An extreme-mass ratio, short-period eclipsing binary consisting of a B dwarf primary and a pre-main-sequence M star companion discovered by KELT
Author
Stevens, Daniel JZhou, George
Johnson, Marshall C
Rizzuto, Aaron C
Rodriguez, Joseph E
Bieryla, Allyson
Collins, Karen A
Villanueva, Steven
Wright, Jason T
Gaudi, B Scott
Latham, David W
Beatty, Thomas G
Lund, Michael B
Siverd, Robert J
Kraus, Adam L
Wachiraphan, Patcharapol
Berlind, Perry
Calkins, Michael L
Esquerdo, Gilbert A
Kielkopf, John F
Kuhn, Rudolf B
Manner, Mark
Pepper, Joshua
Stassun, Keivan G
Affiliation
Univ Arizona, Dept AstronUniv Arizona, Steward Observ
Issue Date
2020-10-12
Metadata
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OXFORD UNIV PRESSCitation
Stevens, D. J., Zhou, G., Johnson, M. C., Rizzuto, A. C., Rodriguez, J. E., Bieryla, A., ... & Stassun, K. G. (2020). An extreme-mass ratio, short-period eclipsing binary consisting of a B dwarf primary and a pre-main-sequence M star companion discovered by KELT. Monthly Notices of the Royal Astronomical Society, 499(3), 3775-3791.Rights
© 2020 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
We present the discovery of KELT J072709 + 072007 (IED 58730), a very low mass ratio (q M-2/M-1 approximate to 0.07) eclipsing binary (EB) identified by the Kilodegree Extremely Little Telescope (KELT) survey. We present the discovery light curve and perform a global analysis of four high-precision ground-based light curves, the Transiting Exoplanets Survey Satellite (TESS) light curve, radial velocity (RV) measurements, Doppler Tomography (DT) measurements, and the broad-band spectral energy distribution. Results from the global analysis are consistent with a fully convective (M-2 = 0.22 +/- 0.02 M-circle dot) M star transiting a late-B primary (M-1 = 3.34(-0.09)(+0.07) M-circle dot and T-eff,T-1 = 11960(-520)(+430) K). We infer that the primary star is 183(-30)(+33) Myr old and that the companion star's radius is inflated by 26 +/- 8 per cent relative to the predicted value from a low-mass isochrone of similar age. We separately and analytically fit for the variability in the out-of-eclipse TESS phase curve, finding good agreement between the resulting stellar parameters and those from the global fit. Such systems are valuable for testing theories of binary star formation and understanding how the environment of a star in a close-but-detached binary affects its physical properties. In particular, we examine how a star's properties in such a binary might differ from the properties it would have in isolation.ISSN
0035-8711EISSN
1365-2966Version
Final published versionSponsors
Pennsylvania State Universityae974a485f413a2113503eed53cd6c53
10.1093/mnras/staa3142