The Gaia-ESO Survey: Detailed abundances in the metal-poor globular cluster NGC 4372

I. San Roman; C. Munoz; D. Geisler; S. Villanova; N. Kacharov; A. Koch; G. Carraro; G. Tautvaisiene; A. Vallenari; E. J. Alfaro; Thomas Bensby; E. Flaccomio; P. Francois; A. J. Korn; E. Pancino; A. Recio-Blanco; R. Smiljanic; M. Bergemann; M. T. Costado; F. Damiani; U. Heiter; A. Hourihane; P. Jofre; C. Lardo; P. de Laverny; T. Masseron; L. Morbidelli; L. Sbordone; S. G. Sousa; C. C. Worley; S. Zaggia

doi:10.1051/0004-6361/201525722

The Gaia-ESO Survey: Detailed abundances in the metal-poor globular cluster NGC 4372

I. San Roman, C. Munoz, D. Geisler, S. Villanova, N. Kacharov, A. Koch, G. Carraro, G. Tautvaisiene, A. Vallenari, E. J. Alfaro, Thomas Bensby, E. Flaccomio, P. Francois, A. J. Korn, E. Pancino, A. Recio-Blanco, R. Smiljanic, M. Bergemann, M. T. Costado, F. DamianiU. Heiter, A. Hourihane, P. Jofre, C. Lardo, P. de Laverny, T. Masseron, L. Morbidelli, L. Sbordone, S. G. Sousa, C. C. Worley, S. Zaggia

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Abstract

We present the abundance analysis for a sample of 7 red giant branch stars in the metal-poor globular cluster NGC 4372 based on UVES spectra acquired as part of the Gaia-ESO Survey. This is the first extensive study of this cluster from high-resolution spectroscopy. We derive abundances of O, Na, Mg, Al, Si, Ca, Sc, Ti, Fe, Cr, Ni, Y, Ba, and La. We find a metallicity of [Fe/H] = -2.19 +/- 0.03 and find no evidence of any metallicity spread. This metallicity makes NGC 4372 one of the most metal-poor Galactic globular clusters. We also find an a-enhancement typical of halo globular clusters at this metallicity. Significant spreads are observed in the abundances of light elements. In particular, we find a Na-O anticorrelation. Abundances of O are relatively high compared with other globular clusters. This could indicate that NGC 4372 was formed in an environment with high O for its metallicity. A Mg-Al spread is also present that spans a range of more than 0.5 dex in Al abundances. Na is correlated with Al and Mg abundances at a lower significance level. This pattern suggests that the Mg-Al burning cycle is active. This behavior can also be seen in giant stars of other massive, metal-poor clusters. A relation between light and heavy s-process elements has been identified.

Original language	English
Article number	A6
Journal	Astronomy & Astrophysics
Volume	579
DOIs	https://doi.org/10.1051/0004-6361/201525722
Publication status	Published - 2015

Subject classification (UKÄ)

Astronomy, Astrophysics and Cosmology

Free keywords

globular clusters: individual: NGC 4372
stars: abundances

Access to Document

10.1051/0004-6361/201525722

Gaia-ESO Survey
Gilmore, G. (PI), Randich, S. (PI), Feltzing, S. (CoI), Bensby, T. (CoI), Howes, L. (Researcher), Gruyters, P. (Researcher), Ryde, N. (CoI), Stonkute, E. (Researcher) & Ruchti, G. (Researcher)
2012/12/24 → 2022/07/01
Project: Research

Cite this

San Roman, I., Munoz, C., Geisler, D., Villanova, S., Kacharov, N., Koch, A., Carraro, G., Tautvaisiene, G., Vallenari, A., Alfaro, E. J., Bensby, T., Flaccomio, E., Francois, P., Korn, A. J., Pancino, E., Recio-Blanco, A., Smiljanic, R., Bergemann, M., Costado, M. T., ... Zaggia, S. (2015). The Gaia-ESO Survey: Detailed abundances in the metal-poor globular cluster NGC 4372. Astronomy & Astrophysics, 579, Article A6. https://doi.org/10.1051/0004-6361/201525722

@article{b115c300cc4a49f0ae9aa3b4240337c9,

title = "The Gaia-ESO Survey: Detailed abundances in the metal-poor globular cluster NGC 4372",

abstract = "We present the abundance analysis for a sample of 7 red giant branch stars in the metal-poor globular cluster NGC 4372 based on UVES spectra acquired as part of the Gaia-ESO Survey. This is the first extensive study of this cluster from high-resolution spectroscopy. We derive abundances of O, Na, Mg, Al, Si, Ca, Sc, Ti, Fe, Cr, Ni, Y, Ba, and La. We find a metallicity of [Fe/H] = -2.19 +/- 0.03 and find no evidence of any metallicity spread. This metallicity makes NGC 4372 one of the most metal-poor Galactic globular clusters. We also find an a-enhancement typical of halo globular clusters at this metallicity. Significant spreads are observed in the abundances of light elements. In particular, we find a Na-O anticorrelation. Abundances of O are relatively high compared with other globular clusters. This could indicate that NGC 4372 was formed in an environment with high O for its metallicity. A Mg-Al spread is also present that spans a range of more than 0.5 dex in Al abundances. Na is correlated with Al and Mg abundances at a lower significance level. This pattern suggests that the Mg-Al burning cycle is active. This behavior can also be seen in giant stars of other massive, metal-poor clusters. A relation between light and heavy s-process elements has been identified.",

keywords = "globular clusters: individual: NGC 4372, stars: abundances",

author = "{San Roman}, I. and C. Munoz and D. Geisler and S. Villanova and N. Kacharov and A. Koch and G. Carraro and G. Tautvaisiene and A. Vallenari and Alfaro, {E. J.} and Thomas Bensby and E. Flaccomio and P. Francois and Korn, {A. J.} and E. Pancino and A. Recio-Blanco and R. Smiljanic and M. Bergemann and Costado, {M. T.} and F. Damiani and U. Heiter and A. Hourihane and P. Jofre and C. Lardo and {de Laverny}, P. and T. Masseron and L. Morbidelli and L. Sbordone and Sousa, {S. G.} and Worley, {C. C.} and S. Zaggia",

year = "2015",

doi = "10.1051/0004-6361/201525722",

language = "English",

volume = "579",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

San Roman, I, Munoz, C, Geisler, D, Villanova, S, Kacharov, N, Koch, A, Carraro, G, Tautvaisiene, G, Vallenari, A, Alfaro, EJ, Bensby, T, Flaccomio, E, Francois, P, Korn, AJ, Pancino, E, Recio-Blanco, A, Smiljanic, R, Bergemann, M, Costado, MT, Damiani, F, Heiter, U, Hourihane, A, Jofre, P, Lardo, C, de Laverny, P, Masseron, T, Morbidelli, L, Sbordone, L, Sousa, SG, Worley, CC & Zaggia, S 2015, 'The Gaia-ESO Survey: Detailed abundances in the metal-poor globular cluster NGC 4372', Astronomy & Astrophysics, vol. 579, A6. https://doi.org/10.1051/0004-6361/201525722

TY - JOUR

T1 - The Gaia-ESO Survey: Detailed abundances in the metal-poor globular cluster NGC 4372

AU - San Roman, I.

AU - Munoz, C.

AU - Geisler, D.

AU - Villanova, S.

AU - Kacharov, N.

AU - Koch, A.

AU - Carraro, G.

AU - Tautvaisiene, G.

AU - Vallenari, A.

AU - Alfaro, E. J.

AU - Bensby, Thomas

AU - Flaccomio, E.

AU - Francois, P.

AU - Korn, A. J.

AU - Pancino, E.

AU - Recio-Blanco, A.

AU - Smiljanic, R.

AU - Bergemann, M.

AU - Costado, M. T.

AU - Damiani, F.

AU - Heiter, U.

AU - Hourihane, A.

AU - Jofre, P.

AU - Lardo, C.

AU - de Laverny, P.

AU - Masseron, T.

AU - Morbidelli, L.

AU - Sbordone, L.

AU - Sousa, S. G.

AU - Worley, C. C.

AU - Zaggia, S.

PY - 2015

Y1 - 2015

N2 - We present the abundance analysis for a sample of 7 red giant branch stars in the metal-poor globular cluster NGC 4372 based on UVES spectra acquired as part of the Gaia-ESO Survey. This is the first extensive study of this cluster from high-resolution spectroscopy. We derive abundances of O, Na, Mg, Al, Si, Ca, Sc, Ti, Fe, Cr, Ni, Y, Ba, and La. We find a metallicity of [Fe/H] = -2.19 +/- 0.03 and find no evidence of any metallicity spread. This metallicity makes NGC 4372 one of the most metal-poor Galactic globular clusters. We also find an a-enhancement typical of halo globular clusters at this metallicity. Significant spreads are observed in the abundances of light elements. In particular, we find a Na-O anticorrelation. Abundances of O are relatively high compared with other globular clusters. This could indicate that NGC 4372 was formed in an environment with high O for its metallicity. A Mg-Al spread is also present that spans a range of more than 0.5 dex in Al abundances. Na is correlated with Al and Mg abundances at a lower significance level. This pattern suggests that the Mg-Al burning cycle is active. This behavior can also be seen in giant stars of other massive, metal-poor clusters. A relation between light and heavy s-process elements has been identified.

AB - We present the abundance analysis for a sample of 7 red giant branch stars in the metal-poor globular cluster NGC 4372 based on UVES spectra acquired as part of the Gaia-ESO Survey. This is the first extensive study of this cluster from high-resolution spectroscopy. We derive abundances of O, Na, Mg, Al, Si, Ca, Sc, Ti, Fe, Cr, Ni, Y, Ba, and La. We find a metallicity of [Fe/H] = -2.19 +/- 0.03 and find no evidence of any metallicity spread. This metallicity makes NGC 4372 one of the most metal-poor Galactic globular clusters. We also find an a-enhancement typical of halo globular clusters at this metallicity. Significant spreads are observed in the abundances of light elements. In particular, we find a Na-O anticorrelation. Abundances of O are relatively high compared with other globular clusters. This could indicate that NGC 4372 was formed in an environment with high O for its metallicity. A Mg-Al spread is also present that spans a range of more than 0.5 dex in Al abundances. Na is correlated with Al and Mg abundances at a lower significance level. This pattern suggests that the Mg-Al burning cycle is active. This behavior can also be seen in giant stars of other massive, metal-poor clusters. A relation between light and heavy s-process elements has been identified.

KW - globular clusters: individual: NGC 4372

KW - stars: abundances

U2 - 10.1051/0004-6361/201525722

DO - 10.1051/0004-6361/201525722

M3 - Article

SN - 0004-6361

VL - 579

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - A6

ER -

The Gaia-ESO Survey: Detailed abundances in the metal-poor globular cluster NGC 4372

Abstract

Subject classification (UKÄ)

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Gaia-ESO Survey

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