THE ARAUCARIA PROJECT: The FIRST-OVERTONE CLASSICAL CEPHEID in the ECLIPSING SYSTEM OGLE-LMC-CEP-2532

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dc.contributor.authorPilecki, Bogumił
dc.contributor.authorGraczyk, Dariusz
dc.contributor.authorGieren, Wolfgang
dc.contributor.authorPietrzyński, Grzegorz
dc.contributor.authorThompson, Ian B.
dc.contributor.authorSmolec, Radosław
dc.contributor.authorUdalski, Andrzej
dc.contributor.authorSoszyński, Igor
dc.contributor.authorKonorski, Piotr
dc.contributor.authorTaormina, Mónica
dc.contributor.authorGallenne, Alexandre
dc.contributor.authorMinniti, Dante
dc.date.accessioned2023-05-18T16:07:31Z
dc.date.available2023-05-18T16:07:31Z
dc.date.issued2015-06
dc.descriptionIndexación: Scopuses
dc.description.abstractWe present here the first spectroscopic and photometric analysis of the double-lined eclipsing binary containing the classical, first-overtone (FO) Cepheid OGLE-LMC-CEP-2532 (MACHO 81.8997.87). The system has an orbital period of 800 days and the Cepheid is pulsating with a period of 2.035 days. Using spectroscopic data from three high-class telescopes and photometry from three surveys spanning 7500 days, we are able to derive the dynamical masses for both stars with an accuracy better than 3%. This makes the Cepheid in this system one of a few lassical Cepheids with an accurate dynamical mass determination (M1 = 3.90 +:0.10 MM). The companion is probably slightly less massive (3.82 ±0.10 MM ), but may have the same mass within errors (M2 M1 = 0.981 ±0.015). The system has an age of about 185 million years and the Cepheid is in a more advanced evolutionary stage. For the first time precise parameters are derived for both stars in this system. Due to the lack of the secondary eclipse for many years, not much was known about the Cepheids companion. In our analysis, we used extra information from the pulsations and the orbital solution from the radial velocity curve. The best model predicts a grazing secondary eclipse shallower than 1 mmag, hence undetectable in the data, about 370 days after the primary eclipse. The dynamical mass obtained here is the most accurate known for a FO Cepheid and will contribute to the solution of the Cepheid mass discrepancy problem. © 2015. The American Astronomical Society. All rights reserved.es
dc.description.urihttps://iopscience-iop-org.recursosbiblioteca.unab.cl/article/10.1088/0004-637X/806/1/29
dc.identifier.citationAstrophysical Journal Volume 806, Issue 110 June 2015 Article number 29es
dc.identifier.doi10.1088/0004-637X/806/1/29
dc.identifier.issn0004-637X
dc.identifier.urihttps://repositorio.unab.cl/xmlui/handle/ria/49781
dc.language.isoenes
dc.publisherInstitute of Physics Publishinges
dc.rights.licenseAtribución 4.0 Internacional (CC BY 4.0)
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/deed.es
dc.subjectbinarieses
dc.subjecteclipsinges
dc.subjectgalaxieses
dc.subjectindividual (LMC)es
dc.subjectstarses
dc.subjectoscillationses
dc.subjectvariableses
dc.subjectCepheidses
dc.titleTHE ARAUCARIA PROJECT: The FIRST-OVERTONE CLASSICAL CEPHEID in the ECLIPSING SYSTEM OGLE-LMC-CEP-2532es
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