Context : We report the results from the determination of stellar masses , carbon and oxygen abundances in the atmospheres of 107 stars from the CHEPS program .
Our stars are drawn from a population with a significantly super-solar metallicity .
At least 10 of these stars are known to host orbiting planets .

Aims : In this work , we set out to understand the behavior of carbon and oxygen abundance in stars with different spectral classes , metallicities and V sin i , within the metal-rich stellar population .

Methods : Masses of these stars were determined using the data from Gaia DR2 release .
The oxygen and carbon abundances were determined by fitting the absorption lines .
Oxygen abundances were determined by fits to the 6300.304 Å O I line , and for the determination of the carbon abundances we used 3 lines of the C I atom and 12 lines of C _ { 2 } molecule .

Results : We determine masses and abundances of 107 CHEPS stars .
There is no evidence that the [ C/O ] ratio depends on V sin i or the mass of the star , within our constrained range of masses , i.e . 0.82 < M _ { * } / M _ { \odot } < 1.5 and metallicities -0.27 < [ Fe / H ] < +0.39 and we confirm that metal-rich dwarf stars with planets are more carbon-rich in comparison with non-planet host stars , with a statistical significance of 96 % .

Conclusions : We find tentative evidence that there is a slight offset to lower abundance and a greater dispersion in oxygen abundances relative to carbon , and interpret this as potentially arising from the production of the oxygen being more effective at more metal-poor epochs .
We also find evidence that for lower mass star’s the angular momentum loss in star’s with planets as measured by V sin i is steeper than star’s without planets .
In general , we find that the fast rotators ( V sin i > 5 kms ^ { -1 } ) are massive stars .