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  1. OA@INAF
  2. PRODOTTI RICERCA INAF
  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
  4. 1.01 Articoli in rivista
Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12386/23068
Title: The Gaia-ESO Survey: Insights into the inner-disc evolution from open clusters
Authors: MAGRINI, LAURA 
RANDICH, Maria Sofia 
Donati, P.
BRAGAGLIA, Angela 
Adibekyan, V.
ROMANO, Donatella 
Smiljanic, R.
Blanco-Cuaresma, S.
Tautvaišienė, G.
Friel, E.
Overbeek, J.
Jacobson, H.
Cantat-Gaudin, T.
VALLENARI, Antonella 
SORDO, ROSANNA 
PANCINO, ELENA 
Geisler, D.
San Roman, I.
Villanova, S.
Casey, A.
Hourihane, A.
Worley, C. C.
Francois, P.
Gilmore, G.
Bensby, T.
FLACCOMIO, Ettore 
Korn, A. J.
Recio-Blanco, A.
Carraro, G.
Costado, M. T.
FRANCIOSINI, Elena 
Heiter, U.
Jofré, P.
Lardo, C.
de Laverny, P.
Monaco, L.
Morbidelli, L. 
SACCO, GIUSEPPE GERMANO 
Sousa, S. G.
ZAGGIA, Simone 
Issue Date: 2015
Journal: ASTRONOMY & ASTROPHYSICS 
Number: 580
First Page: A85
Abstract: Context. The inner disc, which links the thin disc with the bulge, has been somewhat neglected in the past because of the intrinsic difficulties in its study, among which crowding and high extinction. Open clusters located in the inner disc are among thebest tracers of its chemistry at different ages and distances. <BR /> Aims: We analyse the chemical patterns of four open clusters located within 7 kpc of the Galactic centre and of field stars to infer the properties of the inner disc with the Gaia-ESO survey idr2/3 data release. <BR /> Methods: We derive the parameters of the newly observed cluster, Berkeley 81, finding an age of about 1 Gyr and a Galactocentric distance of ~5.4 kpc. We construct the chemical patterns of clusters and we compare them with those of field stars in the solar neighbourhood and in the inner-disc samples. <BR /> Results: Comparing the three populations we observe that inner-disc clusters and field stars are both, on average, enhanced in [O/Fe], [Mg/Fe], and [Si/Fe]. Using the idr2/3 results of M67, we estimate the non-local thermodynamic equilibrium (NLTE) effect on the abundances of Mg and Si in giant stars. After empirically correcting for NLTE effects, we note that NGC 6705 and Be 81 still have a high [α/Fe]. <BR /> Conclusions: The location of the four open clusters and of the field population reveals that the evolution of the metallicity [Fe/H] and of [α/Fe] can be explained within the framework of a simple chemical evolution model: both [Fe/H] and [α/Fe] of Trumpler 20 and of NGC 4815 are in agreement with expectations from a simple chemical evolution model. On the other hand, NGC 6705, and to a lesser degree Berkeley 81, have higher [α/Fe] than expected for their ages, location in the disc, and metallicity. These differences might originate from local enrichment processes as explained in the inhomogeneous evolution framework. <P />Based on observations collected with the FLAMES spectrograph at VLT/UT2 telescope (Paranal Observatory, ESO, Chile), for the Gaia-ESO Large Public Survey (188.B-3002).
Acknowledgments: The Authors thank an anonymous referee whose comments and suggestions improved the quality of the paper. The results presented here benefited from discussions in three Gaia -ESO workshops supported by the ESF (European Science Foundation) through the GREAT ( Gaia Research for European Astronomy Training) Research Network Program (Science meetings 3855, 4127 and 4415). This work was partially supported by the Gaia Research for European Astronomy Training (GREAT-ITN) Marie Curie network, funded through the European Union Seventh Framework Programme [FP7/2007-2013] under grant agreement n. 264895. We acknowledge the support from INAF and Ministero dell’Istruzione, dell’Universitá e della Ricerca (MIUR) in the form of the grant “Premiale VLT 2012” and “The Chemical and Dynamical Evolution of the Milky Way and the Local Group Galaxies” (prot. 2010LY5N2T). V.A. acknowledges the support from the Fundação para a Ciência e a Tecnologia, FCT (Portugal) in the form of the fellowship SFRH/BPD/70574/2010. S.V. gratefully acknowledges the support provided by Fondecyt. reg. 1130721. T.B. was supported by the project grant “The New Milky” from the Knut and Alice Wallenberg foundation. U.H. acknowledges support from the Swedish National Space Board (SNSB/Rymdstyrelsen). G.T. acknowledges the support from the Research Council of Lithuania (grant No. MIP-082/2015). This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France.
URI: http://hdl.handle.net/20.500.12386/23068
URL: https://www.aanda.org/articles/aa/full_html/2015/08/aa26305-15/aa26305-15.html
ISSN: 0004-6361
DOI: 10.1051/0004-6361/201526305
Bibcode ADS: 2015A&A...580A..85M
Fulltext: open
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