Insights into the chemical composition of the metal-poor Milky Way halo globular cluster NGC 6426

Hanke, M. and Koch, Andreas and Hansen, C.J. and McWilliam, A. (2017) Insights into the chemical composition of the metal-poor Milky Way halo globular cluster NGC 6426. Astronomy and Astrophysics, 599. ISSN 1432-0746

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Abstract

We present our detailed spectroscopic analysis of the chemical composition of four red giant stars in the halo globular cluster NGC 6426. We obtained high-resolution spectra using the Magellan2/MIKE spectrograph, from which we derived equivalent widths and subsequently computed abundances of 24 species of 22 chemical elements. For the purpose of measuring equivalent widths, we developed a new semi-automated tool, called EWCODE. We report a mean Fe content of [Fe/H] =−2.34 ± 0.05 dex (stat.) in accordance with previous studies. At a mean α-abundance of [(Mg, Si, Ca)/3 Fe] = 0.39 ± 0.03 dex, NGC 6426 falls on the trend drawn by the Milky Way halo and other globular clusters at comparably low metallicities. The distribution of the lighter α-elements as well as the enhanced ratio [Zn/Fe] = 0.39 dex could originate from hypernova enrichment of the pre-cluster medium. We find tentative evidence for a spread in the elements Mg, Si, and Zn, indicating an enrichment scenario, where ejecta of evolved massive stars of a slightly older population have polluted a newly born younger one. The heavy element abundances in this cluster fit well into the picture of metal-poor globular clusters, which in that respect appear to be remarkably homogeneous. The pattern of the neutron-capture elements heavier than Zn points toward an enrichment history governed by the r-process with little, if any, sign of s-process contributions. This finding is supported by the striking similarity of our program stars to the metal-poor field star HD 108317.

Item Type: Journal Article
Journal or Publication Title: Astronomy and Astrophysics
Uncontrolled Keywords: /dk/atira/pure/subjectarea/asjc/1900/1912
Subjects:
Departments: Faculty of Science and Technology > Physics
ID Code: 83767
Deposited By: ep_importer_pure
Deposited On: 21 Dec 2016 15:34
Refereed?: Yes
Published?: Published
Last Modified: 18 Feb 2020 02:57
URI: https://eprints.lancs.ac.uk/id/eprint/83767

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