All Tables

Table 1: Target clusters and their properties. Literature sources are reported in the text.
Table 2: Observation log of NGC 3960. One star is common to configurations A and B; we consider only clump objects here (7 stars in total). The remaining fibers were assigned to sky and to MS stars.
Table 3: Data for NGC 3960. ID $_{\rm {phot}}$ and BVI photometry (non corrected for differential reddening) are from Prisinzano et al. (2004). The number of exposures for each star is intended as the number of pointings with the same cross-disperser.
Table 4: Observation log of Be 32 and NGC 2660. One star is common to configurations A and B in Be 32 (10 stars in total). The remaining fibers were assigned to the sky.
Table 5: Data for Be 32. ID $_{\rm {phot}}$ , and BVI are from D'Orazi et al. (2006), while ID $_{\rm {fla}}$ is the identification number used for FLAMES observations.
Table 6: Data for NGC 2660. ID and BVI photometry are from Sandrelli et al. (1999).
Table 8: Set of Fe lines adopted for the analysis.
Table 12: Stellar parameters (photometric and spectroscopic) and Fe abundances for the sample stars in the three clusters.
Table 13: Sensitivities of Fe abundances to variations in the atmospheric parameters for typical stars in the three clusters.
Table 14: NGC 3960: comparison with the results by Bragaglia et al. (2006a); numbers in parenthesis are their IDs.
Table 7: Fe line list for the Sun and equivalent widths.
Table 9: Equivalent widths for Fe lines in stars of NGC 3960.
Table 10: Equivalent widths for Fe lines in stars of Be 32.
Table 11: Equivalent widths for Fe lines in stars of NGC 2660.