We have obtained medium-low resolution spectroscopy and BVI CCD imaging of Berkeley 32 , an old open cluster which lies in the anticentre direction .
From the radial velocities of 48 stars in the cluster direction we found that 31 of them , in crucial evolutionary phases , are probable cluster members , with an average radial velocity of +106.7 ( \sigma = 8.5 ) km s ^ { -1 } .

From isochrone fitting to the colour magnitude diagrams of Berkeley 32 we have obtained an age of 6.3 Gyr , ( m - M ) _ { 0 } = 12.48 and E ( B - V ) = 0.10 .
The best fit is obtained with Z=0.008 .
A consistent distance , ( m - M ) _ { 0 } \simeq 12.6 \pm 0.1 , has been derived from the mean magnitude of red clump stars with confirmed membership ; we may assume ( m - M ) _ { 0 } \simeq 12.55 \pm 0.1

The colour magnitude diagram of the nearby field observed to check for field stars contamination looks intriguingly similar to that of the Canis Major overdensity .