Context : Open clusters are key to studying the formation and evolution of the Galactic disc .
However , there is a deficiency of radial velocity and chemical abundance determinations for open clusters in the literature .

Aims : We intend to increase the number of determinations of radial velocities and metallicities from spectroscopy for open clusters .

Methods : We acquired medium-resolution spectra ( R \sim 8000 ) in the infrared region Ca II triplet lines ( \sim 8500 Å ) for several stars in five open clusters with the long-slit IDS spectrograph on the 2.5 m Isaac Newton Telescope ( Roque de los Muchachos Observatory , Spain ) .
Radial velocities were obtained by cross-correlation fitting techniques .
The relationships available in the literature between the strength of infrared Ca II lines and metallicity were also used to derive the metallicity for each cluster .

Results : We obtain \left \langle V _ { r } \right \rangle = 48.6 \pm 3.4 , -58.4 \pm 6.8 , 26.0 \pm 4.3 , and -65.3 \pm 3.2 km s ^ { -1 } for Berkeley 23 , NGC 559 , NGC 6603 , and NGC 7245 , respectively .
We found [ Fe/H ] = -0.25 \pm 0.14 and -0.15 \pm 0.18 for NGC 559 and NGC 7245 , respectively .
Berkeley 23 has low metallicity , [ Fe/H ] = -0.42 \pm 0.13 , which is similar to other open clusters in the outskirts of the Galactic disc .
In contrast , we derived high metallicity ( [ Fe/H ] = +0.43 \pm 0.15 ) for NGC 6603 , which places this system amongst the most metal-rich known open clusters .
To our knowledge , this is the first determination of radial velocities and metallicities from spectroscopy for these clusters , except NGC 6603 , for which radial velocities had been previously determined .
We have also analysed ten stars in the line of sight to King 1 .
Because of the large dispersion obtained in both radial velocity and metallicity , we can not be sure that we have sampled true cluster members .

Conclusions :