Volume 608, December 2017
|Number of page(s)||26|
|Section||Galactic structure, stellar clusters and populations|
|Published online||05 December 2017|
Constraining cosmic scatter in the Galactic halo through a differential analysis of metal-poor stars⋆
1 Universidade de São Paulo, Instituto de Astronomia, Geofísica e Ciências Atmosféricas, IAG, Departamento de Astronomia, rua do Matão 1226, Cidade Universitária, 05508-900, SP, Brazil
2 Max-Planck Institute for Astronomy, Konigstuhl 17, 69117 Heidelberg, Germany
3 Centre for Astrophysics Research, School of Physics, Astronomy and Mathematics, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK
4 Monash Centre for Astrophysics, School of Physics & Astronomy, Monash University, Clayton VIC 3800, Australia
5 Department of Physics, JINA Center for the Evolution of the Elements, University of Notre Dame, Notre Dame, IN 46556, USA
Received: 8 March 2017
Accepted: 1 September 2017
Context. The chemical abundances of metal-poor halo stars are important to understanding key aspects of Galactic formation and evolution.
Aims. We aim to constrain Galactic chemical evolution with precise chemical abundances of metal-poor stars (−2.8 ≤ [Fe/H] ≤ −1.5).
Methods. Using high resolution and high S/N UVES spectra of 23 stars and employing the differential analysis technique we estimated stellar parameters and obtained precise LTE chemical abundances.
Results. We present the abundances of Li, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Zn, Sr, Y, Zr, and Ba. The differential technique allowed us to obtain an unprecedented low level of scatter in our analysis, with standard deviations as low as 0.05 dex, and mean errors as low as 0.05 dex for [X/Fe].
Conclusions. By expanding our metallicity range with precise abundances from other works, we were able to precisely constrain Galactic chemical evolution models in a wide metallicity range (−3.6 ≤ [Fe/H] ≤ −0.4). The agreements and discrepancies found are key for further improvement of both models and observations. We also show that the LTE analysis of Cr II is a much more reliable source of abundance for chromium, as Cr I has important NLTE effects. These effects can be clearly seen when we compare the observed abundances of Cr I and Cr II with GCE models. While Cr I has a clear disagreement between model and observations, Cr II is very well modeled. We confirm tight increasing trends of Co and Zn toward lower metallicities, and a tight flat evolution of Ni relative to Fe. Our results strongly suggest inhomogeneous enrichment from hypernovae. Our precise stellar parameters results in a low star-to-star scatter (0.04 dex) in the Li abundances of our sample, with a mean value about 0.4 dex lower than the prediction from standard Big Bang nucleosynthesis; we also study the relation between lithium depletion and stellar mass, but it is difficult to assess a correlation due to the limited mass range. We find two blue straggler stars, based on their very depleted Li abundances. One of them shows intriguing abundance anomalies, including a possible zinc enhancement, suggesting that zinc may have been also produced by a former AGB companion.
Key words: stars: abundances / stars: evolution / stars: Population II / Galaxy: abundances / Galaxy: evolution / Galaxy: halo
Tables A.1–A.6 are also available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (220.127.116.11) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/608/A46
© ESO, 2017
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