Kovtyukh V.Wallerstein G.Yegorova I.Andrievsky S.Korotin S.Saviane I.Belik S.Davis C.E.Farrell E.M.2022-08-172022-08-172018-05Publications of the Astronomical Society of the Pacific Volume 130, Issue 987May 2018 Article number 05420100046280https://repositorio.unab.cl/xmlui/handle/ria/23563Indexación ScopusWe have analyzed 10 high-resolution spectra of Type II Cepheids with periods less than 3 days. We find that they clearly separate into two groups: those with near or slightly below solar metallicities, and those with [Fe/H] between −1.5 and −2.0. While the former are usually called BLHer stars, we suggest that the latter be called UYEri stars. The UYEri subclass appears to be similar to the short period variables in globular clusters of the Galactic Halo. Globular clusters with [Fe/H] > −1.0 almost never have Type II Cepheids. © 2018. The Astronomical Society of the Pacific. All rights reserved.enPeriodMagellanic CloudsGlobular ClustersGlobular clusters: generalStars: abundances, variable: cepheidsArtículo10.1088/1538-3873/aaacf7