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A comprehensive study of NGC 2345, a young open cluster with a low metallicity

Identificadores del recurso

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

http://dx.doi.org/10.13039/501100011033

http://dx.doi.org/10.13039/501100003329

http://dx.doi.org/10.13039/501100000781

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(DIGITAL.INTA)

Fitxa

Títol:: A comprehensive study of NGC 2345, a young open cluster with a low metallicity
Tema:: 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
Descripció:: Full Tables A.1 and A.4 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/631/A124; 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.; This research is based on observations collected with the MPG/ESO 2.2-m Telescope operated at the La Silla Observatory (Chile) jointly by the Max Planck Institute for Astronomy and the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes 087.D-603(A) and 095.A-9020(A). The AAT observations and the second run taken with FEROS were supported by the OPTICON project (observing proposals 2010B/01 and 2015A/008, respectively), which is funded by the European Community's Seventh Framework Programme. The INT and WHT telescopes are operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The WFC photometry was obtained as part of 151-INT12/11B. The IDS spectroscopy was taken as part of 32-INT3/11A. WYFFOS spectra were obtained under proposal 94-WHT23/12B whereas ISIS spectroscopy was made in service mode as part of SW2011b13. This research is partially supported by the Spanish Government under grants AYA2015-68012C2-2-P and PGC2018-093741-B-C21 (MICIU/AEI/FEDER, UE). This research has made use of the Simbad database, operated at CDS, Strasbourg (France). This publication also made use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation;With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737).; Peer review
Idioma:: English
Relació:: info:eu-repo/grantAgreement/MINECO//AYA2015-68012-C2-2-P; info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PGC2018-093741-B-C21/ES/ESTUDIO EMPIRICO MASIVO DE LA EVOLUCION ESTELAR: DESDE LAS PROTOESTRELLAS HASTA LOS PROGENITORES DE SUPERNOVAS POR COLAPSO GRAVITATORIO Y EMISORES DE ONDAS GRAVITACIONALES/; info:eu-repo/grantAgreement/EC/H2020/730890
Autor/Productor:: Alonso Santiago, J.; Negueruela, I.; Marco, A.; Tabernero, H.; González Fernández, C.; Castro, N.
Editor:: EDP Sciences
Otros colaboradores/productores:: Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737; González Fernández, C. [0000-0003-2612-0118]; Tabernero, H. [0000-0002-8087-4298]; Castro, N. [0000-0003-0521-473X]; European Southern Observatory (ESO); Agencia Estatal de Investigación (AEI); Ministerio de Economía y Competitividad (MINECO); European Research Council (ERC)
Drets:: Attribution-NonCommercial-NoDerivatives 4.0 International; © ESO 2019; https://creativecommons.org/licenses/by-nc-nd/4.0/; info:eu-repo/semantics/openAccess
Data:: 2021-04-14T10:01:59Z; 2019-11-05
Tipo de recurso:: info:eu-repo/semantics/article; info:eu-repo/semantics/publishedVersion; http://purl.org/coar/resource_type/c_6501
Format:: application/pdf

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2. <dc:creator>Alonso Santiago, J.</dc:creator>
3. <dc:creator>Negueruela, I.</dc:creator>
4. <dc:creator>Marco, A.</dc:creator>
5. <dc:creator>Tabernero, H.</dc:creator>
6. <dc:creator>González Fernández, C.</dc:creator>
7. <dc:creator>Castro, N.</dc:creator>
8. <dc:contributor>Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737</dc:contributor>
9. <dc:contributor>González Fernández, C. [0000-0003-2612-0118]</dc:contributor>
10. <dc:contributor>Tabernero, H. [0000-0002-8087-4298]</dc:contributor>
11. <dc:contributor>Castro, N. [0000-0003-0521-473X]</dc:contributor>
12. <dc:contributor>European Southern Observatory (ESO)</dc:contributor>
13. <dc:contributor>Agencia Estatal de Investigación (AEI)</dc:contributor>
14. <dc:contributor>Ministerio de Economía y Competitividad (MINECO)</dc:contributor>
15. <dc:contributor>European Research Council (ERC)</dc:contributor>
16. <dc:subject>Open clusters and associations: individual: NGC 2345</dc:subject>
17. <dc:subject>Hertzsprung–Russell and C–M diagrams</dc:subject>
18. <dc:subject>Stars: abundances</dc:subject>
19. <dc:subject>Stars: fundamental parameters</dc:subject>
20. <dc:subject>Stars: late type</dc:subject>
21. <dc:subject>Stars: emission line, Be</dc:subject>
22. <dc:description>Full Tables A.1 and A.4 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/631/A124</dc:description>
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24. <dc:description>This research is based on observations collected with the MPG/ESO 2.2-m Telescope operated at the La Silla Observatory (Chile) jointly by the Max Planck Institute for Astronomy and the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes 087.D-603(A) and 095.A-9020(A). The AAT observations and the second run taken with FEROS were supported by the OPTICON project (observing proposals 2010B/01 and 2015A/008, respectively), which is funded by the European Community's Seventh Framework Programme. The INT and WHT telescopes are operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The WFC photometry was obtained as part of 151-INT12/11B. The IDS spectroscopy was taken as part of 32-INT3/11A. WYFFOS spectra were obtained under proposal 94-WHT23/12B whereas ISIS spectroscopy was made in service mode as part of SW2011b13. This research is partially supported by the Spanish Government under grants AYA2015-68012C2-2-P and PGC2018-093741-B-C21 (MICIU/AEI/FEDER, UE). This research has made use of the Simbad database, operated at CDS, Strasbourg (France). This publication also made use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation;With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737).</dc:description>
25. <dc:description>Peer review</dc:description>
26. <dc:date>2021-04-14T10:01:59Z</dc:date>
27. <dc:date>2021-04-14T10:01:59Z</dc:date>
28. <dc:date>2019-11-05</dc:date>
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38. <dc:identifier>https://doi.org/10.13039/501100004604</dc:identifier>
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40. <dc:identifier>http://dx.doi.org/10.13039/501100003329</dc:identifier>
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31. <dim:field element="identifier" mdschema="dc" qualifier="funder">http://dx.doi.org/10.13039/501100000781</dim:field>
32. <dim:field element="description" lang="es" mdschema="dc">Full Tables A.1 and A.4 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/631/A124</dim:field>
33. <dim:field element="description" lang="es" mdschema="dc" qualifier="abstract">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.</dim:field>
34. <dim:field element="description" lang="es" mdschema="dc" qualifier="sponsorship">This research is based on observations collected with the MPG/ESO 2.2-m Telescope operated at the La Silla Observatory (Chile) jointly by the Max Planck Institute for Astronomy and the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes 087.D-603(A) and 095.A-9020(A). The AAT observations and the second run taken with FEROS were supported by the OPTICON project (observing proposals 2010B/01 and 2015A/008, respectively), which is funded by the European Community's Seventh Framework Programme. The INT and WHT telescopes are operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The WFC photometry was obtained as part of 151-INT12/11B. The IDS spectroscopy was taken as part of 32-INT3/11A. WYFFOS spectra were obtained under proposal 94-WHT23/12B whereas ISIS spectroscopy was made in service mode as part of SW2011b13. This research is partially supported by the Spanish Government under grants AYA2015-68012C2-2-P and PGC2018-093741-B-C21 (MICIU/AEI/FEDER, UE). This research has made use of the Simbad database, operated at CDS, Strasbourg (France). This publication also made use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation;With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737).</dim:field>
35. <dim:field element="description" lang="es" mdschema="dc" qualifier="peerreviewed">Peer review</dim:field>
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38. <dim:field element="relation" mdschema="dc">info:eu-repo/grantAgreement/MINECO//AYA2015-68012-C2-2-P</dim:field>
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42. <dim:field element="subject" lang="es" mdschema="dc">Hertzsprung–Russell and C–M diagrams</dim:field>
43. <dim:field element="subject" lang="es" mdschema="dc">Stars: abundances</dim:field>
44. <dim:field element="subject" lang="es" mdschema="dc">Stars: fundamental parameters</dim:field>
45. <dim:field element="subject" lang="es" mdschema="dc">Stars: late type</dim:field>
46. <dim:field element="subject" lang="es" mdschema="dc">Stars: emission line, Be</dim:field>
47. <dim:field element="title" lang="es" mdschema="dc">A comprehensive study of NGC 2345, a young open cluster with a low metallicity</dim:field>
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1. <title>A comprehensive study of NGC 2345, a young open cluster with a low metallicity</title>
2. <creator>Alonso Santiago, J.</creator>
3. <creator>Negueruela, I.</creator>
4. <creator>Marco, A.</creator>
5. <creator>Tabernero, H.</creator>
6. <creator>González Fernández, C.</creator>
7. <creator>Castro, N.</creator>
8. <contributor>Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737</contributor>
9. <contributor>González Fernández, C. [0000-0003-2612-0118]</contributor>
10. <contributor>Tabernero, H. [0000-0002-8087-4298]</contributor>
11. <contributor>Castro, N. [0000-0003-0521-473X]</contributor>
12. <contributor>European Southern Observatory (ESO)</contributor>
13. <contributor>Agencia Estatal de Investigación (AEI)</contributor>
14. <contributor>Ministerio de Economía y Competitividad (MINECO)</contributor>
15. <contributor>European Research Council (ERC)</contributor>
16. <subject>Open clusters and associations: individual: NGC 2345</subject>
17. <subject>Hertzsprung–Russell and C–M diagrams</subject>
18. <subject>Stars: abundances</subject>
19. <subject>Stars: fundamental parameters</subject>
20. <subject>Stars: late type</subject>
21. <subject>Stars: emission line, Be</subject>
22. <description>Full Tables A.1 and A.4 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/631/A124</description>
23. <description>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.</description>
24. <date>2021-04-14</date>
25. <date>2021-04-14</date>
26. <date>2019-11-05</date>
27. <type>info:eu-repo/semantics/article</type>
28. <identifier>Astronomy and Astrophysics 631: A124(2019)</identifier>
29. <identifier>0004-6361</identifier>
30. <identifier>https://www.aanda.org/articles/aa/full_html/2019/11/aa36109-19/aa36109-19.html</identifier>
31. <identifier>http://hdl.handle.net/20.500.12666/340</identifier>
32. <identifier>10.1051/0004-6361/201936109</identifier>
33. <identifier>1432-0746</identifier>
34. <identifier>https://doi.org/10.13039/501100004604</identifier>
35. <identifier>http://dx.doi.org/10.13039/501100011033</identifier>
36. <identifier>http://dx.doi.org/10.13039/501100003329</identifier>
37. <identifier>http://dx.doi.org/10.13039/501100000781</identifier>
38. <language>eng</language>
39. <relation>info:eu-repo/grantAgreement/EC/H2020/730890</relation>
40. <relation>info:eu-repo/grantAgreement/MINECO//AYA2015-68012-C2-2-P</relation>
41. <relation>info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PGC2018-093741-B-C21/ES/ESTUDIO EMPIRICO MASIVO DE LA EVOLUCION ESTELAR: DESDE LAS PROTOESTRELLAS HASTA LOS PROGENITORES DE SUPERNOVAS POR COLAPSO GRAVITATORIO Y EMISORES DE ONDAS GRAVITACIONALES/</relation>
42. <rights>© ESO 2019</rights>
43. <rights>https://creativecommons.org/licenses/by-nc-nd/4.0/</rights>
44. <rights>info:eu-repo/semantics/openAccess</rights>
45. <rights>Attribution-NonCommercial-NoDerivatives 4.0 International</rights>
46. <publisher>EDP Sciences</publisher>
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        <mods:abstract>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.</mods:abstract>
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mods

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1. <mods:name>
  1. <mods:namePart>Alonso Santiago, J.</mods:namePart>
  </mods:name>
2. <mods:name>
  1. <mods:namePart>Negueruela, I.</mods:namePart>
  </mods:name>
3. <mods:name>
  1. <mods:namePart>Marco, A.</mods:namePart>
  </mods:name>
4. <mods:name>
  1. <mods:namePart>Tabernero, H.</mods:namePart>
  </mods:name>
5. <mods:name>
  1. <mods:namePart>González Fernández, C.</mods:namePart>
  </mods:name>
6. <mods:name>
  1. <mods:namePart>Castro, N.</mods:namePart>
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7. <mods:extension>
  1. <mods:dateAvailable encoding="iso8601">2021-04-14T10:01:59Z</mods:dateAvailable>
  </mods:extension>
8. <mods:extension>
  1. <mods:dateAccessioned encoding="iso8601">2021-04-14T10:01:59Z</mods:dateAccessioned>
  </mods:extension>
9. <mods:originInfo>
  1. <mods:dateIssued encoding="iso8601">2019-11-05</mods:dateIssued>
  </mods:originInfo>
10. <mods:identifier type="citation">Astronomy and Astrophysics 631: A124(2019)</mods:identifier>
11. <mods:identifier type="issn">0004-6361</mods:identifier>
12. <mods:identifier type="other">https://www.aanda.org/articles/aa/full_html/2019/11/aa36109-19/aa36109-19.html</mods:identifier>
13. <mods:identifier type="uri">http://hdl.handle.net/20.500.12666/340</mods:identifier>
14. <mods:identifier type="doi">10.1051/0004-6361/201936109</mods:identifier>
15. <mods:identifier type="e-issn">1432-0746</mods:identifier>
16. <mods:identifier type="funder">https://doi.org/10.13039/501100004604</mods:identifier>
17. <mods:identifier type="funder">http://dx.doi.org/10.13039/501100011033</mods:identifier>
18. <mods:identifier type="funder">http://dx.doi.org/10.13039/501100003329</mods:identifier>
19. <mods:identifier type="funder">http://dx.doi.org/10.13039/501100000781</mods:identifier>
20. <mods:abstract>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.</mods:abstract>
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22. <mods:accessCondition type="useAndReproduction">© ESO 2019</mods:accessCondition>
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31. <mods:subject>
  1. <mods:topic>Stars: emission line, Be</mods:topic>
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1. <dc:title>A comprehensive study of NGC 2345, a young open cluster with a low metallicity</dc:title>
2. <dc:creator>Alonso Santiago, J.</dc:creator>
3. <dc:creator>Negueruela, I.</dc:creator>
4. <dc:creator>Marco, A.</dc:creator>
5. <dc:creator>Tabernero, H.</dc:creator>
6. <dc:creator>González Fernández, C.</dc:creator>
7. <dc:creator>Castro, N.</dc:creator>
8. <dc:contributor>Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737</dc:contributor>
9. <dc:contributor>González Fernández, C. [0000-0003-2612-0118]</dc:contributor>
10. <dc:contributor>Tabernero, H. [0000-0002-8087-4298]</dc:contributor>
11. <dc:contributor>Castro, N. [0000-0003-0521-473X]</dc:contributor>
12. <dc:contributor>European Southern Observatory (ESO)</dc:contributor>
13. <dc:contributor>Agencia Estatal de Investigación (AEI)</dc:contributor>
14. <dc:contributor>Ministerio de Economía y Competitividad (MINECO)</dc:contributor>
15. <dc:contributor>European Research Council (ERC)</dc:contributor>
16. <dc:subject>Open clusters and associations: individual: NGC 2345</dc:subject>
17. <dc:subject>Hertzsprung–Russell and C–M diagrams</dc:subject>
18. <dc:subject>Stars: abundances</dc:subject>
19. <dc:subject>Stars: fundamental parameters</dc:subject>
20. <dc:subject>Stars: late type</dc:subject>
21. <dc:subject>Stars: emission line, Be</dc:subject>
22. <dcterms:abstract>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.</dcterms:abstract>
23. <dcterms:dateAccepted>2021-04-14T10:01:59Z</dcterms:dateAccepted>
24. <dcterms:available>2021-04-14T10:01:59Z</dcterms:available>
25. <dcterms:created>2021-04-14T10:01:59Z</dcterms:created>
26. <dcterms:issued>2019-11-05</dcterms:issued>
27. <dc:type>info:eu-repo/semantics/article</dc:type>
28. <dc:identifier>Astronomy and Astrophysics 631: A124(2019)</dc:identifier>
29. <dc:identifier>0004-6361</dc:identifier>
30. <dc:identifier>https://www.aanda.org/articles/aa/full_html/2019/11/aa36109-19/aa36109-19.html</dc:identifier>
31. <dc:identifier>http://hdl.handle.net/20.500.12666/340</dc:identifier>
32. <dc:identifier>10.1051/0004-6361/201936109</dc:identifier>
33. <dc:identifier>1432-0746</dc:identifier>
34. <dc:identifier>https://doi.org/10.13039/501100004604</dc:identifier>
35. <dc:identifier>http://dx.doi.org/10.13039/501100011033</dc:identifier>
36. <dc:identifier>http://dx.doi.org/10.13039/501100003329</dc:identifier>
37. <dc:identifier>http://dx.doi.org/10.13039/501100000781</dc:identifier>
38. <dc:language>eng</dc:language>
39. <dc:relation>info:eu-repo/grantAgreement/EC/H2020/730890</dc:relation>
40. <dc:relation>info:eu-repo/grantAgreement/MINECO//AYA2015-68012-C2-2-P</dc:relation>
41. <dc:relation>info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PGC2018-093741-B-C21/ES/ESTUDIO EMPIRICO MASIVO DE LA EVOLUCION ESTELAR: DESDE LAS PROTOESTRELLAS HASTA LOS PROGENITORES DE SUPERNOVAS POR COLAPSO GRAVITATORIO Y EMISORES DE ONDAS GRAVITACIONALES/</dc:relation>
42. <dc:rights>© ESO 2019</dc:rights>
43. <dc:rights>https://creativecommons.org/licenses/by-nc-nd/4.0/</dc:rights>
44. <dc:rights>info:eu-repo/semantics/openAccess</dc:rights>
45. <dc:rights>Attribution-NonCommercial-NoDerivatives 4.0 International</dc:rights>
46. <dc:publisher>EDP Sciences</dc:publisher>
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  1. <dc:title>A comprehensive study of NGC 2345, a young open cluster with a low metallicity</dc:title>
  2. <dc:creator>Alonso Santiago, J.</dc:creator>
  3. <dc:creator>Negueruela, I.</dc:creator>
  4. <dc:creator>Marco, A.</dc:creator>
  5. <dc:creator>Tabernero, H.</dc:creator>
  6. <dc:creator>González Fernández, C.</dc:creator>
  7. <dc:creator>Castro, N.</dc:creator>
  8. <dc:contributor>Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737</dc:contributor>
  9. <dc:contributor>González Fernández, C. [0000-0003-2612-0118]</dc:contributor>
  10. <dc:contributor>Tabernero, H. [0000-0002-8087-4298]</dc:contributor>
  11. <dc:contributor>Castro, N. [0000-0003-0521-473X]</dc:contributor>
  12. <dc:contributor>European Southern Observatory (ESO)</dc:contributor>
  13. <dc:contributor>Agencia Estatal de Investigación (AEI)</dc:contributor>
  14. <dc:contributor>Ministerio de Economía y Competitividad (MINECO)</dc:contributor>
  15. <dc:contributor>European Research Council (ERC)</dc:contributor>
  16. <dc:subject>Open clusters and associations: individual: NGC 2345</dc:subject>
  17. <dc:subject>Hertzsprung–Russell and C–M diagrams</dc:subject>
  18. <dc:subject>Stars: abundances</dc:subject>
  19. <dc:subject>Stars: fundamental parameters</dc:subject>
  20. <dc:subject>Stars: late type</dc:subject>
  21. <dc:subject>Stars: emission line, Be</dc:subject>
  22. <dc:description>Full Tables A.1 and A.4 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/631/A124</dc:description>
  23. <dc:description>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.</dc:description>
  24. <dc:date>2021-04-14T10:01:59Z</dc:date>
  25. <dc:date>2021-04-14T10:01:59Z</dc:date>
  26. <dc:date>2019-11-05</dc:date>
  27. <dc:type>info:eu-repo/semantics/article</dc:type>
  28. <dc:identifier>Astronomy and Astrophysics 631: A124(2019)</dc:identifier>
  29. <dc:identifier>0004-6361</dc:identifier>
  30. <dc:identifier>https://www.aanda.org/articles/aa/full_html/2019/11/aa36109-19/aa36109-19.html</dc:identifier>
  31. <dc:identifier>http://hdl.handle.net/20.500.12666/340</dc:identifier>
  32. <dc:identifier>10.1051/0004-6361/201936109</dc:identifier>
  33. <dc:identifier>1432-0746</dc:identifier>
  34. <dc:identifier>https://doi.org/10.13039/501100004604</dc:identifier>
  35. <dc:identifier>http://dx.doi.org/10.13039/501100011033</dc:identifier>
  36. <dc:identifier>http://dx.doi.org/10.13039/501100003329</dc:identifier>
  37. <dc:identifier>http://dx.doi.org/10.13039/501100000781</dc:identifier>
  38. <dc:language>eng</dc:language>
  39. <dc:relation>info:eu-repo/grantAgreement/EC/H2020/730890</dc:relation>
  40. <dc:relation>info:eu-repo/grantAgreement/MINECO//AYA2015-68012-C2-2-P</dc:relation>
  41. <dc:relation>info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PGC2018-093741-B-C21/ES/ESTUDIO EMPIRICO MASIVO DE LA EVOLUCION ESTELAR: DESDE LAS PROTOESTRELLAS HASTA LOS PROGENITORES DE SUPERNOVAS POR COLAPSO GRAVITATORIO Y EMISORES DE ONDAS GRAVITACIONALES/</dc:relation>
  42. <dc:rights>© ESO 2019</dc:rights>
  43. <dc:rights>https://creativecommons.org/licenses/by-nc-nd/4.0/</dc:rights>
  44. <dc:rights>info:eu-repo/semantics/openAccess</dc:rights>
  45. <dc:rights>Attribution-NonCommercial-NoDerivatives 4.0 International</dc:rights>
  46. <dc:publisher>EDP Sciences</dc:publisher>
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