Pulsating stars in ω Centauri. Near-IR properties and period-luminosity relations

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dc.contributor.authorNavarrete, C.
dc.contributor.authorCatelan, M.
dc.contributor.authorContreras Ramos, R.
dc.contributor.authorAlonso-García, J.
dc.contributor.authorGran, F.
dc.contributor.authorDékány, I.
dc.contributor.authorMinniti, D.
dc.date.accessioned2018-03-13T13:59:57Z
dc.date.available2018-03-13T13:59:57Z
dc.date.issued2017-09
dc.descriptionIndexación: Scopus.es_ES
dc.description.abstractω Centauri (NGC 5139) contains many variable stars of different types, including the pulsating type II Cepheids, RR Lyrae and SX Phoenicis stars. We carried out a deep, wide-field, near-infrared (IR) variability survey of ω Cen, using the VISTA telescope. We assembled an unprecedented homogeneous and complete J and KS near-IR catalog of variable stars in the field of ω Cen. In this paper we compare optical and near-IR light curves of RR Lyrae stars, emphasizing the main differences. Moreover, we discuss the ability of near-IR observations to detect SX Phoenicis stars given the fact that the amplitudes are much smaller in these bands compared to the optical. Finally, we consider the case in which all the pulsating stars in the three different variability types follow a single period-luminosity relation in the near-IR bands.es_ES
dc.description.urihttps://www.epj-conferences.org/articles/epjconf/pdf/2017/21/epjconf_puls2017_07005.pdf
dc.identifier.citationEPJ Web of Conferences Volume 152, 8 September 2017, Article number 07005es_ES
dc.identifier.issn2101-6275
dc.identifier.otherDOI: 10.1051/epjconf/201715207005
dc.identifier.urihttp://repositorio.unab.cl/xmlui/handle/ria/5426
dc.language.isoenes_ES
dc.publisherEDP Scienceses_ES
dc.rights.licenseAttribution 4.0 International (CC BY 4.0)
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/
dc.titlePulsating stars in ω Centauri. Near-IR properties and period-luminosity relationses_ES
dc.typeArtículoes_ES
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