Following deep astrometric and photometric study of the cluster NGC 2682 ( M 67 ) , we are able to accurately determine its fundamental parameters .
Being an old and rich cluster , M 67 is a relevant object for the analysis of the Galactic disk evolution .
M 67 is well studied but the lack of a wide and deep Strömgren photometric study makes our results worthwhile .
The brightest stars of the open cluster M 67 were used as uvby - H _ { \beta } standard stars in our studies of NGC 1817 and NGC 2548 , and the extension of the field covered , as well as the amount of observations , allowed to obtain the best set of Strömgren data ever published for this cluster .
We discuss the results of our CCD uvby - H _ { \beta } intermediate-band photometry , covering an area of about 50 \arcmin \times 50 \arcmin down to V \sim 19 .
Moreover , a complete membership segregation based on astrometric and photometric criteria is obtained .
The photometric analysis of a selected sample of stars yields a reddening value of E ( b - y ) = 0.03 \pm 0.03 , a distance modulus of V _ { 0 } - M _ { V } = 9.7 \pm 0.2 and [ Fe/H ] = 0.01 \pm 0.14 .
Through isochrone fitting we found an age of \log t = 9.6 \pm 0.1 ( 4.2 \pm 0.2 Gyr ) .
A clump of approximately 60 stars around V = 16 , ( b - y ) = 0.4 could be interpreted as a population of pre-cataclysmic variable stars ( if members ) , or as a stream of field G-type stars placed at twice the distance of the cluster ( if non-members ) .