We present the non-local thermodynamic equilibrium ( non-LTE ) calculations for O I with the updated model atom that includes quantum-mechanical rate coefficients for O I + H I inelastic collisions from the recent study of Barklem ( 2018 ) .
The non-LTE abundances from the O I lines were determined for the Sun and 46 FG stars in a wide metallicity range , -2.6 < [ Fe/H ] < 0.2 .
An application of accurate atomic data leads to larger departures from LTE and lower oxygen abundances compared to that for the Drawin ’ s theoretical approximation .
For the infrared O I 7771-5 Å triplet lines , the change in the non-LTE abundance is -0.11 dex for the solar atmospheric parameters and decreases in absolute value towards lower metallicity .
We revised the [ O/Fe ] – [ Fe/H ] trend derived in our earlier study .
The change in [ O/Fe ] is small in the [ Fe/H ] range from –1.5 to 0.2 .
For stars with [ Fe/H ] < -1 , the [ O/Fe ] ratio has increased such that [ O/Fe ] = 0.60 at [ Fe/H ] = –0.8 and increases up to [ O/Fe ] = 0.75 at [ Fe/H ] = –2.6 .