The Gaia-ESO Survey : the N/O abundance ratio in the Milky Way
View/
Author
Magrini, L.
Vincenzo, F.
Randich, S.
Pancino, E.
Casali, G.
Tautvaisiene, G.
Drazdauskas, A.
Mikolaitis, S.
Minkeviciute, R.
Stonkute, E.
Chorniy, Y.
Bagdonas, V.
Kordopatis, G.
Frie, E.
Roccatagliata, V.
Jimenez-Esteban, F. M.
Gilmore, G.
Vallenari, A.
Bensby, T.
Bragaglia, A.
Korn, A. J.
Lanzafame, A. C.
Smiljanic, R.
Bayo, A.
Casey, A. R.
Costado, M. T.
Franciosini, E.
Hourihane, A.
Jofré, P.
Lewis, J.
Monaco, L.
Morbidelli, L.
Sacco, G.
Worley, C.
Attention
2299/20620
Abstract
The abundance ratio N/O is a useful tool to study the interplay of galactic processes, e.g. star formation efficiency, time-scale of infall and outflow loading factor We aim to trace log(N/O) versus [Fe/H] in the Milky Way and to compare it with a set of chemical evolution models to understand the role of infall, outflow and star formation efficiency in the building-up of the Galactic disc. We use the abundances from idr2-3, idr4, idr5 data releases of the Gaia-ESO Survey both for Galactic field and open cluster stars.We determine membership and average composition of open clusters and we separate thin and thick disc field stars.We consider the effect of mixing in the abundance of N in giant stars. We compute a grid of chemical evolution models, suited to reproduce the main features of our Galaxy, exploring the effects of the star formation efficiency, the infall time-scale and the differential outflow. With our samples, we map the metallicity range -0.6