We used the Ultraviolet and Visual Echelle Spectrograph of the ESO-Very Large Telescope to obtain a high resolution and high signal-to-noise ratio spectrum of Stock 16-12 , an early-type star which previous \Delta a photometric observations suggest being a chemically peculiar ( CP ) star .
We used spectral synthesis to perform a detailed abundance analysis obtaining an effective temperature of 8400 \pm 400 K , a surface gravity of 4.1 \pm 0.4 , a microturbulence velocity of 3.4 ^ { +0.7 } _ { -0.3 } \mathrm { km s } ^ { -1 } , and a projected rotational velocity of 68 \pm 4 \mathrm { km s } ^ { -1 } .
We provide photometric and spectroscopic evidence showing the star is most likely a member of the young Stock 16 open cluster ( age 3–8 Myr ) .
The probable cluster membership , the star ’ s position in the Hertzsprung-Russell diagram , and the found infrared excess strongly suggest the star is still in the pre-main-sequence ( PMS ) phase .
We used PMS evolutionary tracks to determine the stellar mass , which ranges between 1.95 and 2.3 M _ { \odot } , depending upon the adopted spectroscopic or photometric data results .
Similarly , we obtained a stellar age ranging between 4 and 6 Myr , in agreement with that of the cluster .
Because the star ’ s chemical abundance pattern resembles well that known of main sequence CP metallic line ( Am ) stars , the object sets important constraints to the diffusion theory .
Additional spectroscopic and spectropolarimetric data allowed us to conclude that the object is probably a single non-magnetic star .