THE DISTANCE TO THE LARGE MAGELLANIC CLOUD CLUSTER NGC 1866 FROM ITS CEPHEID MEMBERS

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dc.contributor.authorGIEREN, WP
dc.contributor.authorRICHTLER, T
dc.contributor.authorHILKER, M
dc.date.accessioned2025-01-21T01:35:13Z
dc.date.available2025-01-21T01:35:13Z
dc.date.issued1994
dc.description.abstractWe have derived distances to four Cepheid variables of similar periods (2.6-3.5 days) in the field of the young LMC cluster NGC 1866 using the visual surface brightness modification of the Baade-Wesselink method. For three of these variables, consistent distances are obtained which support their cluster membership and yield a true cluster distance modulus of 18.47 +/- 0.20 mag. The distances have been corrected for the nonsolar metallicity of -0.6 dex recently determined for NGC 1866 by Hilker et al. A fourth Cepheid, HV 12204, is shown to have a bright blue companion star which invalidates the Baade-Wesselink analysis; this Cepheid is likely to be a cluster member in a spectroscopic binary system.
dc.description.abstractWe determine the radii of the variables and find consistent values in the narrow range between 26 and 31 R., which agree very well with the values expected from the galactic Cepheid period-radius relation.
dc.fuente.origenWOS
dc.identifier.issn0004-637X
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/97654
dc.identifier.wosidWOS:A1994PJ92700006
dc.issue.numero2
dc.language.isoen
dc.pagina.finalL76
dc.pagina.inicioL73
dc.revistaAstrophysical journal
dc.rightsacceso restringido
dc.subjectCEPHEIDS
dc.subjectGALAXIES, STAR CLUSTERS
dc.subjectMAGELLANIC CLOUDS
dc.titleTHE DISTANCE TO THE LARGE MAGELLANIC CLOUD CLUSTER NGC 1866 FROM ITS CEPHEID MEMBERS
dc.typeartículo
dc.volumen433
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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