TY - JOUR
T1 - The Gaia-ESO Survey
T2 - the N/O abundance ratio in the Milky Way
AU - Magrini, L.
AU - Vincenzo, F.
AU - Randich, S.
AU - Pancino, E.
AU - Casali, G.
AU - Tautvaisiene, G.
AU - Drazdauskas, A.
AU - Mikolaitis, S.
AU - Minkeviciute, R.
AU - Stonkute, E.
AU - Chorniy, Y.
AU - Bagdonas, V.
AU - Kordopatis, G.
AU - Frie, E.
AU - Roccatagliata, V.
AU - Jimenez-Esteban, F. M.
AU - Gilmore, G.
AU - Vallenari, A.
AU - Bensby, T.
AU - Bragaglia, A.
AU - Korn, A. J.
AU - Lanzafame, A. C.
AU - Smiljanic, R.
AU - Bayo, A.
AU - Casey, A. R.
AU - Costado, M. T.
AU - Franciosini, E.
AU - Hourihane, A.
AU - Jofré, P.
AU - Lewis, J.
AU - Monaco, L.
AU - Morbidelli, L.
AU - Sacco, G.
AU - Worley, C.
N1 - 9 pages, 7 figures (Appendix not available in the current version), accepted for publication on A&A.
Reproduced with permission from Astronomy & Astrophysics. © 2018 ESO
PY - 2018/10/1
Y1 - 2018/10/1
N2 - Context. The abundance ratio N/O is a useful tool to study the interplay of galactic processes, for example star formation e ciency, timescale of infall, and outflow loading factor. Aims. We aim to trace log(N/O) versus [Fe/H] in the Milky Way and to compare this ratio with a set of chemical evolution models to understand the role of infall, outflow, and star formation e ciency in the building up of the Galactic disc. Methods. We used the abundances from IDR2-3, IDR4, IDR5 data releases of the Gaia-ESO Survey both for Galactic field and open cluster stars. We determined membership and average composition of open clusters and we separated thin and thick disc field stars. We considered the e ect of mixing in the abundance of N in giant stars. We computed a grid of chemical evolution models, suited to reproduce the main features of our Galaxy, exploring the e ects of the star formation e ciency, infall timescale, and di erential outflow. Results. With our samples, we map the metallicity range0:6 [Fe/H] 0.3 with a corresponding1:2 log(N/O) 0:2, where the secondary production of N dominates. Thanks to the wide range of Galactocentric distances covered by our samples, we can distinguish the behaviour of log(N/O) in di erent parts of the Galaxy. Conclusions. Our spatially resolved results allow us to distinguish di erences in the evolution of N/O with Galactocentric radius. Comparing the data with our models, we can characterise the radial regions of our Galaxy. A shorter infall timescale is needed in the inner regions, while the outer regions need a longer infall timescale, coupled with a higher star formation e ciency. We compare our results with nebular abundances obtained in MaNGA galaxies, finding in our Galaxy a much wider range of log(N/O) than in integrated observations of external galaxies of similar stellar mass, but similar to the ranges found in studies of individual H II regions.
AB - Context. The abundance ratio N/O is a useful tool to study the interplay of galactic processes, for example star formation e ciency, timescale of infall, and outflow loading factor. Aims. We aim to trace log(N/O) versus [Fe/H] in the Milky Way and to compare this ratio with a set of chemical evolution models to understand the role of infall, outflow, and star formation e ciency in the building up of the Galactic disc. Methods. We used the abundances from IDR2-3, IDR4, IDR5 data releases of the Gaia-ESO Survey both for Galactic field and open cluster stars. We determined membership and average composition of open clusters and we separated thin and thick disc field stars. We considered the e ect of mixing in the abundance of N in giant stars. We computed a grid of chemical evolution models, suited to reproduce the main features of our Galaxy, exploring the e ects of the star formation e ciency, infall timescale, and di erential outflow. Results. With our samples, we map the metallicity range0:6 [Fe/H] 0.3 with a corresponding1:2 log(N/O) 0:2, where the secondary production of N dominates. Thanks to the wide range of Galactocentric distances covered by our samples, we can distinguish the behaviour of log(N/O) in di erent parts of the Galaxy. Conclusions. Our spatially resolved results allow us to distinguish di erences in the evolution of N/O with Galactocentric radius. Comparing the data with our models, we can characterise the radial regions of our Galaxy. A shorter infall timescale is needed in the inner regions, while the outer regions need a longer infall timescale, coupled with a higher star formation e ciency. We compare our results with nebular abundances obtained in MaNGA galaxies, finding in our Galaxy a much wider range of log(N/O) than in integrated observations of external galaxies of similar stellar mass, but similar to the ranges found in studies of individual H II regions.
KW - Galaxy: abundances
KW - Galaxy: disk
KW - Open clusters and associations: general
UR - http://www.scopus.com/inward/record.url?scp=85056145632&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/201833224
DO - 10.1051/0004-6361/201833224
M3 - Article
SN - 0004-6361
VL - 618
JO - Astronomy & Astrophysics
JF - Astronomy & Astrophysics
M1 - A102
ER -