3 Blanco 1 Cluster coordinates previously published do not coincide with 3 the maximum of the projected stellar density. Therefore, 3 the new cluster centre is shifted by 0.36 deg to the SW. 4 Alessi 20 Cluster coordinates previously published do not coincide with 4 the maximum of the projected stellar density. Therefore, 4 the new cluster centre is shifted by 0.18 deg to the NE, 4 to the group of B5 - A0 stars. 9 NGC 146 Cluster projected onto the Cas OB2 association in the 9 background. The stars with r>0.13 deg show motions which 9 are different from the cluster proper motion. 13 Alessi 1 For this cluster, Dias et al. give d=302 pc, E(B-V) = 0.09, 13 log t = 8.20. The results differ from our findings (d=800 pc, 13 E(B-V) = 0.10, log t = 8.85). Probably, they include three 13 brightest stars in this region in the age determination, 13 but from their kinematics, these are not members. Possibly, 13 there are two clusters projected into each other. 14 NGC 381 Cluster projected onto the Cas OB1 association in the 14 background. The stars with r>0.10 deg show motions which 14 are different from the cluster proper motion. 17 NGC 457 Due to the brightest members, i.e. two Post-MS stars F0Ia 17 and B6Ib, the cluster is expected to be younger by 17 diff(log t)= 0.05-0.1. Nevertheless, we failed to find 17 an isochrone which is consistent with all cluster members. 18 NGC 581 Compared to the estimates of Loktin et al., E(B-V) is 18 increased from 0.382 mag to 0.39 mag. 19 NGC 637 According to the cluster CMD, E(B-V) is decreased from 19 0.634 mag (Loktin et al.) to 0.61 mag. 20 NGC 581 There are no members within the Evolved MS. The age was 20 estimated by isochrone fitting, manually. 23 Collinder 463 The reddening seems to be variable over the cluster area. 23 Also, the estimates derived by different authors range from 23 E(B-V) = 0.0 (Lynga) to 0.26 (Loktin). We find E(B-V) = 0.30. 28 Stock 2 In order to keep a symmetric form of the cluster, its centre 28 (usually referred to in the past) is shifted by 0.22 deg 28 to the S. 29 NGC 864 In order to avoid a possible influence of the neighbouring 29 (h Per) chi Per cluster, the proper motion, RV, and log t are 29 determined by use of stars in the core, only. Compared to the 29 estimates of Loktin et al., E(B-V) is decreased from 0.58 mag 29 to 0.48 mag. 30 NGC 884 In order to avoid a possible influence of the neighbouring 30 (chi Per) h Per cluster, the proper motion, RV, and log t are 30 determined by use of stars in the core, only. 32 Stock 7 The reddening is variable. Compared to Loktin et al., 32 (Mark 6) E(B-V) is decreased from 0.61 mag to 0.56 mag. 39 Collinder 33 The luminosity classes of some bright stars identified as 39 cluster members do not follow the cluster CMD. Possibly, a 39 a group of co-moving stars. 42 Melotte 20 In order to keep a symmetric form of the cluster, its centre 42 (alpha Per) is shifted to (RA, Dec) = (3.433 h, 49.12 deg). There are 42 3 bright stars (V=1.803,4.308,4.686; B-V=+0.527,-.062, -.107) 42 with a photometric probability of P_ph = 1 which are located 42 along the isochrone defined by fainter cluster stars. A 42 relatively low kinematic probability (P_kin= 5, 13, 51%) 42 results from formally small mean errors in proper motions 42 which are used for the determination of kinematic 42 probabilities. The mean errors could be underestimated in the 42 Hipparcos catalogue. Otherwise, we should assume a larger 42 internal motion of the cluster stars. 46 IC 348 The cluster is projected onto the Per OB2 association. The 46 reddening is variable. Compared to the estimates of Loktin 46 et al., E(B-V) is decreased from 0.93 mag to 0.82 mag. 46 From the grid of Pre-MS isochrones, there are some indications 46 that the derived age may be overestimated. 47 Melotte 22 There are 9 bright (V<5.5) stars located in the cluster core 47 (Pleiades) (dr<=r_core), but only 4 of them have P_kin & P_ph >=61: 47 V B-V P_ki P_ph 47 +2.870 -0.062 94.30 100.00 47 +3.622 -0.070 49.18 100.00 47 +3.706 -0.092 89.75 100.00 47 +3.870 -0.055 61.04 100.00 47 +4.164 -0.047 90.17 004.39 47 +4.293 -0.091 51.56 100.00 47 +5.048 -0.079 11.39 100.00 47 +5.440 -0.065 40.95 100.00 47 +5.447 -0.038 88.80 100.00 47 It is possible that the mean errors of proper motions and 47 photometric data used for computing the probabilities 47 are underestimated in the original catalogues. Otherwise, 47 we should assume an internal spread of the kinematical and 47 photometric parameters in the cluster. 49 NGC 1502 The reddening is variable. Compared to the estimates of 49 Loktin et al., E(B-V) is decreased from 0.76 mag to 0.65 mag. 50 NGC 1528 Compared to the estimates of Loktin et al., E(B-V) is 50 decreased from 0.26 mag to 0.24 mag. 53 Platais 3 Compared to the estimates of Platais et al. (1998) based on 53 Hipparcos parallaxes, the distance of the cluster is 53 increased from 161 pc to 200 pc. 54 NGC 1647 Compared to the estimates of Loktin et al., E(B-V) is 54 decreased from 0.37 mag to 0.32 mag. 54 The cluster has a complex CMD and possibly consists of two 54 overlapping clusters with different reddenings, 54 E(B-V) = 0.37 mag and E(B-V) = 0.32 mag. 58 Berkeley 14A According to Dias et al., Berkeley 14 at a distance of 58 5500 pc and E(B-V)=0.52 mag is located in this sky area. Due 58 to the relatively bright magnitude limit, such a cluster can 58 not be identified with the ASCC-2.5 data. Instead, a nearer 58 (at 1100 pc) and larger (r=0.74 deg) cluster was found. 60 NGC 1746 There are three clusters in this area which are often mixed 60 up: 60 NGC 1746 5.064 h +23.77 d 60 NGC 1750 5.065 h +23.66 d 60 NGC 1758 5.076 h +23.80 d 60 We decided to study this area as a single complex with 60 d = 760 pc, E(B-V)=0.25. The complex is named after the 60 cluster NGC 1746 located near the common center. 61 Platais 4 Since the rich cluster NGC 1746 is situated 1.7 deg to 61 the N and its members contaminate the area of the cluster, we 61 assume a radius of 1.25 deg for the cluster Platais 4. 62 NGC 1778 Compared to the estimates of Loktin et al., E(B-V) is 62 increased from 0.34 mag to 0.35 mag. 66 NGC 1893 Compared to the estimates of Loktin et al., E(B-V) is 66 decreased from 0.58 mag to 0.40 mag. 68 Collinder 65 The cluster has different coordinates in the Lund catalogue 68 (RA, Dec = 5.732 h, +16.10 d) and in Dias et al. 68 (RA, Dec = 5.435 h, +16.70 d). We derived a cluster centre at 68 (RA, Dec) = (5.435 h, +15.70 d). 72 Collinder 69 In order to keep a symmetrical form of the cluster, its 72 centre is shifted by 0.23 deg to the S. 74 NGC 1976 The cluster is younger than the age derived from the 74 Trapezium Turn-off point. It is a very difficult case for the 74 applied member selection pipeline: 74 From six bright (V<6.7) Trapezium stars only one has both 74 probabilities P_kin & P_ph >=61. 74 V B-V P_ki P_ph 74 5.018 -0.036 04.12 00.27 74 5.068 -0.023 19.66 00.56 74 5.802 -0.239 00.79 94.84 74 6.206 -0.123 69.38 100.00 74 6.538 -0.020 57.78 02.73 74 6.710 +0.070 57.81 00.66 82 NGC 2099 The Turn-off point at V = 12.5 (given in literature) 82 cannot be observed with the ASCC-2.5 data. A few most 82 probable and bright members yield a too young age 82 (log t = 8.29) for the cluster. Therefore, the age estimate 82 of log t = 8.54 by Loktin et al. and the corresponding 82 isochrone are accepted. 83 Basel 11B There is some confusion with the published data on the 83 clusters Basel 11B and Basel 11A (the cluster 131 in our 83 sample): 83 Basel 11B Basel 11A 83 RA, Dec (J2000) ===> 5.970 h,+21.97 d 7.285 h,-13.97d 83 d(pc),E(B-V),logt(Lynga) 1500, - ,8.30 1514,0.000,8.506 83 d(pc),E(B-V),logt(Loktin) - , - , - 1692,0.315,7.816 83 d(pc),E(B-V),logt(Dias) 1692,0.315,7.816 1520,0.000,8.30 83 From our findings: 83 d(ps),E(B-V),log t 1500,0.10, 8.82 1500,0.18 ,7.43 84 NGC 2129 The reddening is variable. Compared to the estimates of 84 Loktin et al., E(B-V) is increased from 0.65 mag to 0.74 mag. 85 NGC 2143 There are no stars in the Evolved MS. Therefore, log t 85 was determined manually. 89 NGC 2184 Dubious cluster, possibly seen through a hole in the 89 interstellar matter. 90 NGC 2186 Compared to the estimates of Loktin et al., E(B-V) is 90 decreased from 0.27 mag to 0.26 mag. 91 Platais 6 An increase of the radial density at r > 1.57 degree is 91 caused by variable reddening and contamination by 91 neighbouring clusters. 93 Collinder 89 The published coordinates of the cluster centre seem to be 93 incorrect. Therefore, the cluster centre is shifted by 93 0.48 deg to the SE. 95 NGC 2232 There is confusion with cluster coordinates in different 95 catalogues: Lynga - (RA, Dec) = (6.467 h, -4.85 d), 95 Dias - (RA, Dec) = (6.454 h, -4.76 d). 95 From our determinations: (RA, Dec) = (6.465 h, -4.80 d). 98 NGC 2244 Compared to the estimates of Loktin et al., E(B-V) is 98 decreased from 0.467 mag to 0.40 mag. 102 NGC 2251 The CMD is not sufficiently accurate. The age estimate with 102 the brightest and most probable members yields a too young 102 age (log t = 7.95) for the cluster. Therefore, the age 102 derived by Loktin et al. (log t = 8.43) and the corresponding 102 isochrone were used. 105 Collinder 107 No cluster could be found with ASCC-2.5 data at the 105 published coordinates. On the other hand, there is a compact 105 group of a few B stars, 0.23 deg to the SE where a cluster 105 can be located. 106 Collinder 110A The published coordinates of the centre of Collinder 110 106 seem to be wrong and are, therefore, shifted by 0.15 deg to 106 the E. The published distance and reddening of d=1500 pc and 106 E(B-V)=0.50 mag seem to be overestimated. Our determinations 106 yield d=450 pc, E(B-V)=0.32 mag. Probably, a new cluster. 115 Collinder 121 The cluster is projected onto the central region of the 115 Collinder 121 association, but it is at a distance twice 115 as large as the distance of the association (see, also, 115 Eggen O.J, 1981ApJ...247..507E). 115 There is confusion with cluster coordinates in different 115 catalogues: Lynga - (RA, Dec) = (6.903 h, -24.42 d), 115 Dias - (RA, Dec) = (6.939 h, -24.73 d). 115 From our determinations: (RA, Dec) = (6.912 h, -24.30 d). 122 NGC 2343 There are different ages published for this cluster: 122 Loktin et al. - log t = 7.10 122 Lynga - log t = 8.23. 122 From our determinations: log t = 7.89 123 NGC 2345 Compared to the estimates of Loktin et al., E(B-V) is 123 increased from 0.62 mag to 0.68 mag. 126 Collinder 132 The published coordinates of the cluster are not correct and 126 therefore, shifted by 0.52 deg to the SW. 128 NGC 2353 The revised age of log t = 7.05 differs considerably from 128 the estimates of Loktin et al. (log t=7.97). Possibly, these 128 authors omitted (unjustified) the brightest member from 128 the age determination. 131 Basel 11A There is some confusion with the published data on the 131 clusters Basel 11A and Basel 11B (see the corresponding note 131 to the cluster 83 Basel 11B). 133 Collinder 135 The published coordinates of the cluster are not correct and 133 therefore, shifted by 0.36 deg to the S. 136 Collinder 140 There is confusion with cluster coordinates in different 136 catalogues: Lynga - (RA, Dec) = (7.387 h, -32.03 d), 136 Dias - (RA, Dec) = (7.407 h, -31.85 d). 136 From our determinations: (RA, Dec) = (7.388 h, -32.06 d). 138 NGC 2383 Our age estimate of log t = 8.65 is in agreement with the 138 presence of K giants in the CMD. The blue star with V = 10 138 used by Loktin et al. for the age determination 138 (log t = 7.17) belongs to the neighbouring young 138 cluster NGC 2384. 139 NGC 2384 See note to 138 NGC 2383. 142 Bochum 5 This cluster is missing in Dias et al. 142 The CMD, age estimate and spectral classes of members suit 142 badly each other. Possibly, this is a group of co-moving 142 stars. 143 Bochum 4 This cluster is missing in Dias et al. 150 Melotte 71 The Turn-off point is fainter than the limiting magnitude of 150 the ASCC-2.5. The age estimate by Loktin (log t = 8.37) and 150 the corresponding isochrone are adopted. 157 NGC 2432 At the published coordinates no cluster could be identified 157 with the ASCC-2.5 data. The cluster center is shifted 157 by 0.12 deg to the SE, where two B stars are located. One of 157 them has RV measured and according to Dias et al., belongs 157 to the cluster. 159 NGC 2451A The clusters are overlapping each other, their CMDs are 162 NGC 2451B mutually contaminated. In order to keep a symmetric form of 162 the cluster, the center of NGC 2451A is shifted by 0.40 deg 162 to the SW. 173 Trumpler 7 Compared to the estimates of Loktin et al., E(B-V) is 173 decreased from 0.25 mag to 0.19 mag. 178 NGC 2506 The Turn-off point is fainter than the limiting magnitude of 178 the ASCC-2.5. The age estimate by Loktin (log t = 9.05) and 178 the corresponding isochrone are adopted. 188 Ruprecht 56 Possibly, this is a stellar group. 201 NGC 2632 Due to proper motion errors underestimated in the original 201 (Praesepe) catalogue and/or intermal motion, a complete selection of 201 cluster members is difficult. 204 Mamajek 1 We could not find an isochrone which would suit for all 204 kinematic members. Therefore, the age (log t = 6.90) is 204 taken from Dias et al. 209 NGC 2669 There are two clusters close to each other in this area: 209 NGC 2669 8.773 h -52.95 d 209 vdB-Hagen 52 8.775 h -52.90 d. 209 We could not separate them in neither diagram and therefore, 209 consider them as a single complex with 209 d = 1046 pc, E(B-V)=0.18 as given by Loktin. 212 NGC 2682 The Turn-off point is fainter than the limiting magnitude of 212 the ASCC-2.5. There are only a few brighter blue stragglers 212 which are the most probable cluster members. The age 212 estimate by Loktin (log t = 9.41) and the corresponding 212 isochrone are adopted. 216 Platais 8 Compared to Platais et al., the cluster radius is decreased 216 from 7.9 deg to 3 deg to avoid a contamination by 216 surrounding clusters. The distance is increased to 150 pc, 216 instead of 132 pc estimated by Platais et al. 218 Platais 9 Compared to the estimates of Platais et al. based on 218 Hipparcos parallaxes, the distance of the cluster is 218 increased from 174 pc to 200 pc. 219 vdB-Hagen 66 Compared to Dias et al., E(B-V) is decreased from 0.40mag 219 to 0.30 mag. 223 Turner 5 According to Dias et al., a cluster at a distance of 223 2300 pc and E(B-V)=0.31 mag is located in this sky area. Due 223 to the relatively bright magnitude limit, such a cluster can 223 not be identified with the ASCC-2.5 data. Instead, a nearer 223 (at 400 pc) cluster at 0.30 deg to the NW was found. 227 Ruprecht 82 The Turn-off point is fainter than the limiting magnitude of 227 the ASCC-2.5. The age from the Lynga catalogue (log t = 8.50) 227 and the corresponding isochrone are adopted. 231 Pismis 16 Compared to the estimates of Loktin et al., E(B-V) is 231 increased from 0.56 mag to 0.61 mag. 233 Ruprecht 85 No cluster can be seen at coordinates previously published. 233 The cluster center is shifted by 0.10 deg to the N. 234 NGC 3114 The brightest proper motion members are probably, 234 co-moving stars. 235 Loden 143 Cluster distance and E(B-V) were determined with the two 235 members F3 Ib and O9.5 IAB/B. The age was estimated by 235 isochrone fitting, manually. 241 NGC 3228 There are different distances and reddenings published 241 for this cluster: 241 Loktin et al. - d = 806 pc, E(B-V) = 0.13 mag 241 Lynga - d = 499 pc, E(B-V) = 0.03 mag. 241 Our findings confirm the Lynga results. 243 IC 2581 Compared to the estimates of Loktin et al., E(B-V) is 243 increased from 0.415 mag to 0.45 mag. 248 Collinder 223 The cluster has different coordinates in different 248 catalogues: Lynga - (RA, Dec) = (10.508 h, -59.82 d), 248 Dias - (RA, Dec) = (10.538 h, -60.02 d), 248 From our determinations: (RA, Dec) = (10.538 h, -60.02 d). 249 Ruprecht 90 No cluster could be identified at the coordinates published: 249 Lynga - (RA, Dec) = (10.514 h, -58.23 d), 249 Dias - (RA, Dec) = (10.517 h, -58.45 d), 249 From our determinations: (RA, Dec) = (10.530 h, -58.24 d). 251 Loden 153 The angular distance between the clusters Loden 153 and 253 NGC 3293 NGC 3293 is 0.18 deg. Underestimates of their sizes are 253 therefore, possible. 259 IC 2602 An decrease of the stellar density is observed in the cluster 259 core where the brighter stars are located. This indicates a 259 gap of Tycho-2 stars in cluster area. 259 The brightest star (V = 2.7) has P_ki = 4 % and is not used 259 for the age determination. Fainter stars follow the isochrone 259 well. 262 Collinder 228 The reddening is variable. Compared to Loktin et al., 262 E(B-V) decreased from 0.34 mag to 0.26 mag. 263 Trumpler 14 The reddening is variable. Compared to Loktin et al., 263 E(B-V) decreased from 0.50 mag to 0.45 mag. 264 Trumpler 15 The reddening is variable. Compared to Loktin et al., 264 E(B-V) decreased from 0.64 mag to 0.45 mag. 265 Trumpler 16 The reddening is variable. Compared to Loktin et al., 265 E(B-V) decreased from 0.535 mag to 0.52 mag. 278 Feinstein 1 No cluster could be identified at the coordinates published. 278 The cluster center is shifted by 0.16 deg to the E. 278 Compared to the Lynga data, E(B-V) is increased from 0.40 mag 278 to 0.42 mag. 279 vdB-Hagen 111 The age estimate could not be performed properly with our 279 usual algorithm. Therefore, the age was estimated by 279 isochrone fitting, manually. 280 Loden 309 There is confusion with cluster coordinates in different 280 catalogues: Lynga - (RA, Dec) = (11.158 h, -60.63 d), 280 Dias - (RA, Dec) = (11.179 h, -60.38 d). 280 From our determination:(RA, Dec) = (11.161 h, -60 58 d). 281 NGC 3572 Compared to the estimates of Loktin et al., E(B-V) is 281 decreased from 0.39 mag to 0.34 mag. 289 Ruprecht 164 The age estimate could not be performed properly with our 289 usual algorithm. Therefore, the age was estimated by isochrone 289 fitting, manually. 291 Loden 402 The age estimate could not be performed properly with our 291 usual algorithm. Therefore, the age was estimated by isochrone 291 fitting, manually. 292 IC 2994 There is some confusion with the published coordinates of 294 vdB-Hagen 121 the clusters IC 2944 and vdBergh-Hagen 121: 294 IC 2944 vdBergh-Hagen 121 294 Lynga - (RA, Dec) 11.548 h, -60.72 d 11.635 h, -63.33 d 294 Dias - (RA, Dec) 11.639 h, -63.37 d - , - 294 From our detemination: 294 (RA, Dec) 11.602 h, -62.95 d 11.635 h, -63.33 d. 295 IC 2948 Possibly, this cluster is a part of vdB-Hagen 121. 297 Ruprecht 96 The age estimate could not be performed properly with our 297 usual algorithm. Therefore, the age was estimated by isochrone 297 fitting, manually. 303 NGC 4103 According to the LF analysis (Piskunov et al. 2004, 303 MNRAS,349,449), this cluster could be younger. 308 Melotte 111 In order to keep a symmetric form of the cluster, its centre 308 (Coma Ber) is shifted to (RA, Dec) = (12.375 h, +25.75 deg). 309 NGC 4349 The Turn-off point is fainter than the limiting magnitude of 309 the ASCC-2.5. The age from Loktin et al. (log t = 8.32) and 309 and the corresponding isochrone are adopted. 309 The cluster RV is determined from one star (Sp=F8V) which 309 is the brightest cluster member (P_ki = 91%). At the 309 distance of the cluster, this star would have M_V = -4.5. 309 On the other hand, this would contradict its spectral type 309 (M_V = +4.1 is expected for a F8V star at the cluster 309 distance). Therefore, the cluster RV is doubtful as long as 309 RVs are not observed for other cluster members. 313 NGC 4463 Compared to the estimates of Loktin et al., E(B-V) is 313 increased from 0.434 mag to 0.52 mag. 319 NGC 4852 There are a few bright giants widely distributed over 319 the cluster area. Probably, they are foreground stars. 320 NGC 5045 There is no cluster at the coordinates published. Therefore, 320 the cluster centre is shifted by 0.32 deg to the W, to a 320 group of O - B stars. 322 Stock 16 The published coordinates are incorrect. The cluster centre 322 is shifted by 0.14 deg to the NW. Compared to the estimates 322 of Loktin et al., E(B-V) is decreased from 0.491 mag to 322 0.48 mag. 330 NGC 5168 Compared to the estimates of Loktin et al., E(B-V) is 330 decreased from 0.43 mag to 0.33 mag. 336 NGC 5281 Compared to the estimates of Loktin et al., E(B-V) is 336 increased from 0.225 mag to 0.27 mag. 342 NGC 5359 There are no members within the Evolved MS. The age was 342 estimated by isochrone fitting, manually. 349 ESO 175-06 The age estimate could not be performed properly with our 349 usual algorithm. Therefore, the age was estimated by isochrone 349 fitting, manually. 361 NGC 5823 The Turn-off point is fainter than the limiting magnitude of 361 the ASCC-2.5. The age from Loktin et al. (log t = 8.90) and 361 the corresponding isochrone are adopted. 365 Ruprecht 113 The reddening is variable. Therefore, the density profile is 365 distorted. 369 NGC 6067 Compared to the estimates of Loktin et al., E(B-V) is 369 increased from 0.38 mag to 0.40 mag. 370 Harvard 10 Compared to the estimates of Loktin et al., E(B-V) is 370 decreased from 0.36 mag to 0.25 mag. 372 Ruprecht 116 The age estimate could not be performed properly with our 372 usual algorithm. Therefore, the age was estimated by isochrone 372 fitting, manually. 374 NGC 6134 Compared to the estimates of Dias et al., E(B-V) is 374 decreased from 0.395 mag to 0.38 mag. 376 NGC 6152 Compared to the estimates of Dias et al., E(B-V) is 376 decreased from 0.30 mag to 0.20 mag. 377 NGC 6167 Compared to the estimates of Loktin et al., E(B-V) is 377 increased from 0.779 mag to 0.79 mag. 382 NGC 6204 Although the clusters are located at an angular distance 383 Hogg 22 of 0.1 deg, they have very different cluster parameters: 383 NGC 6204 ==> d = 1085 pc, E(B-V) = 0.43 mag, log t = 8.28 383 Hogg 22 ==> d = 1297 pc, E(B-V) = 0.65 mag, log t = 6.70. 384 NGC 6208 There are no members within the Evolved MS. The Turn-off 384 point is fainter than the limiting magnitude of the ASCC-2.5. 384 The age from Loktin et al. (log t = 9.07) and the 384 corresponding isochrone are adopted. 394 Bochum 13 Compared to the estimates of Loktin et al., E(B-V) is 394 decreased from 0.85 mag to 0.78 mag. 395 NGC 6322 Compared to the estimates of Loktin et al., E(B-V) is 395 decreased from 0.59 mag to 0.53 mag. 401 Collinder 333 The age estimate could not be performed properly with our 401 usual algorithm. Therefore, the age was estimated by isochrone 401 fitting, manually. 406 Collinder 338 The age estimate could not be performed properly with our 406 usual algorithm. Therefore, the age was estimated by isochrone 406 fitting, manually. 410 Alessi 9 Cluster coordinates previously published do not coincide with 410 the maximum of the projected stellar density. Therefore, 410 the new cluster centre is shifted by 0.31 deg to the SE. 411 NGC 6416 The cluster has a complex CMD and VPD. Although the stellar 411 density is higher at r > r_corona = 0.22 deg than the 411 background, the stars at r > 0.22 deg have different 411 proper motions than the mean cluster proper motion. 423 Collinder 359 We can not confirm a cluster at a distance d = 254 pc 423 published by Loktin et al. The best fitting of the 423 observations is achieved with d = 640 pc, E(B-V) = 0.16 mag 423 derived from 7 B-, A- stars with known luminosity classes. 426 NGC 6520 Compared to the estimates of Loktin et al., E(B-V) is 426 decreased from 0.43 mag to 0.42 mag. 428 NGC 6530 Compared to the estimates of Loktin et al., E(B-V) is 428 decreased from 0.32 mag to 0.30 mag. 432 Collinder 367 Cluster coordinates previously published do not coincide with 432 the maximum of the projected stellar density. Therefore, 432 the new cluster centre is shifted by 0.17 deg to the N. 436 Markarian 38 Compared to the estimates of Loktin et al., E(B-V) is 436 decreased from 0.37 mag to 0.30 mag. 439 NGC 6604 Compared to the estimates of Loktin et al., E(B-V) is 439 decreased from 0.97 mag to 0.95 mag. 440 NGC 6603 The CMD is complex. The distance (d = 2880 pc) from the 440 Lynga catalogue is accepted. We derived E(B-V) = 0.50 mag. 441 NGC 6611 The reddening is very variable. Compared to the estimates of 441 Loktin et al., E(B-V) is decreased from 0.76 mag to 0.70 mag. 442 Alessi 19 Cluster coordinates previously published do not coincide with 442 the maximum of the projected stellar density. Therefore, 442 the new cluster centre is shifted by 0.15 deg to the E. 449 IC 4725 Compared to the estimates of Loktin et al., E(B-V) is 449 decreased from 0.476 mag to 0.45 mag. 454 NGC 6709 Compared to the estimates of Loktin et al., E(B-V) is 454 increased from 0.304 mag to 0.32 mag. 456 Stephenson 1 Cluster coordinates previously published do not coincide with 456 the maximum of the projected stellar density. Therefore, 456 the new cluster centre is shifted by 0.14 deg to the SE. 457 NGC 6716 Compared to the estimates of Loktin et al., E(B-V) is 457 decreased from 0.22 mag to 0.20 mag. 469 NGC 6828 The derived cluster age does not suit well to spectral 469 classes of the members. Possibly, this is a group of 469 co-moving stars. 475 Dolidze 38 There are no members within the Evolved MS. The age estimate 475 could not be performed properly with our usual algorithm. 475 Therefore, the age was estimated by isochrone fitting, 475 manually. 482 NGC 6882 Compared to the estimates of Loktin et al., E(B-V) is 482 decreased from 0.039 mag to 0.02 mag. 483 IC 4996 Compared to the estimates of Loktin et al., E(B-V) is 483 decreased from 0.67 mag to 0.60 mag. 488 NGC 6913 The reddening is very variable. Compared to the estimates of 488 Loktin et al., E(B-V) is increased from 0.74 mag to 0.98 mag. 494 NGC 6991 There is confusion with cluster coordinates in different 494 catalogues: 494 Lynga - (RA, Dec) = (20.927 h, 47.41 d), 494 Dias - (RA, Dec) = (20.915 h, 47.42 d), 494 From our detemination: (RA, Dec) = (20.909 h, 47.45 d). 495 NGC 7039 Two brightest proper motion members do not suit the cluster 495 CMD. Probably, they are co-moving stars. 501 NGC 7160 Compared to the estimates of Loktin et al., E(B-V) is 501 decreased from 0.37 mag to 0.35 mag. 511 NGC 7510 Compared to the estimates of Loktin et al., E(B-V) is 511 increased from 0.855 mag to 0.90 mag. 514 Stock 12 There is confusion with cluster coordinates in different 514 catalogues: 514 Lynga - (RA, Dec) = (23.593 h, 52.69 d), 514 Dias - (RA, Dec) = (23.606 h, 52.54 d). 514 We confirm the Lynga data. 517 NGC 7788 Compared to the estimates of Loktin et al., E(B-V) is 517 increased from 0.28 mag to 0.48 mag. 518 NGC 7789 The Turn-off point is fainter than the limiting magnitude of 518 the ASCC-2.5. There are only a few brighter blue stragglers 518 which are the most probable cluster members. The age 518 estimate by Loktin (log t = 9.23) and the corresponding 518 isochrone are adopted.