The Gaia-ESO Survey: radial metallicity gradients and age-metallicity relation of stars in the Milky Way disk

被引：167

作者：

Bergemann, M. ^{[1
]}

Ruchti, G. R. ^{[2
]}

Serenelli, A. ^{[3
]}

Feltzing, S. ^{[2
]}

Alves-Brito, A. ^{[4
,23
]}

Asplund, M. ^{[4
]}

Bensby, T. ^{[2
]}

Gruiters, P. ^{[5
]}

Heiter, U. ^{[5
]}

Hourihane, A. ^{[1
]}

Korn, A. ^{[5
]}

Lind, K. ^{[1
]}

Marino, A. ^{[4
]}

Jofre, P. ^{[1
]}

Nordlander, T. ^{[5
]}

Ryde, N. ^{[2
]}

Worley, C. C. ^{[1
]}

Gilmore, G. ^{[1
]}

Randich, S. ^{[6
]}

Ferguson, A. M. N. ^{[10
]}

Jeffries, R. D. ^{[11
]}

Micela, G. ^{[12
]}

Negueruela, I. ^{[13
]}

Prusti, T. ^{[14
]}

Rix, H. -W. ^{[15
]}

Vallenari, A. ^{[16
]}

Alfaro, E. J. ^{[21
]}

Allende Prieto, C. ^{[7
]}

Bragaglia, A. ^{[16
]}

Koposov, S. E. ^{[1
,8
]}

Lanzafame, A. C. ^{[24
]}

Pancino, E. ^{[9
,17
]}

Recio-Blanco, A. ^{[18
]}

Smiljanic, R. ^{[19
,20
]}

Walton, N. ^{[1
]}

Costado, M. T. ^{[21
]}

Franciosini, E. ^{[6
]}

Hill, V. ^{[18
]}

Lardo, C. ^{[17
]}

de Laverny, P. ^{[18
]}

Magrini, L. ^{[6
]}

Maiorca, E. ^{[6
]}

Masseron, T. ^{[1
]}

Morbidelli, L. ^{[6
]}

Sacco, G. ^{[6
]}

Kordopatis, G. ^{[1
]}

Tautvaisiene, G. ^{[22
]}

机构：

[1] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England

[2] Lund Observ, Dept Astron & Theoret Phys, S-22100 Lund, Sweden

[3] Fac Ciencies, Inst Space Sci IEEC CSIC, Bellaterra 08193, Spain

[4] Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia

[5] Uppsala Univ, Dept Phys & Astron, Div Astron & Space Phys, Angstrom Lab, S-75120 Uppsala, Sweden

[6] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy

[7] Inst Astrofis Canarias, Tenerife 38205, Spain

[8] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia

[9] ASI Sci Data Ctr, I-00133 Rome, Italy

[10] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland

[11] Keele Univ, Astrophys Grp, Res Inst Environm Phys Sci & Appl Math, Keele ST5 5BG, Staffs, England

[12] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy

[13] Univ Alicante, Dept Fis Ingn Sistemas & Teoria Senal, E-03080 Alicante, Spain

[14] Estec, ESA, NL-2200 AG Noordwijk, Netherlands

[15] Max Planck Inst Astron, D-69117 Heidelberg, Germany

[16] INAF Padova Observ, I-35122 Padua, Italy

[17] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy

[18] Univ Nice Sophia Antipolis, Lab Lagrange UMR7293, CNRS, Observ Cote Azur,CS 34229, F-06304 Nice 4, France

[19] Nicolaus Copernicus Astron Ctr, Dept Astrophys, PL-87100 Torun, Poland

[20] European So Observ, D-85748 Garching, Germany

[21] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain

[22] Vilnius State Univ, Inst Theoret Phys & Astron, LT-01108 Vilnius, Lithuania

[23] Univ Fed Rio Grande do Sul, Inst Fis, Porto Alegre, RS, Brazil

[24] Univ Catania, Sez Astrofis, Dipartimento Fis & Astron, I-95123 Catania, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2014年 / 565卷

基金：

瑞典研究理事会;

关键词：

stars: abundances; stars: fundamental parameters; solar neighborhood; Galaxy: disk; Galaxy: formation; surveys; GENEVA-COPENHAGEN SURVEY; INFRARED FLUX METHOD; MONO-ABUNDANCE SUBPOPULATIONS; LTE LINE FORMATION; G-DWARF STARS; SOLAR NEIGHBORHOOD; CHEMICAL EVOLUTION; THICK DISK; GALACTIC DISK; OPEN CLUSTERS;

D O I：

10.1051/0004-6361/201423456

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We study the relationship between age, metallicity, and alpha-enhancement of FGK stars in the Galactic disk. The results are based upon the analysis of high-resolution UVES spectra from the Gaia-ESO large stellar survey. We explore the limitations of the observed dataset, i.e. the accuracy of stellar parameters and the selection effects that are caused by the photometric target preselection. We find that the colour and magnitude cuts in the survey suppress old metal-rich stars and young metal-poor stars. This suppression may be as high as 97% in some regions of the age-metallicity relationship. The dataset consists of 144 stars with a wide range of ages from 0.5 Gyr to 13.5 Gyr, Galactocentric distances from 6 kpc to 9.5 kpc, and vertical distances from the plane 0 < vertical bar Z vertical bar < 1.5 kpc. On this basis, we find that i) the observed age-metallicity relation is nearly flat in the range of ages between 0 Gyr and 8 Gyr; ii) at ages older than 9 Gyr, we see a decrease in [Fe/H] and a clear absence of metal-rich stars; this cannot be explained by the survey selection functions; iii) there is a significant scatter of [Fe/H] at any age; and iv) [Mg/Fe] increases with age, but the dispersion of [Mg/Fe] at ages > 9 Gyr is not as small as advocated by some other studies. In agreement with earlier work, we find that radial abundance gradients change as a function of vertical distance from the plane. The [Mg/Fe] gradient steepens and becomes negative. In addition, we show that the inner disk is not only more alpha-rich compared to the outer disk, but also older, as traced independently by the ages and Mg abundances of stars.

引用

页数：11

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