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dc.contributor.authorLehmann, H.
dc.contributor.authorBorkovits, T.
dc.contributor.authorNgo, H.
dc.contributor.authorMawet, D.
dc.contributor.authorCsizmadia, Sz.
dc.contributor.authorRappaport, Saul A.
dc.contributor.authorForgacs-Dajka, E.
dc.date.accessioned2016-05-24T13:13:31Z
dc.date.available2016-05-24T13:13:31Z
dc.date.issued2016-02
dc.date.submitted2015-11
dc.identifier.issn1538-4357
dc.identifier.issn0004-637X
dc.identifier.urihttp://hdl.handle.net/1721.1/102651
dc.description.abstractKIC 7177553 was observed by the Kepler satellite to be an eclipsing eccentric binary star system with an 18-day orbital period. Recently, an eclipse timing study of the Kepler binaries has revealed eclipse timing variations (ETVs) in this object with an amplitude of ~100 s and an outer period of 529 days. The implied mass of the third body is that of a super-Jupiter, but below the mass of a brown dwarf. We therefore embarked on a radial velocity (RV) study of this binary to determine its system configuration and to check the hypothesis that it hosts a giant planet. From the RV measurements, it became immediately obvious that the same Kepler target contains another eccentric binary, this one with a 16.5-day orbital period. Direct imaging using adaptive optics reveals that the two binaries are separated by 0[" over .]4 (~167 AU) and have nearly the same magnitude (to within 2%). The close angular proximity of the two binaries and very similar γ velocities strongly suggest that KIC 7177553 is one of the rare SB4 systems consisting of two eccentric binaries where at least one system is eclipsing. Both systems consist of slowly rotating, nonevolved, solar-like stars of comparable masses. From the orbital separation and the small difference in γ velocity, we infer that the period of the outer orbit most likely lies in the range of 1000–3000 yr. New images taken over the next few years, as well as the high-precision astrometry of the Gaia satellite mission, will allow us to set much narrower constraints on the system geometry. Finally, we note that the observed ETVs in the Kepler data cannot be produced by the second binary. Further spectroscopic observations on a longer timescale will be required to prove the existence of the massive planet.en_US
dc.language.isoen_US
dc.publisherIOP Publishingen_US
dc.relation.isversionofhttp://dx.doi.org/10.3847/0004-637x/819/1/33en_US
dc.rightsArticle is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.en_US
dc.sourceIOP Publishingen_US
dc.titleKIC 7177553: A QUADRUPLE SYSTEM OF TWO CLOSE BINARIESen_US
dc.typeArticleen_US
dc.identifier.citationLehmann, H., T. Borkovits, S. A. Rappaport, H. Ngo, D. Mawet, Sz. Csizmadia, and E. Forgacs-Dajka. “KIC 7177553: A QUADRUPLE SYSTEM OF TWO CLOSE BINARIES.” The Astrophysical Journal 819, no. 1 (February 25, 2016): 33. © 2016 The American Astronomical Societyen_US
dc.contributor.departmentMassachusetts Institute of Technology. Department of Physicsen_US
dc.contributor.mitauthorRappaport, Saul A.en_US
dc.relation.journalThe Astrophysical Journalen_US
dc.eprint.versionFinal published versionen_US
dc.type.urihttp://purl.org/eprint/type/JournalArticleen_US
eprint.statushttp://purl.org/eprint/status/PeerRevieweden_US
dspace.orderedauthorsLehmann, H.; Borkovits, T.; Rappaport, S. A.; Ngo, H.; Mawet, D.; Csizmadia, Sz.; Forgacs-Dajka, E.en_US
dspace.embargo.termsNen_US
dc.identifier.orcidhttps://orcid.org/0000-0003-3182-5569
mit.licensePUBLISHER_POLICYen_US


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