2007
DOI: 10.1051/0004-6361:20077344
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Abstract: Aims. Based on a new set of sulphur abundances in very metal-poor stars and an improved analysis of previous data, we aim at resolving current discrepancies on the trend of S/Fe vs. Fe/H and thereby gain better insight into the nucleosynthesis of sulphur. The trends of Zn/Fe and S/Zn will also be studied. Methods. High resolution VLT/UVES spectra of 40 main-sequence stars with −3.3 < [Fe/H] < −1.0 are used to derive S abundances from the weak λ8694.6 S i line and the stronger λλ9212.9, 9237.5 pair of S i lines… Show more

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Cited by 153 publications
(238 citation statements)
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References 98 publications
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“…The Hβ-based temperatures are higher by 50-100 K when [Fe/H] > −2, but lower by about 100 K for [Fe/H] < −2.5. In the transition region, −2.5 ≤ [Fe/H] ≤ −2, there is a large scatter (Nissen et al 2007). This is essentially the same behaviour as just discussed when comparing with the estimates by …”
Section: Stellar Parameterssupporting
confidence: 80%
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“…The Hβ-based temperatures are higher by 50-100 K when [Fe/H] > −2, but lower by about 100 K for [Fe/H] < −2.5. In the transition region, −2.5 ≤ [Fe/H] ≤ −2, there is a large scatter (Nissen et al 2007). This is essentially the same behaviour as just discussed when comparing with the estimates by …”
Section: Stellar Parameterssupporting
confidence: 80%
“…This UVES sample is the same as that used by Nissen et al (2007); therefore we direct the reader to the description of the observations therein. Here we just mention that the UVES spectra cover the blue region 3800−5000 Å and the near-IR region 6700−10500 Å, both with a resolving power R ≡ λ/Δλ 60 000.…”
Section: Observations and Data Reductionmentioning
confidence: 99%
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“…Sulfur abundances in Milky Way (MW) stars have been obtained by several authors in the last years (Nissen et al 2007; Based on observations made with the ESO VLT-Kueyen telescope at the Paranal Observatory, Chile, in the course of the ESO-Large Programme 165.L-0263. Caffau et al 2007a;Ryde 2006;Caffau et al 2005b;Korn & Ryde 2005;Nissen et al 2004;Ryde & Lambert 2004, among the most recent), but agreement on its behavior at low metallicities has not been reached yet.…”
Section: Introductionmentioning
confidence: 99%
“…While some of the cited authors (e.g. Nissen et al 2007) find that S follows the same trend as other α-elements ( [S/Fe] showing a plateau at low metallicities), others point towards a steady growth in [S/Fe] with decreasing metallicity (Israelian & Rebolo 2001;Takada-Hidai et al 2002), or an increase in the scatter of [S/Fe] at low [Fe/H] (Caffau et al 2005b). The cited debate can in fact be extended to the overall behavior of α-elements.…”
Section: Introductionmentioning
confidence: 99%