| Issue |
A&A
Volume 624, April 2019
|
|
|---|---|---|
| Article Number | A44 | |
| Number of page(s) | 9 | |
| Section | Stellar atmospheres | |
| DOI | https://doi.org/10.1051/0004-6361/201834741 | |
| Published online | 05 April 2019 | |
Be and O in the ultra metal-poor dwarf 2MASS J18082002-5104378: the Be–O correlation★,★★
1
GEPI, Observatoire de Paris, Université PSL, CNRS, Place Jules Janssen,
92190 Meudon, France
e-mail: monique.spite@obspm.fr
2
European Southern Observatory,
Casilla 19001,
Santiago, Chile
3
Max Planck Institut für Astronomie,
69117 Heidelberg, Germany
Received:
29
November
2018
Accepted:
14
February
2019
Context. Measurable amounts of Be could have been synthesised primordially if the Universe were non-homogeneous or in the presence of late decaying relic particles.
Aims. We investigate the Be abundance in the extremely metal-poor star 2MASS J1808-5104 ([Fe/H] = −3.84) with the aim of constraining inhomogeneities or the presence of late decaying particles.
Methods. High resolution, high signal-to-noise ratio (S/N) UV spectra were acquired at ESO with the Kueyen 8.2 m telescope and the UVES spectrograph. Abundances were derived using several model atmospheres and spectral synthesis code.
Results. We measured log(Be/H) = −14.3 from a spectrum synthesis of the region of the Be line. Using a conservative approach, however we adopted an upper limit two times higher, i.e. log(Be/H) < −14.0. We measured the O abundance from UV–OH lines and find [O/H] = −3.46 after a 3D correction.
Conclusions. Our observation reinforces the existing upper limit on primordial Be. There is no observational indication for a primordial production of 9Be. This places strong constraints on the properties of putative relic particles. This result also supports the hypothesis of a homogeneous Universe, at the time of nucleosynthesis. Surprisingly, our upper limit of the Be abundance is well below the Be measurements in stars of similar [O/H]. This may be evidence that the Be–O relation breaks down in the early Galaxy, perhaps due to the escape of spallation products from the gas clouds in which stars such as 2MASS J1808-5104 have formed.
Key words: stars: abundances / binaries: spectroscopic / stars: Population II / stars: individual: 2MASS J18082002-5104378
Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes 101.A-0229(A), (PI M.Spite) and 293.D-5036 (PI J. Mélendez). This research has also made use of Keck Observatory Archive (KOA), operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration (PI A. Boesgaard).
The 3D values of the oxygen abundance are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/624/A44
© M. Spite et al. 2019
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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