Variability Survey of ω Centauri in the Near-IR: Period-Luminosity Relations

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dc.catalogadorpau
dc.contributor.authorNavarrete, C.
dc.contributor.authorCatelan, Marcio
dc.contributor.authorContreras Ramos, R.
dc.contributor.authorGran, F.
dc.contributor.authorAlonso-García, J.
dc.contributor.authorDékány, I.
dc.date.accessioned2024-03-05T15:14:47Z
dc.date.available2024-03-05T15:14:47Z
dc.date.issued2017
dc.description.abstractω Centauri is by far the most massive globular star cluster in the Milky Way, and possibly the remnant of a dwarf galaxy. As such, it contains a large number of variable stars of different classes. Here we report on an extensive, wide-field time-series study of ω Cen in the J and K S bands, which has allowed us to study the near-IR period-luminosity relations for different variability classes, including the first such relations for the SX Phoenicis stars.
dc.fuente.origenORCID
dc.identifier.doi10.1017/S1743921315009059
dc.identifier.urihttps://doi.org/10.1017/S1743921315009059
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/84034
dc.identifier.wosidWOS:000456237800084
dc.information.autorucInstituto de Astrofísica; Catelan , Marcio; 0000-0001-6003-8877; 1001556
dc.language.isoen
dc.nota.accesocontenido parcial
dc.rightsacceso restringido
dc.titleVariability Survey of ω Centauri in the Near-IR: Period-Luminosity Relations
dc.typecomunicación de congreso
sipa.codpersvinculados1001556
sipa.trazabilidadORCID;2024-01-22
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