NGC1893 The proper motion provided by BDW is based on only one star. The star NGC1893 considered is HIP 25103 (pmRAcosDE=-1.3mas/yr and pmDE=+0.21mas/yr). NGC1893 This star is present in the Tycho2 catalogue (pmRAcosDE=-1.1mas/yr and NGC1893 pmDE=-1.8mas/yr), so that the proper motion is a little different from NGC1893 the Hipparcos one in pmDE. Note that the radial velocity of HIP 25103 NGC1893 (V=-7.5km/s, Crampton & Fisher, 1974PDAO...14..283C) is compatible NGC1893 with the mean radial velocity of the cluster (-4.7+/-4.4km/s) provided NGC1893 by Rastorguev et al. (1999, Cat. ). From a photometric NGC1893 point of view, the spectral type of this star (O5) suggests that it NGC1893 belongs to the cluster. The difference found in pmDE for that star NGC1893 explains partly the difference in the mean proper motion of the NGC1893 cluster in the two works. Since we used a dozen stars to segregate the NGC1893 members, we believe that our result is the more correct one, NGC1893 considering also that our result maintains the membership of the NGC1893 star HIP 25103. NGC5138 Proper motion provided by BDW is based on only one star. The star NGC5138 considered by BDW is HIP 65618. This star is present in the Tycho2 NGC5138 sample and our analysis shows that this star has high membership NGC5138 probability (P=85%). The difference obtained is due to the difference NGC5138 between Tycho2 (pmRAcosDE=-3.00mas/yr and pmDE=+3.10mas/yr) and NGC5138 Hipparcos (pmRAcosDE=-1.73mas/yr and pmDE=-4.79mas/yr) proper motions. NGC5138 To corroborate that our result is correct we note that Dias (2000, NGC5138 Master dissertation: Proper motion and membership in open clusters, NGC5138 Universidade de Sao Paulo, Sao Paulo, Brazil) determined the mean NGC5138 proper motion of this cluster, obtaining components NGC5138 (pmRAcosDE=-4.2mas/yr and pmDE=+1.9mas/yr) compatible with those NGC5138 derived in the present paper. NGC2360 A few open clusters present differences with BDW greater than the NGC2360 maximum expected value (about 2.5 mas/yr, which is the typical error NGC2360 in Tycho2 proper motions of single stars). In the cases of the NGC2360 clusters NGC 2360, NGC 2244, NGC 6531 and Trumpler 15 it seems that NGC2360 our method is unable to distinguish the members from the background, NGC2360 which has approximately the same proper motion (see the VPDs in NGC2360 Fig. 2). Based on the bad segregation of the two populations (field NGC2360 and cluster) in the VPD, we suggest that the results given by BDW are NGC2360 the correct ones. However, it is important to pay close attention to NGC2360 the fact that the proper motions provided by the Tycho2 catalogue NGC2360 differs from the Hipparcos ones, specially for the stars used by BDW NGC2360 for the cluster NGC 6531. NGC2244 See NGC2360 NGC6531 See NGC2360 tru15 See NGC2360