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We present a spectroscopic study at high resolution, R~50,000, of 14 starslocated on the main sequence, at the turn-off point and on the early subgiantbranch in the cluster M67 in order to investigate its detailed chemicalcomposition, for comparison with the Sun and solar twins in the solarneighbourhood, and to explore selective atomic diffusion of chemical elementsas predicted by stellar-structure theory. We have obtained VLT/FLAMES-UVESspectra and analysed these strictly differentially in order to explorechemical-abundance similarities and differences between the M67 stars and theSun, and among the M67 stars themselves. Individual abundances of 19 differentchemical elements are obtained for the stars. They are found to agree very wellwith solar abundances, with abundance ratios closer to solar than those of mostsolar twins in the solar neighbourhood. An exception is Li which shows aconsiderable scatter among the cluster stars. There is a tendency for thecluster-star abundances to be depleted relative to the abundances in the fieldstars in correlation with the condensation temperature of the elements, atendency earlier found also for the Sun. The results support the hypothesisthat the gas of the proto-cluster was depleted by formation and cleansing ofdust before the stars formed. They also add support to the proposal that theSun was once formed in a dense stellar environment. Moreover, the observedminor reductions of heavy elements in the atmospheres of the dwarfs andturn-off point stars relative to our standard star M67-1194 and the subgiantsseem to suggest that diffusion processes are at work in these stars, althoughthe evidence is not compelling. Based on theoretical models thediffusion-corrected initial metallicity of M67 is estimated to be [Fe/H]=+0.06.

Abundances and possible diffusion of elements in M67 stars