We present manganese abundances in 10 red-giant members of the globular cluster \omega Centauri ; 8 stars are from the most metal-poor population ( RGB MP and RGB MInt1 ) while two targets are members of the more metal rich groups ( RGB MInt2 and MInt3 ) .
This is the first time Mn abundances have been studied in this peculiar stellar system .
The LTE values of [ Mn/Fe ] in \omega Cen overlap those of Milky Way stars in the metal poor \omega Cen populations ( [ Fe/H ] \sim -1.5 to -1.8 ) , however unlike what is observed in Milky Way halo and disk stars , [ Mn/Fe ] declines in the two more metal-rich RGB MInt2 and MInt3 targets .
Non-LTE calculations were carried out in order to derive corrections to the LTE Mn abundances .
The non-LTE results for \omega Cen in comparison with the non-LTE [ Mn/Fe ] versus [ Fe/H ] trend obtained for the Milky Way confirm and strengthen the conclusion that the manganese behavior in \omega Cen is distinct .
These results suggest that low-metallicity supernovae ( with metallicities \leq -2 ) of either Type II or Type Ia dominated the enrichment of the more metal-rich stars in \omega Cen .
The dominance of low-metallicity stars in the chemical evolution of \omega Cen has been noted previously in the s-process elements where enrichment from metal-poor AGB stars is indicated .
In addition , copper , which also has metallicity dependent yields , exhibits lower values of [ Cu/Fe ] in the RGB MInt2 and MInt3 \omega Cen populations .