Digital INTA
author
Alonso Santiago, J.
author
Negueruela, I.
author
Marco, A.
author
Tabernero, H. M.
author
González Fernández, C.
author
Castro, N.
other
Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
orcid
González Fernández, C. [0000-0003-2612-0118]
orcid
Tabernero, H. [0000-0002-8087-4298]
orcid
Castro, N. [0000-0003-0521-473X]
funder
European Southern Observatory (ESO)
funder
Agencia Estatal de Investigación (AEI)
funder
Ministerio de Economía y Competitividad (MINECO)
funder
European Research Council (ERC)
2021-04-14T10:01:59Z
2021-04-14T10:01:59Z
2019-11-05
Astronomy and Astrophysics 631: A124(2019)
0004-6361
https://www.aanda.org/articles/aa/full_html/2019/11/aa36109-19/aa36109-19.html
http://hdl.handle.net/20.500.12666/340
10.1051/0004-6361/201936109
1432-0746
https://doi.org/10.13039/501100004604
Context. NGC 2345 is a young open cluster that hosts seven blue and red supergiants, low metallicity, and a high fraction of Be stars, which makes it a privileged laboratory to study stellar evolution. Aims. We aim to improve the determination of the cluster parameters and study the Be phenomenon. Our objective is also to characterise the seven evolved stars found in NGC 2345 by deriving their atmospheric parameters and chemical abundances. Methods. We performed a complete analysis combining for the first time ubvy photometry with spectroscopy as well as the Gaia Data Release 2. We obtained spectra with classification purposes for 76 stars and high-resolution spectroscopy for an in-depth analysis of the blue and red evolved stars. Results. We identify a new red supergiant and 145 B-type likely members within a radius of 18.7 ± 1.2 arcmin, which implies an initial mass, Mcl ≈ 5200 M⊙. We find a distance of 2.5 ± 0.2 kpc for NGC 2345, placing it at RGC = 10.2 ± 0.2 kpc. Isochrone fitting supports an age of 56 ± 13 Ma, implying masses around 6.5 M⊙ for the supergiants. A high fraction of Be stars (≈10%) is found. From the spectral analysis we estimate an average vrad = +58.6 ± 0.5 km s−1 and a low metallicity, [Fe/H] = −0.28 ± 0.07, for the cluster. We also determine chemical abundances for Li, O, Na, Mg, Si, Ca, Ti, Ni, Rb, Y, and Ba for the evolved stars. The chemical composition of the cluster is consistent with that of the Galactic thin disc. One of the K supergiants, S50, is a Li-rich star, presenting an A(Li) ≈ 2.1. An overabundance of Ba is found, supporting the enhanced s-process. Conclusions. NGC 2345 has a low metallicity for its Galactocentric distance, which is comparable to typical Large Magellanic Cloud stars. It is massive enough to serve as a test bed for theoretical evolutionary models for massive intermediate-mass stars.
eng
Attribution-NonCommercial-NoDerivatives 4.0 International
Open clusters and associations: individual: NGC 2345
Hertzsprung–Russell and C–M diagrams
Stars: abundances
Stars: fundamental parameters
Stars: late type
Stars: emission line, Be
A comprehensive study of NGC 2345, a young open cluster with a low metallicity
info:eu-repo/semantics/article
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URL
https://digital.inta.es:8443/jspui/bitstream/20.500.12666/340/3/aa36109-19.pdf
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