Context :

Aims : 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 \sim 1 Gyr , Galactocentric distance of 8.68 kpc ) , NGC 3960 ( \sim 1 Gyr , 7.80 kpc ) , and Be 32 ( \sim 6–7 Gyr , 11.30 kpc ) .
For Be 32 and NGC 2660 , our study provides the first metallicity determination based on high-resolution spectra .

Methods : We performed equivalent width analysis with the spectral code MOOG , which allows us to define a metallicity scale and build a homogeneous sample .

Results : 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 .

Conclusions :