Two distinct halo populations in the solar neighborhood

Nissen, P. E.; Schuster, W. J.

doi:10.1051/0004-6361/201116619

Cited by 161 publications

(224 citation statements)

References 75 publications

(91 reference statements)

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“…8 we compare the present bulge Zn abundances with those for thick disk stars in the literature. The results by Nissen & Schuster (2011) are maintained in all panels in Fig. 8, showing good agreement with other samples of thick disk stars.…”

Section: Comparison With Thick Disk Zn Abundancessupporting

confidence: 84%

“…7b we show the same stars as in Fig. 7a, adding metal-poor halo stars analysed by Cayrel et al (2004) and halo and thick disk stars results from Ishigaki et al (2013) and Nissen & Schuster (2011 …”

Section: Resultsmentioning

confidence: 93%

“…Therefore, A&A 580, A40 (2015) References. References in Col. 7: 1) Biémont & Godefroid (1980); 2) Ramírez & Allende-Prieto (2011); 3) Nissen & Schuster (2011); 4) astrophysical log gf from present fits. Kobayashi et al (2006) have invoked hypernovae to explain the high [Zn/Fe] ratios in metal-poor stars.…”

Section: Introductionmentioning

confidence: 81%

“…Sneden et al 1991;Nissen et al 2000;Ishigaki et al 2013;Barbuy et al 2013). Nissen & Schuster (2011) find that Zn behaves like alpha elements, with high-alpha halo stars and thick disk stars displaying also high Zn abundances, whereas the low-alpha halo stars show a lower Zn enhancement that decreases with metallicity. This distinct behaviour is explained if both these elements (Zn and alphas) are produced by core-collapse SNe.…”

Section: Introductionmentioning

confidence: 99%

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Zinc abundances in Galactic bulge field red giants: Implications for damped Lyman-αsystems

Barbuy

Friaça

Silveira

et al. 2015

A&A

107

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Context. Zinc in stars is an important reference element because it is a proxy to Fe in studies of damped Lyman-α systems (DLAs), permitting a comparison of chemical evolution histories of bulge stellar populations and DLAs. In terms of nucleosynthesis, it behaves as an alpha element because it is enhanced in metal-poor stars. Abundance studies in different stellar populations can give hints to the Zn production in different sites. Aims. The aim of this work is to derive the iron-peak element Zn abundances in 56 bulge giants from high resolution spectra. These results are compared with data from other bulge samples, as well as from disk and halo stars, and damped Lyman-α systems, in order to better understand the chemical evolution in these environments. Methods. High-resolution spectra were obtained using FLAMES+UVES on the Very Large Telescope. We computed the Zn abun-

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Section: Comparison With Thick Disk Zn Abundancessupporting

confidence: 84%

Section: Resultsmentioning

confidence: 93%

Section: Introductionmentioning

confidence: 81%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Zinc abundances in Galactic bulge field red giants: Implications for damped Lyman-αsystems

Barbuy

Friaça

Silveira

et al. 2015

A&A

107

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“…Manganese is thought to be mostly produced by explosive silicon burning in massive stars in their outer incomplete Si-burning layers (Umeda & Nomoto 2005) and in SNIa (Iwamoto et al 1999). If Mn were overproduced in SNIa compared to Fe, it would be expected that the low α population in Nissen & Schuster (2011) should be enriched in Mn compared to the high α (see Fig. 6c).…”

Section: The Origin Of Mnmentioning

confidence: 99%

The origin and evolution of the odd-Z iron-peak elements Sc, V, Mn, and Co in the Milky Way stellar disk

Battistini

Bensby

2015

A&A

140

213

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Context. Elements heavier than Li are produced in the interiors of stars. However, for many elements the exact production sites and the timescales on which they are dispersed into the interstellar medium are unknown. Having a clear picture on the origins of the elements is important for our ability to trace and understand the formation and chemical evolution of the Milky Way and its stellar populations. Aims. The aim of this study is to investigate the origin and evolution of Sc, V, Mn, and Co for a homogeneous and statistically significant sample of stars probing the different populations of the Milky Way, in particular the thin and thick disks. Methods. Using high-resolution spectra obtained with the MIKE, FEROS, SOFIN, FIES, UVES, and HARPS spectrographs, we determine Sc, V, Mn, and Co abundances for a large sample of F and G dwarfs in the solar neighborhood. The method is based on spectral synthesis and using one-dimensional, plane-parallel, local thermodynamic equilibrium (LTE) model stellar atmospheres calculated with the MARCS 2012 code. The non-LTE (NLTE) corrections from the literature were applied to Mn and Co. Results. We find that the abundance trends derived for Sc (594 stars

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Homogenized effective temperatures for metal deficient stars from stellar catalogues

Malyuto

2013

Astron Nachr

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Homogeneous independent subsamples from selected catalogues and libraries of effective temperatures for metal deficient F-G stars are treated here by combining them in triples and pairs for the stars in common to determine their external errors from data intercomparisons. The effective temperatures are then averaged (with the weights inversely proportional to the squared errors) to produce mean homogenized catalogues which may be used for calibration of spectral and photometric data in large Galactic surveys.

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Two distinct halo populations in the solar neighborhood

Abstract: Context. Current models of galaxy formation predict that the Galactic halo was assembled hierarchically. By measuring abundance ratios in stars it may be possible to identify substructures in the halo resulting from this process.

Cited by 161 publications

References 75 publications

Zinc abundances in Galactic bulge field red giants: Implications for damped Lyman-αsystems

Zinc abundances in Galactic bulge field red giants: Implications for damped Lyman-αsystems

The origin and evolution of the odd-Z iron-peak elements Sc, V, Mn, and Co in the Milky Way stellar disk

Homogenized effective temperatures for metal deficient stars from stellar catalogues

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