EPIC 219217635: a doubly eclipsing quadruple system containing an evolved binary

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  • T. Borkovits, Hungarian Acad Sci, Hungarian Academy of Sciences, Res Ctr Astron & Earth Sci, Konkoly Observ
  • ,
  • S. Albrecht
  • S. Rappaport, MIT, Massachusetts Institute of Technology (MIT), Kavli Inst Astrophys & Space Res
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  • L. Nelson, Bishops Univ, Bishops University, Dept Phys & Astron
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  • A. Vanderburg, Univ Texas Austin, University of Texas Austin, Dept Astron
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  • B. L. Gary, Hereford Arizona Observ
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  • T. G. Tan, Perth Exoplanet Survey Telescope
  • ,
  • A. B. Justesen
  • M. H. Kristiansen, Tech Univ Denmark, Technical University of Denmark, DTU Space, Natl Space Inst, Dept Math & Computat Geosci, Brorfelde Observ
  • ,
  • T. L. Jacobs
  • ,
  • D. LaCourse
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  • H. Ngo, CALTECH, California Institute of Technology, Div Geol & Planetary Sci
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  • N. Wallack, CALTECH, California Institute of Technology, Div Geol & Planetary Sci
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  • G. Ruane, CALTECH, California Institute of Technology, Dept Astron
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  • D. Mawet, CALTECH, Jet Prop Lab, Infrared Proc & Anal Ctr
  • ,
  • S. B. Howell, NASA, Ames Research Center, National Aeronautics & Space Administration (NASA), Ames Res Ctr, Space Sci & Astrobiol Div
  • ,
  • R. Tronsgaard, Nord Opt Telescope

We have discovered a doubly eclipsing, bound, quadruple star system in the field of K2 Campaign 7. EPIC 219217635 is a stellar image with K-p = 12.7 that contains an eclipsing binary (EB) with P-A = 3.59470 d and a second EB with P-B = 0.61825 d. We have obtained follow-up radial velocity (RV) spectroscopy observations, adaptive optics imaging, and ground-based photometric observations. From our analysis of all the observations, we derive good estimates for a number of the system parameters. We conclude that (1) both binaries are bound in a quadruple star system; (2) a linear trend to the RV curve of binary A is found over a 2-yr interval, corresponding to an acceleration, = 0.0024 +/- 0.0007 cm s(-2); (3) small irregular variations are seen in the eclipse timing variations (ETVs) detected over the same interval; (4) the orbital separation of the quadruple system is probably in the range of 8-25 au; and (5) the orbital planes of the two binaries must be inclined with respect to each other by at least 25 degrees. In addition, we find that binary B is evolved, and the cooler and currently less massive star has transferred much of its envelope to the currently more massive star. We have also demonstrated that the system is sufficiently bright that the eclipses can be followed using small ground-based telescopes, and that this system may be profitably studied over the next decade when the outer orbit of the quadruple is expected to manifest itself in the ETV and/or RV curves.

Original languageEnglish
JournalMonthly Notices of the Royal Astronomical Society
Pages (from-to)5135-5152
Number of pages18
Publication statusPublished - Aug 2018

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