# 2012A&A...544A.102B

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 Query : 2012A&A...544A.102B

2012A&A...544A.102B - Astronomy and Astrophysics, volume 544A, 102-102 (2012/8-1)

An upper limit on the sulphur abundance in HE 1327-2326.

BONIFACIO P., CAFFAU E., VENN K.A. and LAMBERT D.L.

Abstract (from CDS):

Star HE1327-2326 is a unique object, with the lowest measured iron abundance ([Fe/H]~-6) and a peculiar chemical composition that includes large overabundances of C, N, and O with respect to iron. One important question is whether the chemical abundances in this star reflect the chemical composition of the gas cloud from which it was formed or if they have been severely affected by other processes, such as dust-gas winnowing. We measure or provide an upper limit to the abundance of the volatile element sulphur, which can help to discriminate between the two scenarios. We observed HE1327-2326 with the high resolution infra-red spectrograph CRIRES at the VLT to observe the SI lines of Multiplet 3 at 1045nm. We do not detect the SI line. A 3σ upper limit on the equivalent width (EW) of any line in our spectrum is EW<0.66pm. Using either one-dimensional static or three-dimensional hydrodynamical model-atmospheres, this translates into a robust upper limit of [S/H]←2.6. This upper limit does not provide conclusive evidence for or against dust-gas winnowing, and the evidence coming from other elements (e.g., Na and Ti) is also inconclusive or contradictory. The formation of dust in the atmosphere versus an origin of the metals in a metal-poor supernova with extensive fall-back'' are not mutually exclusive. It is possible that dust formation distorts the peculiar abundance pattern created by a supernova with fall-back, thus the abundance ratios in HE1327-2326 may be used to constrain the properties of the supernova(e) that produced its metals, but with some caution.

Journal keyword(s): stars: abundances - stars: individual: HE 1327-2326 - stars: Population II - Galaxy: evolution - Galaxy: abundances - line: formation

Full paper

 Number of rows : 9
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 HE 0107-5240 Pe* 01 09 29.1555567432 -52 24 34.202039148   15.89 15.07 15.10 14.283 CEMP-no 235 0
2 V* UY CMa RV* 06 18 16.3755429480 -17 02 34.676976156   11.55 10.80     G0V 41 0
3 V* PS Gem pA* 07 03 39.6305052432 +10 46 13.068774048   7.76 7.37     A0 113 0
4 HD 89353 pA* 10 18 07.5899342712 -28 59 31.195183524   5.76 5.53     B9.5Ib/II 299 0
5 UCAC3 215-112497 Pe* 10 29 15.1489854864 +17 29 27.924626724         15.98 ~ 101 0
6 HE 1327-2326 Pe* 13 30 05.9394958608 -23 41 49.699340844 13.761 14.01 13.55 13.50 12.803 CEMP-no 229 0
7 HD 140283 Pe* 15 43 03.0971190219 -10 56 00.595693188 7.508 7.711 7.212 6.63 8.21 F9VkA5mA1 899 0
8 V* HP Lyr pA* 19 21 39.0673459320 +39 56 08.202817716   11.12 10.38 10.15 9.615 A3Ia/Iab 56 1
9 SN 2008ha SN* 23 34 52.69 +18 13 35.4           SNIax 171 1

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2022.11.29-19:21:11