2013A&A...559A.115M


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST07:29:51

2013A&A...559A.115M - Astronomy and Astrophysics, volume 559A, 115-115 (2013/11-1)

Galactic chemical evolution of sulphur. Sulphur abundances from the [SI] λ1082 nm line in giants.

MATROZIS E., RYDE N. and DUPREE A.K.

Abstract (from CDS):

The Galactic chemical evolution of sulphur is still under debate. At low metallicities some studies find no correlation between [S/Fe] and [Fe/H], which is typical for α-elements, while others find [S/Fe] increasing towards lower metallicities, and still others find a combination of the two. Each scenario has different implications for the Galactic chemical evolution of sulphur. The aim of this study is to contribute to the discussion on the Galactic chemical evolution of sulphur by deriving sulphur abundances from non-local thermodynamic equilibrium (LTE) insensitive spectral diagnostics in disk and halo stars with homogeneously determined stellar parameters. We derived effective temperatures from photometric colours, surface gravities from stellar isochrones and Bayesian estimation, and metallicities and sulphur abundances from spectrum synthesis. We derived sulphur abundances from the [SI] λ1082nm line in 39 mostly cool and metal-poor giants using 1D LTE MARCS model atmospheres to model our high-resolution near-infrared spectra obtained with the VLT, NOT, and Gemini South telescopes. We derive homogeneous stellar parameters for 29 of the 39 stars. Our results argue for a chemical evolution of sulphur that is typical for α-elements, contrary to some previous studies that have found high sulphur abundances ([S/Fe]>0.6) for stars with -2.5<[Fe/H]←1. Our abundances are systematically higher by about 0.1dex than those of other studies that arrived at similar conclusions using other sulphur diagnostics. We find the [SI] line to be a valuable diagnostic of sulphur abundances in cool giants down to [Fe/H]≃-2.3. We argue that a homogeneous determination of stellar parameters is necessary, since the derived abundances are sensitive to them. Our results ([S/Fe]) agree reasonably well with predictions of contemporary models of Galactic chemical evolution. In these models sulphur is predominantly created in massive stars by oxygen burning and is ejected into the interstellar medium during Type II supernovae explosions. Systematic differences with previous studies most likely fall within modelling uncertainties.

Abstract Copyright:

Journal keyword(s): Galaxy: evolution - stars: fundamental parameters - stars: abundances - infrared: stars

Simbad objects: 41

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Number of rows : 41

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 HD 2796 Pe* 00 31 16.9149599675 -16 47 40.792690842 9.58 9.28 8.50 8.14 8.67 Fw 178 0
2 * eps And PM* 00 38 33.3473333007 +29 18 42.328589821 5.72 5.25 4.38 3.70 3.19 G7IIIFe-3CH1 259 0
3 HD 8724 PM* 01 26 17.5944981072 +17 07 35.123836665   9.29 8.34     G5 104 0
4 * nu. Psc * 01 41 25.8939097 +05 29 15.406225 7.36 5.81 4.44 3.38 2.67 K3III 223 0
5 HD 13979 Pe* 02 15 20.8534621275 -25 54 54.874562581   9.81 9.18     F/Gw 78 0
6 HD 21581 Pe* 03 28 54.4846692612 -00 25 03.106157430 9.75 9.54 8.71     G8w 116 0
7 HD 23798 Pe* 03 46 45.7222019530 -30 51 13.332706976   9.35 8.32     G8/K1(III)wF0/3 63 0
8 HD 26297 Pe* 04 09 03.4179730777 -15 53 27.057216777   8.55 7.47 7.09   G5/6IVw 140 0
9 V* HP Eri LP* 04 38 55.7330333369 -13 20 48.133826226 10.91 9.72 8.33     G8/K0IIIwF7 125 0
10 * 16 Aur SB* 05 18 10.5702141 +33 22 17.808530       3.8   K2.5IIIbCN-0.5 136 0
11 HD 36702 Pe* 05 31 52.2291028356 -38 33 24.042415815   9.53 8.38     F0wG/K 62 0
12 * phi02 Ori PM* 05 36 54.3881859 +09 17 26.409553 5.70 5.04 4.09 3.33 2.78 G9.5IIIbFe-2.5 338 0
13 HD 40460 PM* 06 00 06.0385647008 +27 16 19.871506773   7.651 6.617     K1III 80 0
14 HD 44007 Pe* 06 18 48.5271098810 -14 50 43.424752212   8.85 8.06 7.69   G5(IV)wF3/5 170 0
15 * 28 Mon Ro* 08 01 13.3357402 -01 23 33.393493   6.147 4.680     K4III 70 1
16 HD 81192 Pe* 09 24 45.3354695684 +19 47 11.868330072 8.06 7.50 6.56     G8IIICH 113 0
17 HD 83212 Pe* 09 36 19.9520860588 -20 53 14.744519420   9.582 9.177 7.83   G6/K0IIIwF7 117 0
18 HD 85773 Pe* 09 53 39.2425768656 -22 50 08.422584118   10.51 9.43     Gwl: 85 0
19 HD 103545 Pe* 11 55 27.1609688264 +09 07 45.021393553   9.91 9.20 9.17   KIIvw 65 0
20 HD 110184 Pe* 12 40 14.0784174924 +08 31 38.056629204 10.20 9.45 8.27 8.52   KIIvw 126 0
21 HD 111721 PM* 12 51 25.1948813622 -13 29 28.166794065   8.78 7.97     G6V 145 0
22 HD 117876 PM* 13 32 48.21379 +24 20 48.2809   7.03   5.5   G8II-III 115 1
23 HD 122563 Pe* 14 02 31.8456299772 +09 41 09.942736952 7.47 7.10 6.19 5.37 4.79 G8:III:Fe-5 746 0
24 HD 122956 PM* 14 05 13.0245301143 -14 51 25.455585497   8.18 7.25 6.88   G6IV/VwF6 142 0
25 * alf Boo RG* 14 15 39.67207 +19 10 56.6730 2.46 1.18 -0.05 -1.03 -1.68 K1.5IIIFe-0.5 2133 0
26 BD+30 2611 * 15 06 53.8283818900 +30 00 36.942401309 11.50 10.37 9.13     G8III 122 0
27 * 16 Ser SB* 15 36 29.5749786777 +10 00 36.557426427   6.217 5.253     K0III:CN1Ba0.7Sr2 196 0
28 * 83 Her PM* 17 42 28.3624886832 +24 33 50.606183458   6.993 5.558     K4III 67 0
29 HD 166161 PM* 18 09 40.6841408875 -08 46 45.602722086 9.53 9.13 8.16     G0wF0 129 0
30 * eta Ser PM* 18 21 18.6005560 -02 53 55.776595 4.84 4.19 3.25 2.55 2.05 K0III-IV 351 0
31 * mu. Aql PM* 19 34 05.3535328 +07 22 44.179596 6.87 5.63 4.45 3.55 2.94 K3-IIIbFe0.5 251 1
32 HD 187111 Pe* 19 48 39.5745673482 -12 07 19.741286114   8.92 7.75     G8wF8III/IV 130 0
33 * bet Aql PM* 19 55 18.7925630 +06 24 24.342501 5.040 4.560 3.710 3.05 2.56 G8IV 514 0
34 HD 204543 * 21 29 28.2127594590 -03 30 55.356028557   9.17 8.30 7.99   F6/8(V) 124 0
35 * 35 Peg PM* 22 27 51.5223252490 +04 41 44.391554789 6.74 5.86 4.80 4.02 3.46 K1-III-IV 253 0
36 * 40 Peg PM* 22 38 52.5948415909 +19 31 20.106630489 7.370 6.750 5.820     G8II 59 0
37 HD 216143 Pe* 22 50 31.0884300128 -06 54 49.557528724   8.78 7.81 7.44   G2/3(IV)(we) 128 0
38 * gam Psc PM* 23 17 09.9374911 +03 16 56.237975 5.20 4.62 3.70 2.98 2.47 G9III:Fe-2 250 0
39 * tet Psc PM* 23 27 58.0952890 +06 22 44.371999 6.41 5.38 4.30 3.50 2.97 K0.5III 162 0
40 HD 221170 Pe* 23 29 28.8087923676 +30 25 57.847432750 9.43 8.74 7.66     G2IV 263 0
41 NAME Galactic Bulge reg ~ ~           ~ 3391 0

    Equat.    Gal    SGal    Ecl

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2020.07.13-07:29:51

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