| Name | UT date | V | (B-V) | SWB | Age | [Fe/H] |
| (1) | (2) | (3) | (4) | (5) | (6) | (7) |
| NGC 1754 | 2006 Nov. 18 | 11.57 | 0.75 | VII | 10 | -1.42a, -1.54b |
| NGC 2005 | 2006 Nov. 29 | 11.57 | 0.73 | VII | 10 | -1.35a, -1.92b, -1.80c, -1.33d |
| NGC 2019 | 2006 Dec. 10 | 10.86 | 0.76 | VII | 10 | -1.23a, -1.18b, -1.37c, -1.10d |
| NGC 1806 | 2006 Dec. 06 | 11.10 | 0.73 | V | 1.1 | -0.23b, -0.71e |
| NGC 2162 | 2006 Dec. 05 | 12.70 | 0.68 | V | 1.1 | -0.23b, -0.46f |
| NGC 2173 | 2006 Dec. 06 | 11.88 | 0.82 | V-VI | 2 | -0.24b, -0.42f, -0.51g |
Notes. (1) Cluster name; (2) date of observation; (3) integrated V-band magnitude; (4) (B-V) colour and (5) SWB type taken from (Bica et al. 1996,1999); (6) Age of the cluster in Gyr, based on the SWB type (Frogel et al. 1990); (7) [Fe/H] derived using different methods: (a) Olsen et al. (1998) - slope of the RGB; (b) Olszewski et al. (1991) - low-resolution Ca II triplet; (c) Johnson et al. (2006) - high-resolution Fe I; (d) Johnson et al. (2006) - high-resolution Fe II; (e) Dirsch et al. (2000) - Strömgren photometry; (f) Grocholski et al. (2006) - low-resolution Ca II triplet; (g) Mucciarelli et al. (2008) - high-resolution spectroscopy.
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