Context : Open clusters are ideal test particles for studying the formation and evolution of the Galactic disk .
However , the number of clusters with information about their radial velocities and chemical compositions remains largely insufficient .

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

Methods : We acquired medium-resolution spectra ( R \sim 8000 ) in the region of the infrared Ca II triplet lines ( \sim 8500Å ) for several stars in four open clusters with the long-slit spectrograph IDS at the 2.5m Isaac Newton Telescope , Roque de los Muchachos Observatory , Spain .
Radial velocities were obtained by cross-correlating the observed spectra with those of two template stars .
We used the relationships available in the literature between the strength of infrared Ca II lines and metallicities to derive the metal content of each cluster .

Results : We provide the first spectroscopic determinations of radial velocities and metallicities for the open clusters Berkeley 26 , Berkeley 70 , NGC 1798 , and NGC 2266 .
We obtain \langle V _ { r } \rangle =68 \pm 12 , -15 \pm 7 , 2 \pm 10 , and -16 \pm 15 km s ^ { -1 } for Berkeley 26 , Berkeley 70 , NGC 1798 , and NGC 2266 , respectively .
For Berkeley 26 we derive a metallicity of [ Fe/H ] =-0.35 \pm 0.17 dex .
Berkeley 70 has a solar metallicity of [ Fe/H ] =-0.01 \pm 0.14 dex , while NGC 1798 has a slightly lower metal content of [ Fe/H ] =-0.12 \pm 0.07 dex .
Finally , we derive a metallicity of [ Fe/H ] =-0.38 \pm 0.06 dex for NGC 2266 .

Conclusions :