2001ApJ...557L..43I

Query : 2001ApJ...557L..43I

2001ApJ...557L..43I - Astrophys. J., 557, L43-L46 (2001/August-2)

Sulphur abundance in very metal-poor stars.

ISRAELIAN G. and REBOLO R.

Abstract (from CDS):

We have obtained high-resolution high signal-to-noise ratio spectra of the S I near-infrared doublet at 8694 Å in eight metal-poor stars with metallicities in the range -0.6≤[Fe/H]≤-3.0. Elemental sulphur abundances were derived for six targets, and upper limits were set for two of the most metal-poor stars in the sample. The sulphur doublet at 8694.62 Å has been detected in three stars (HD 19445, HD 2665, and HD 2796) with [Fe/H]≤-1.9. Our observations, combined with those available in the literature, indicate a monotonic increase of the [S/Fe] ratio as [Fe/H] decreases, reaching values of [S/Fe]∼0.7-0.8 below [Fe/H]=-2. We discuss plausible scenarios for the interpretation of these results.

Abstract Copyright: ∼

Journal keyword(s): Galaxy: Evolution - Nuclear Reactions, Nucleosynthesis, Abundances - Stars: Abundances - Stars: Late-Type - Stars: Population II

Simbad objects: 29

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Number of rows : 29
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 HD 2665 PM* 00 30 45.4469338728 +57 03 53.628989292 8.66 8.51 7.72     G5IIIw 188 0
2 HD 2796 Pe* 00 31 16.9147531152 -16 47 40.790991624 9.58 9.28 8.50 8.14 8.67 Fw 203 0
3 HD 19445 Pe* 03 08 25.5883873084 +26 19 51.400965175 8.29 8.52 8.06 7.60 7.27 G2VFe-3 801 0
4 HD 24616 PM* 03 53 59.4642188174 -23 08 13.471094216   7.52 6.71     G8IV/V 119 0
5 HD 59984 PM* 07 32 05.7629164512 -08 52 52.775251032   6.431 5.916     G0VFe-1.6CH-0.5 233 0
6 * 171 Pup SB* 07 45 34.9212542040 -34 10 21.185626324   5.909 5.362     F9V 318 0
7 * chi Cnc PM* 08 20 03.8607602556 +27 13 03.738171893   5.61   4.8   F6V 331 0
8 HD 76932 PM* 08 58 43.9327642391 -16 07 57.817644364 6.47 6.39 5.86     G2VFe-1.8CH-1 426 0
9 HD 88218 ** 10 09 31.7680664925 -35 51 24.404175359   6.73 6.13     G0V 151 0
10 * Y Vel PM* 10 31 21.8208713206 -53 42 55.740987419   5.39 4.89     F9VFe-0.8CH-0.7 173 0
11 HD 94028 PM* 10 51 28.1256073369 +20 16 38.965439278 8.51 8.69 8.22 7.82 7.54 F8 375 0
12 HD 102365 PM* 11 46 31.0725331317 -40 30 01.285867174 5.65 5.55 4.88 4.35 3.97 G2V 378 1
13 HD 106516 SB* 12 15 10.55731 -10 18 44.6354 6.44 6.57 6.11     F9VFe-1.7CH-0.7 443 0
14 HD 121384 SB* 13 56 32.9436065448 -54 42 16.783257240   6.78 6.01     G8VCH+0.3CaIwk 108 0
15 HD 132475 PM* 14 59 49.7651173448 -22 00 45.815162806 8.98 9.11 8.55     F5/6V 256 1
16 * nu.02 Lup PM* 15 21 48.1499105161 -48 19 03.469906910 6.35 6.30 5.65     G2-V 354 1
17 HD 140283 Pe* 15 43 03.0971190219 -10 56 00.595693188 7.508 7.711 7.212 6.63 8.21 F9VkA5mA1 985 0
18 HD 148816 PM* 16 30 28.4586254384 +04 10 41.602836534 7.75 7.81 7.28 6.82 6.49 F7V 329 0
19 V* V1033 Sco HXB 16 54 00.1423963019 -39 50 44.761701340       16.14   F3-6IV 1980 0
20 * w Her RG* 17 20 39.5674498400 +32 28 03.877958860 6.08 6.01 5.39 4.89 4.56 G0V 481 0
21 HD 157089 PM* 17 21 07.0564477831 +01 26 34.983929347 7.60 7.59 7.01 6.46 6.14 F8VgF8mF6 258 0
22 * ome Sgr SB* 19 55 50.3625499909 -26 17 57.693299065   5.45 4.70     G5IV 146 0
23 BD-18 5550 Pe* 19 58 49.7371417608 -18 12 11.140126164 10.18 10.03 9.35 9.04 8.74 CEMP-no 185 0
24 HD 193901 PM* 20 23 35.8471605389 -21 22 14.226959304 9.08 9.22 8.67 8.17 7.87 F7V 298 0
25 HD 194598 PM* 20 26 11.9183775668 +09 27 00.429558608 8.62 8.82 8.34 7.90 7.56 F8 315 0
26 HD 201891 Pe* 21 11 59.0321495469 +17 43 39.890919730 7.74 7.88 7.37 6.91 6.59 G5V_Fe-2.5 409 0
27 HD 201889 ** 21 11 59.52350 +24 10 05.3897 8.60 8.64 8.05 7.52 7.15 G1V 163 0
28 * gam Pav PM* 21 26 26.6049826473 -65 21 58.313057521 4.57 4.70 4.22 3.75 3.45 F9VFe-1.4CH-0.7 439 0
29 * nu. Ind ** 22 24 36.8853892493 -72 15 19.488237466   5.94 5.29     G9VFe-3.1CH-1.5 290 0

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