AGB nucleosynthesis in the Large Magellanic Cloud: Detailed abundance analysis of the RV Tauri star MACHO 47.2496.8
2007 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 461, no 2, 641-650 p.Article in journal (Refereed) Published
Context. Abundance analysis of post-AGB objects as probes of AGB nucleosynthesis. Aims. A detailed photospheric abundance study is performed on the carbon-rich post-AGB candidate MACHO 47.2496.8 in the LMC. Methods. High-resolution, high signal-to-noise ESO VLT-UVES spectra of MACHO 47.2496.8 are analysed by performing detailed spectrum synthesis modelling using state-of-the-art carbon-rich MARCS atmosphere models. Results. The spectrum of MACHO 47.2496.8 is not only dominated by bands of carbon bearing molecules, but also by lines ofatomic transitions of s-process elements. The metallicity of [Fe/H] = -1.4 is surprisingly low for a field LMC star. The C/O ratio, however difficult to quantify, is greater than 2, and the s-process enrichment is large: the light s-process elements are enhanced by 1.2dex compared to iron ([Is/Fe] = +1.2), while for the heavy s-process elements an even stronger enrichment is measured: [hs/Fe] = +2.1. The lead abundance is comparable to the [hs/Fe]. With its low intrinsic metallicity and its luminosity at the low end of the carbon star luminosity function, the star represents likely the final stage of a low initial mass star. Conclusions. The LMC RVTauri star MACHO 47.2496.8 is highly carbon and s-process enriched, and is most probable a genuine post-C(N-type) AGB star. This is the first detailed abundance analysis of an extragalactic post-AGB star to date.
Place, publisher, year, edition, pages
2007. Vol. 461, no 2, 641-650 p.
Carbon oxygen ratio, Magellanic Clouds, Asymptotic giant branch, Low-mass stars, Luminosity function, Carbon stars, Luminosity, Heavy element, Light element, Metallicity, s process, Atmosphere model, RV Tauri stars, Stellar abundance, Large Magellanic Cloud, Nucleosynthesis
IdentifiersURN: urn:nbn:se:uu:diva-25622DOI: 10.1051/0004-6361:20065893ISI: 000243004700026OAI: oai:DiVA.org:uu-25622DiVA: diva2:53396