Abundances in the Galactic Bulge: Evidence for fast chemical enrichment

M. Zoccali, A. Lecureur, B. Barbuy, V. Hill, A. Renzini, D. Minniti, Y. Momany, A. Gómez, S. Ortolani

Research output: Contribution to journalArticle

Abstract

We spectroscopically characterize the Galactic Bulge to infer its star formation timescale, compared to the other Galactic components, through the chemical signature on its individual stars. O, Na, Mg, Al were obtained for 50 K giants in four fields towards the Galactic bulge from UVES spectra (R=45,000), while Fe was measured in more than 400 stars with a slightly low resolution (R=20,000) and the GIRAFFE spectrograph at VLT. Oxygen and Magnesium show a well defined trend with [Fe/H], with abundances larger than those measured in both thin and thick disk stars, supporting a scenario in which the bulge formed before and more rapidly than the disk. On the other hand the iron distribution peaks at solar metallicity and it is slightly narrower than that measured in previous works. Part of the present results have been published by Zoccali et al. (2006) and Lecureur et al. (2006), and part will be discussed in forthcoming papers.

Original languageEnglish
Pages (from-to)73-77
Number of pages5
JournalProceedings of the International Astronomical Union
Volume2
Issue numberS241
DOIs
Publication statusPublished - Dec 2006

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galactic bulge
magnesium
timescale
iron
stars
oxygen
spectrographs
metallicity
star formation
signatures
trends
distribution
chemical
trend

Keywords

  • Atmospheres
  • Galaxy: bulge Stars: Abundances

ASJC Scopus subject areas

  • Astronomy and Astrophysics

Cite this

Zoccali, M. ; Lecureur, A. ; Barbuy, B. ; Hill, V. ; Renzini, A. ; Minniti, D. ; Momany, Y. ; Gómez, A. ; Ortolani, S. / Abundances in the Galactic Bulge : Evidence for fast chemical enrichment. In: Proceedings of the International Astronomical Union. 2006 ; Vol. 2, No. S241. pp. 73-77.
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Zoccali, M, Lecureur, A, Barbuy, B, Hill, V, Renzini, A, Minniti, D, Momany, Y, Gómez, A & Ortolani, S 2006, 'Abundances in the Galactic Bulge: Evidence for fast chemical enrichment', Proceedings of the International Astronomical Union, vol. 2, no. S241, pp. 73-77. https://doi.org/10.1017/S1743921307004723

Abundances in the Galactic Bulge : Evidence for fast chemical enrichment. / Zoccali, M.; Lecureur, A.; Barbuy, B.; Hill, V.; Renzini, A.; Minniti, D.; Momany, Y.; Gómez, A.; Ortolani, S.

In: Proceedings of the International Astronomical Union, Vol. 2, No. S241, 12.2006, p. 73-77.

Research output: Contribution to journalArticle

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T1 - Abundances in the Galactic Bulge

T2 - Evidence for fast chemical enrichment

AU - Zoccali, M.

AU - Lecureur, A.

AU - Barbuy, B.

AU - Hill, V.

AU - Renzini, A.

AU - Minniti, D.

AU - Momany, Y.

AU - Gómez, A.

AU - Ortolani, S.

PY - 2006/12

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N2 - We spectroscopically characterize the Galactic Bulge to infer its star formation timescale, compared to the other Galactic components, through the chemical signature on its individual stars. O, Na, Mg, Al were obtained for 50 K giants in four fields towards the Galactic bulge from UVES spectra (R=45,000), while Fe was measured in more than 400 stars with a slightly low resolution (R=20,000) and the GIRAFFE spectrograph at VLT. Oxygen and Magnesium show a well defined trend with [Fe/H], with abundances larger than those measured in both thin and thick disk stars, supporting a scenario in which the bulge formed before and more rapidly than the disk. On the other hand the iron distribution peaks at solar metallicity and it is slightly narrower than that measured in previous works. Part of the present results have been published by Zoccali et al. (2006) and Lecureur et al. (2006), and part will be discussed in forthcoming papers.

AB - We spectroscopically characterize the Galactic Bulge to infer its star formation timescale, compared to the other Galactic components, through the chemical signature on its individual stars. O, Na, Mg, Al were obtained for 50 K giants in four fields towards the Galactic bulge from UVES spectra (R=45,000), while Fe was measured in more than 400 stars with a slightly low resolution (R=20,000) and the GIRAFFE spectrograph at VLT. Oxygen and Magnesium show a well defined trend with [Fe/H], with abundances larger than those measured in both thin and thick disk stars, supporting a scenario in which the bulge formed before and more rapidly than the disk. On the other hand the iron distribution peaks at solar metallicity and it is slightly narrower than that measured in previous works. Part of the present results have been published by Zoccali et al. (2006) and Lecureur et al. (2006), and part will be discussed in forthcoming papers.

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