  We obtained high-resolution UVES/FLAMES observations of a sample of nine old
open clusters spanning a wide range of ages and Galactocentric radii. The goal
of the project is to investigate the radial metallicity gradient in the disk,
as well as the abundance of key elements (alpha and Fe-peak elements). In this
paper we present the results for the metallicity of three clusters: NGC 2660
(age ~1 Gyr, Galactocentric distance of 8.68 kpc), NGC 3960 (~ 1 Gyr, 7.80
kpc), and Be 32 (~6-7 Gyr, 11.30 kpc). For Be 32 and NGC 2660, our study
provides the first metallicity determination based on high-resolution spectra.
We performed equivalent width analysis with the spectral code MOOG, which
allows us to define a metallicity scale and build a homogeneous sample. We find
that NGC 3960 and NGC 2660 have a metallicity that is very close to solar
([Fe/H]=+0.02 and +0.04, respectively), while the older Be 32 turns out to have
[Fe/H]=$-$0.29.
