C.D.S. - SIMBAD4 rel 1.7 - 2020.07.05CEST06:45:25

2007A&A...470..699C - Astronomy and Astrophysics, volume 470, 699-708 (2007/8-1)

Sulphur abundances from the SI near-infrared triplet at 1045nm.


Abstract (from CDS):

Unlike silicon and calcium, sulphur is an α-element that does not form dust. Some of the available observations of the evolution of sulphur with metallicity indicate an increased scatter of sulphur-to-iron ratios at low metallicities or even a bimodal distribution, with some stars showing constant S/Fe at all metallicities and others showing an increasing S/Fe ratio with decreasing metallicity. In metal-poor stars Si lines of Multiplet 1 at 920nm are not yet too weak to permit the measurement of the sulphur abundance A(S); however, in ground-based observations they are severely affected by telluric lines. We investigate the possibility of measuring sulphur abundances from Si Mult. 3 at 1045nm lines. These lie in the near infrared and are slightly weaker than those of Mult. 1, but lie in a range not affected by telluric lines. We investigated the lines of Mult. 3 in the Sun (G2V), Procyon (F5V), HD 33256 (F5V), HD 25069 (G9V), and ε Eri (HD 22049, K2V). For the Sun and Procyon the analysis was performed with CO5BOLD 3D hydrodynamical model atmospheres, while the three other stars, for which hydrodynamical simulations are not available, were analysed using 1D model atmospheres. For our sample of stars we find a global agreement between A(S) from lines of different multiplets. Our results suggest that the infrared lines of Mult. 3 are a viable indicator of the sulphur abundance that, because of the intrinsic strength of this multiplet, should be suitable for studying the trend of [S/Fe] at low metallicities.

Abstract Copyright:

Journal keyword(s): Sun: abundances - stars: abundances - Galaxy: abundances - hydrodynamics - line: formation - radiative transfer

Simbad objects: 4

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Number of rows : 4

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
1 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1697 1
2 HD 25069 RG* 03 58 52.3938998575 -05 28 11.810156197   6.848 5.833     K0/1III 63 0
3 * 68 Eri PM* 05 08 43.6984486634 -04 27 22.340521388   5.546 5.119     F5.5VkF4mF2 202 0
4 * alf CMi SB* 07 39 18.11950 +05 13 29.9552 0.82 0.79 0.37 -0.05 -0.28 F5IV-V+DQZ 1757 0

    Equat.    Gal    SGal    Ecl

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