TY - JOUR
T1 - The Gaia-ESO Survey:
T2 - radial distribution of abundances in the Galactic disc from open clusters and young field stars
AU - Magrini, L.
AU - Randich, S.
AU - Kordopatis, G.
AU - Prantzos, N.
AU - Romano, D.
AU - Chieffi, A.
AU - Limongi, M.
AU - Francois, P.
AU - Pancino, E.
AU - Friel, E.
AU - Bragaglia, A.
AU - Tautvaisiene, G.
AU - Spina, L.
AU - Overbeek, J.
AU - Cantat-Gaudin, T.
AU - Donati, P.
AU - Vallenari, A.
AU - Sordo, R.
AU - Jimenez-Esteban, F. M.
AU - Tang, B.
AU - Drazdauskas, A.
AU - Sousa, S.
AU - Duffau, S.
AU - Jofre, P.
AU - Gilmore, G.
AU - Feltzing, S.
AU - Alfaro, E.
AU - Bensby, T.
AU - Flaccomio, E.
AU - Koposov, S.
AU - Lanzafame, A.
AU - Smiljanic, R.
AU - Bayo, A.
AU - Carraro, G.
AU - Casey, A. R.
AU - Costado, M. T.
AU - Damiani, F.
AU - Franciosini, E.
AU - Hourihane, A.
AU - Lardo, C.
AU - Lewis, J.
AU - Monaco, L.
AU - Morbidelli, L.
AU - Sacco, G.
AU - Sbordone, L.
AU - Worley, C. C.
AU - Zaggia, S.
N1 - 20 pages, 8 figures, 4 table, online tables sent on request
PY - 2017/7/1
Y1 - 2017/7/1
N2 - Context. The spatial distribution of elemental abundances in
the disc of our Galaxy gives insights both on its assembly process and
subsequent evolution, and on the stellar nucleogenesis of the different
elements. Gradients can be traced using several types of objects as, for
instance, (young and old) stars, open clusters, HII regions, planetary
nebulae.
Aims. We aim to trace the radial distributions of abundances of elements produced through different nucleosynthetic channels – the α-elements O, Mg, Si, Ca and Ti, and the iron-peak elements Fe, Cr, Ni and Sc – by use of the Gaia-ESO IDR4 results for open clusters and young-field stars.
Methods. From the UVES spectra of member stars, we have determined the average composition of clusters with ages > 0.1
Gyr. We derived statistical ages and distances of field stars. We
traced the abundance gradients using the cluster and field populations
and compared them with a chemo-dynamical Galactic evolutionary model.
Results. The adopted chemo-dynamical model, with the
new generation of metallicity-dependent stellar yields for massive
stars, is able to reproduce the observed spatial distributions of
abundance ratios, in particular the abundance ratios of [O/Fe] and
[Mg/Fe] in the inner disc (5 kpc <RGC< 7 kpc), with their differences, that were usually poorly explained by chemical evolution models.
Conclusions. Oxygen and magnesium are often considered to be equivalent in tracing α-element
abundances and in deducing, for example, the formation timescales of
different Galactic stellar populations. In addition, often [α/Fe] is computed combining several α-elements. Our results indicate, as expected, a complex and diverse nucleosynthesis of the various α-elements,
in particular in the high metallicity regimes, pointing towards a
different origin of these elements and highlighting the risk of
considering them as a single class with common features.
AB - Context. The spatial distribution of elemental abundances in
the disc of our Galaxy gives insights both on its assembly process and
subsequent evolution, and on the stellar nucleogenesis of the different
elements. Gradients can be traced using several types of objects as, for
instance, (young and old) stars, open clusters, HII regions, planetary
nebulae.
Aims. We aim to trace the radial distributions of abundances of elements produced through different nucleosynthetic channels – the α-elements O, Mg, Si, Ca and Ti, and the iron-peak elements Fe, Cr, Ni and Sc – by use of the Gaia-ESO IDR4 results for open clusters and young-field stars.
Methods. From the UVES spectra of member stars, we have determined the average composition of clusters with ages > 0.1
Gyr. We derived statistical ages and distances of field stars. We
traced the abundance gradients using the cluster and field populations
and compared them with a chemo-dynamical Galactic evolutionary model.
Results. The adopted chemo-dynamical model, with the
new generation of metallicity-dependent stellar yields for massive
stars, is able to reproduce the observed spatial distributions of
abundance ratios, in particular the abundance ratios of [O/Fe] and
[Mg/Fe] in the inner disc (5 kpc <RGC< 7 kpc), with their differences, that were usually poorly explained by chemical evolution models.
Conclusions. Oxygen and magnesium are often considered to be equivalent in tracing α-element
abundances and in deducing, for example, the formation timescales of
different Galactic stellar populations. In addition, often [α/Fe] is computed combining several α-elements. Our results indicate, as expected, a complex and diverse nucleosynthesis of the various α-elements,
in particular in the high metallicity regimes, pointing towards a
different origin of these elements and highlighting the risk of
considering them as a single class with common features.
KW - astro-ph.GA
KW - astro-ph.SR
U2 - 10.1051/0004-6361/201630294
DO - 10.1051/0004-6361/201630294
M3 - Article
SN - 0004-6361
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
ER -