709 straggler area according to the photoelectric data (181). How- NGC 6709 wever, when the photographic data of the same reference are NGC 6709 plotted, stars 298, 301, and 335 appear as stragglers. Member- NGC 6709 ship probabilities by (163): star 235, 67%; star 293, 40%. NGC 6709 Star 277 also appears as a straggler in (379), but it is not a NGC 6709 cluster member according to (163). NGC 6791 The red limit of the straggler area is (B-V)=0.8. According to NGC 6791 (227), stars 96, 63, and 106 are probable cluster members. NGC 6791 Stars 63 and 106 are cited as blue stragglers in (151). In (227) NGC 6791 attention is drawn to several `red stragglers' that are probable NGC 6791 cluster members. The CCD study (209) mentions the existence of NGC 6791 a possible FK Comae star. Spectra from (227): star 39, G0V; NGC 6791 star 45, F2IV; star 102, F2IV; star 67, G2V; star 129, F9V; star NGC 6791 63, G0V. Star 123 = V6 (216) is an EW variable (216); the NGC 6791 authors also discover two EW variables (V1 and V7) that they NGC 6791 mark as stragglers: both stars have mean (B-V) colours redder NGC 6791 than our limit of 0.8. NGC 6811 Star 147 has a membership probability of 97% (347). NGC 6819 The apparent cluster diameter is from (162). Several stragglers NGC 6819 are pointed out in (25). Membership probabilities from (349): NGC 6819 star 32, 88%; star 35, 90%; star 36, 92%; star 40, 81%; star 55, NGC 6819 66%; star 59, 86%; star 65, 89%; star 70, 92%; star 96, 49%; NGC 6819 star 103, 57%; star 118, 77%; star 6044, 33%. Attention is NGC 6819 drawn in (340) on several clump stars that appear to be more NGC 6819 massive than the turnoff stars: it is suggested that they are NGC 6819 the descendants of blue stragglers. NGC 6834 Only the photoelectric data of (181) were examined. Star 5 is NGC 6834 cited as a blue straggler in (185),but in (394) it is con- NGC 6834 sidered to be a normal evolved star that appears bluer because NGC 6834 of differential reddening. Star 5 = HD 332844 has a spectrum NGC 6834 F2V (391) and star 10 has a spectrum B5V (180). NGC 6866 Only the photoelectric data of (181) were examined. NGC 6871 Only the photoelectric data of (181) were examined. Star 1 = NGC 6871 HD 190918 = V1617 Cygni is a WR, double star of components NGC 6871 near the cluster turnoff (87). Star 4 = HD 190864 (O7IIIf) NGC 6871 is cited as a blue straggler in (281). NGC 6913 The apparent cluster diameter was taken from (162). The de- NGC 6913 reddened diagram of (202) was examined. NGC 6939 Membership probabilities from (439): star 7, 98%; star 13, 97%; NGC 6939 star 87, 86%; star 94, 99%. Stars 7 and 13 (339), and 59 and NGC 6939 349 (WEBDA) are cited as straggler candidates in (52) and (283). NGC 6939 Star 59 is also cited as a blue straggler in (151), although is NGC 6939 probably a non-member. NGC 6940 The following membership probabilities are from (348): star 50, NGC 6940 83%; star 70, 90%; star 153, 90%; star 172=HD 334735, 89%; NGC 6940 star 175, 85%; star 179=HD 334755, 83%. Some spectra: star 50, NGC 6940 F0 (415); star 70, F5II-III (428); star 153, A0 (243); star 175, NGC 6940 A5 (243); star 179, A0 (243). Stars 70 and 77 are cited as blue NGC 6940 stragglers in (151). NGC 7039 According to (362) there would be two clusters: the first one at NGC 7039 700 pc, and the second one at 1500 pc. NGC 7063 Only the photoelectric data of (181) were examined. NGC 7082 The apparent cluster diameter was taken from (169). Star 120 NGC 7082 seems to appear as a straggler only in the V vs. (U-B) diagram. NGC 7160 Star 3=HD 208440 has a spectrum B1V (180). NGC 7243 Identification chart in (33); Adopted cluster centre: star 1. NGC 7243 In (176) star 370 is given the following: v=9.95, (b-y)=0.052, NGC 7243 m1=0.093, c1=0.528, beta=2.742, spectrum A0Vp. It is a cluster NGC 7243 a membership probability of 96% (244). NGC 7788 Probability memberships according to (438): star 10, 62%; star NGC 7788 102, 54%; star 108, 61%. NGC 7789 The first selection was based on the photometric study (49), NGC 7789 which is complete (it includes stars up to 7.5' from the cluster NGC 7789 centre); the star designations are from (235). A further NGC 7789 selection took into account the detailed membership analysis for NGC 7789 each blue straggler (45), and the proper-motion study (279). NGC 7789 The following membership probabilities are from (279): star 88, NGC 7789 98%; star 168, 77%; star 192, 52%; star 197, 46%; star 282, 97%; NGC 7789 star 316, 98%; star 342, 96%; star 371, 98%; star 409, 53%; star NGC 7789 410, 78%; star 453, 98%; star 651, 98%; star 677, NGC 7789 53%; star 696, 98%; star 746, 98%; star 753, 95%; NGC 7789 star 861, 88%; star 1047, 96%; star 1097, 70%; star 1211, 97%. NGC 7789 Star 1211 seems to be on the magnitude limit that the mass NGC 7789 transfer theory predicts, and star 677 is above that limit (47). NGC 7789 An extensive halo of blue stragglers was described in (274), but NGC 7789 these stars would belong to the field (406): at most, the strag- NGC 7789 glers have the same radial distribution that the cluster giants. NGC 7789 In the photometric ubvy study of 28 blue stragglers (406) there NGC 7789 appears to be no peculiar stars among them, except star 1211 NGC 7789 (sp. Ap); in general, the objects seem to have evolved from the NGC 7789 ZAMS. A spectroscopic study of eight, confirmed stragglers (364) NGC 7789 shows deficiency of surface Mg and low projected rotational NGC 7789 velocities. Star 753 is a Delta Scuti variable (star V10 in ref. NGC 7789 189). In (382) this cluster is given E(B-V)=0.31 and age= NGC 7789 1.6 Gyr. NGC 7790 Star 586 is cited as a blue straggler in (281), and has a NGC 7790 spectrum B2II-IV (231). Probability memberships according to NGC 7790 (438): star 586, 70%; star 810, 66%; star 1360, 72%. Pismis 2 Only straggler candidates inside a radius of 3' around the centre Pismis 2 of coordinates have been considered. Pismis 7 All cluster parameters are from (7). Pismis 18 All the cluster parameters are from (8). The diagram of stars Pismis 18 up to 3' was examined. Pleiades Adopted cluster centre: star 1432=HD 23630, which has a spectrum Pleiades B8IIIe (46), a projected velocity v.sin i=230 km/sec (275), and Pleiades it is cited as a blue straggler in (281). Roslund 3 The dereddened colour-magnitude diagram in (399) was examined. Roslund 3 Adopted cluster centre: star 41 in (399). Stars A=HD 350990 and Roslund 3 B=HD 350991 have spectra B6IIIn and are cluster members (399). Roslund 3 The author assigns the unusual positions of these stars in the Roslund 3 colour-magnitude diagram to high rotation velocities. Ruprecht 36 Star 1=CD-26 5011 appears as a straggler in (421), but it is a Ruprecht 36 non-member according to that reference. Ruprecht 46 The red limit of the blue straggler area is (V-I)=0.78. Ruprecht 67 Adopted cluster centre: star 10 in (291). Ruprecht 75 All cluster parameters are from (7). Only stars up to 2' from Ruprecht 75 the centre were considered. Ruprecht 79 The dereddened colour-magnitude diagram in (425) was examined. Ruprecht 79 Star designations and adopted cluster centre (star J = star 3 Ruprecht 79 in WEBDA) are from (166). Could not be a true cluster (WEBDA). Ruprecht 98 Star 1=HD 104013 has a spectrum A0V (184). Adopted cluster Ruprecht 98 centre: star 6 in (288). Ruprecht 115 Selected angular diameter from (259). Ruprecht 119 Selected angular diameter from (259). Ruprecht 120 Selected angular diameter from (259). Stock 1 Cluster age taken from (306). Star 11=HD 184762 has a spectrum Stock 1 B8, and star 56=HD 184121 has a spectrum B7 (376). Stock 2 Adopted cluster centre: star 69 in (232). Star 2=HD 13088 Stock 2 (member?), star 161=HD 14172 (non-member?), star 164=HD 14183 Stock 2 (member?), according to (232); their spectra are A1V, A2V, A0V, Stock 2 respectively (273). Stock 13 Star 1=HD 97597 has a spectrum B2II/III (184). Stock 13 Adopted cluster centre: star 4 in (292). Stock 24 The diagram for stars inside a radius of 3' around the centre of Stock 24 coordinates was examined. Tombaugh 1 The V vs (B-V) diagram in (395) and the V vs. (V-I) diagram in Tombaugh 1 (63) were examined. Star 2 is cited as a probable straggler in Tombaugh 1 (395). Tombaugh 2 Only straggler candidates inside a radius of 2' around the centre Tombaugh 2 of coordinates have been considered. Trumpler 5 Only straggler candidates inside a radius of 8' around the centre Trumpler 5 of coordinates have been considered. The red limit of the blue Trumpler 5 straggler area is (B-V)=0.87. Trumpler 9 Star 2=DM-25 5278 appears to have a small reddening, is a non- Trumpler 9 evolved star (beta=2.784), and is a non-member according to (421) Trumpler 10 Adopted cluster centre: star 9 in (258). Star 2=HD 75387 has a Trumpler 10 spectrum B2V (184). Trumpler 11 The adopted age is a mean value of the range determined by (341). Trumpler 11 The adopted apparent diameter is the selected diameter given by Trumpler 11 (259). Trumpler 14 The dereddened colour-magnitude diagram was examined (128). Trumpler 14 The selected angular diameter is from (259). Trumpler 16 The dereddened colour-magnitude diagram was examined (128). Trumpler 16 The cluster apparent diameter was taken from (398). Trumpler 18 Star 75=HD 97223 has a spectrum B3V (184). Trumpler 27 The dereddened colour-magnitude diagram was examined (386). vdB-Hagen 99 The dereddened colour-magnitude diagram in (238) was examined.