A spectroscopic study of the globular cluster M28 (NGC 6626)

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dc.contributor.authorVillanova, S.
dc.contributor.authorMoni Bidin, C.
dc.contributor.authorMauro, F.
dc.contributor.authorMunoz, C.
dc.contributor.authorMonaco, L.
dc.date.accessioned2022-07-28T23:51:26Z
dc.date.available2022-07-28T23:51:26Z
dc.date.issued2017-01
dc.descriptionIndexación Scopuses
dc.description.abstractWe present the abundance analysis for a sample of 17 red giant branch stars in the metal-poor globular cluster M28 based on high-resolution spectra. This is the first extensive spectroscopic study of this cluster. We derive abundances of O, Na, Mg, Al, Si, Ca, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Zn, Y, Zr, Ba, La, Ce, and Eu. We find a metallicity of [Fe/H]=-1.29 ± 0.01 and an a-enhancement of +0.34 ± 0.01 (errors on the mean), typical of halo globular clusters in this metallicity regime. A large spread is observed in the abundances of light elements O, Na, and Al. Mg also shows an anti-correlation with Al with a significance of 3σ. The cluster shows a Na-O anti-correlation and a Na-Al correlation. This correlation is not linear but 'segmented' and that the stars are not distributed continuously, but form at least three well-separated subpopulations. In this aspect, M28 resembles NGC 2808 that was found to host at least five sub-populations. The presence of a Mg-Al anti-correlation favour massive AGB stars as the main polluters responsible for the multiple-population phenomenon. © 2016 The Authors.es
dc.identifier.citationMonthly Notices of the Royal Astronomical Society Volume 464, Issue 3, Pages 2730 - 274021 January 2017es
dc.identifier.doi10.1093/mnras/stw2509
dc.identifier.issn0035-8711
dc.identifier.urihttps://repositorio.unab.cl/xmlui/handle/ria/23376
dc.language.isoenes
dc.publisherMonthly Notices of the Royal Astronomical Societyes
dc.subjectGlobulares
dc.subjectclusters:es
dc.subjectindividual:es
dc.subjectM28es
dc.subject(NGC 6626)es
dc.titleA spectroscopic study of the globular cluster M28 (NGC 6626)es
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