The Gaia-ESO Survey: The N/O abundance ratio in the Milky Way

被引：25

作者：

Magrini, L. ^{[1
]}

Vincenzo, F. ^{[2
]}

Randich, S. ^{[1
]}

Pancino, E. ^{[1
,3
]}

Casali, G. ^{[1
,4
]}

Tautvaisiene, G. ^{[5
]}

Drazdauskas, A. ^{[5
]}

Mikolaitis, S. ^{[5
]}

Minkeviciute, R. ^{[5
]}

Stonkute, E. ^{[5
]}

Chorniy, Y. ^{[5
]}

Bagdonas, V. ^{[5
]}

Kordopatis, G. ^{[6
]}

Friel, E. ^{[7
]}

Roccatagliata, V. ^{[1
]}

Jimenez-Esteban, F. M. ^{[8
]}

Gilmore, G. ^{[9
]}

Vallenari, A. ^{[10
]}

Bensby, T. ^{[11
]}

Bragaglia, A. ^{[12
]}

Korn, A. J. ^{[13
]}

Lanzafame, A. C. ^{[14
]}

Smiljanic, R. ^{[15
]}

Bayo, A. ^{[16
,17
]}

Casey, A. R. ^{[18
,19
]}

Costado, M. T. ^{[20
]}

Franciosini, E. ^{[1
]}

Hourihane, A. ^{[9
]}

Jofre, P. ^{[21
]}

Lewis, J. ^{[9
]}

Monaco, L. ^{[22
]}

Morbidelli, L. ^{[1
]}

Sacco, G. ^{[1
]}

Worley, C. ^{[9
]}

机构：

[1] INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy

[2] Univ Hertfordshire, Ctr Astrophys Res, Coll Lane, Hatfield AL10 9AB, Herts, England

[3] Space Sci Data Ctr Agenzia Spaziale Italiana, Via Politecn SNC, I-00133 Rome, Italy

[4] Univ Firenze, Dipartimento Fis & Astron, Via Sansone 1, I-50019 Sesto Fiorentino, Italy

[5] Vilnius Univ, Inst Theoret Phys & Astron, Sauletekio Av 3, LT-10257 Vilnius, Lithuania

[6] Univ Cote dAzur, Observ Cote dAzur, CNRS, Lab Lagrange, Nice, France

[7] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA

[8] Ctr Astrobiol INTA CSIC, Dept Astrofis, ESAC Campus,Camino Bajo Castillo S-N, Madrid 28692, Spain

[9] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[10] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

[11] Lund Observ, Dept Astron & Theoret Phys, Box 43, S-22100 Lund, Sweden

[12] INAF Osservatorio Astron Bologna, Via Gobetti 93-3, I-40129 Bologna, Italy

[13] Uppsala Univ, Dept Phys & Astron, Box 516, S-75120 Uppsala, Sweden

[14] Univ Catania, Dipartimento Fis & Astron, Sez Astrofis, Via S Sofia 78, I-95123 Catania, Italy

[15] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland

[16] Univ Valparaiso, Inst Fis & Astron, Valparaiso, Chile

[17] Univ Valparaiso, Nucleo Milenio Formac Planetaria NPF, Av Gran Bretana 1111, Valparaiso, Chile

[18] Monash Univ, Sch Phys & Astron, Monash Ctr Astrophys, Clayton, Vic 3800, Australia

[19] Monash Univ, Monash Fac Informat Technol, Clayton, Vic 3800, Australia

[20] Univ Cadiz, Dept Didact, Cadiz 11519, Spain

[21] Univ Diego Portales, Nucleo Astron, Fac Ingn, Av Ejercito 441, Santiago, Chile

[22] Univ Andres Bello, Dept Ciencias Fis, Fernandez Concha 700, Santiago, Chile

来源：

ASTRONOMY & ASTROPHYSICS | 2018年 / 618卷

基金：

英国科学技术设施理事会;

关键词：

Galaxy: abundances; open clusters and associations: general; Galaxy: disk; GAMMA-RAY BURST; OXYGEN GALACTIC GRADIENTS; CHEMICAL EVOLUTION; STELLAR EVOLUTION; HOST GALAXIES; IA SUPERNOVAE; DATA RELEASE; NITROGEN ABUNDANCES; EXTRASOLAR PLANETS; ELEMENT ABUNDANCES;

D O I：

10.1051/0004-6361/201833224

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The abundance ratio N/O is a useful tool to study the interplay of galactic processes, for example star formation efficiency, 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 efficiency 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 effect 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 effects of the star formation efficiency, infall timescale, and differential outflow. Results. With our samples, we map the metallicity range -0. 6 <= [Fe/H] <= 0.3 with a corresponding -1.2 <= 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 different parts of the Galaxy. Conclusions. Our spatially resolved results allow us to distinguish differences 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 efficiency. 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.

引用

页数：10

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