Volume 595, November 2016
|Number of page(s)||6|
|Published online||31 October 2016|
III. An ultra iron-poor multiple CEMP system ⋆
1 GEPI, Observatoire de Paris, PSL Research University, CNRS, Univ. Paris Diderot, Sorbonne Paris Cité, Place Jules Janssen, 92190 Meudon, France
2 Departamento de Ciencias Fisicas, Universidad Andres Bello, 220 Republica, Santiago, Chile
3 European Southern Observatory, Casilla 19001, Santiago, Chile
4 UPJV, Université de Picardie Jules Verne, 33 rue St Leu, 80080 Amiens, France
5 Laboratoire Univers et Particules de Montpellier, LUPM, Université de Montpellier, CNRS, 34095 Montpellier Cedex 5, France
6 Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5, 35122 Padova, Italy
7 Zentrum für Astronomie der Universität Heidelberg, Landessternwarte, Königstuhl 12, 69117 Heidelberg, Germany
8 Phyics Department, Lancaster University, Lancaster LA1 4YB, UK
9 Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany
10 Zentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik, Albert-Ueberle-Straβ 2, 69120 Heidelberg, Germany
11 Interdisziplinäres Zentrum für Wissenschaftliches Rechnen (IWR) der Universität Heidelberg
Received: 22 September 2016
Accepted: 7 October 2016
Aims. One of the primary objectives of the TOPoS survey is to search for the most metal-poor stars. Our search has led to the discovery of one of the most iron-poor objects known, SDSS J092912.32+023817.0. This object is a multiple system, in which two components are clearly detected in the spectrum.
Methods. We have analysed 16 high-resolution spectra obtained using the UVES spectrograph at the ESO 8.2 m VLT telescope to measure radial velocities and determine the chemical composition of the system.
Results. Cross correlation of the spectra with a synthetic template yields a double-peaked cross-correlation function (CCF) for eight spectra, and in one case there is evidence for the presence of a third peak. Chemical analysis of the spectrum obtained by averaging all the spectra for which the CCF showed a single peak found that the iron abundance is [Fe/H] = −4.97. The system is also carbon enhanced with [C/Fe] = +3.91 (A(C) = 7.44). From the permitted oxygen triplet we determined an upper limit for oxygen of [O/Fe] < +3.52 such that C/O > 1.3. We are also able to provide more stringent upper limits on the Sr and Ba abundances ([Sr/Fe] < +0.70, and [Ba/Fe] < +1.46, respectively).
Key words: stars: Population II / stars: abundances / binaries: spectroscopic / Galaxy: abundances / Galaxy: formation / Galaxy: halo
© ESO, 2016
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