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Characterizing the Cool KOIs. V. KOI-256: A Mutually Eclipsing Post-common Envelope Binary

Muirhead, Philip S. and Shporer, Avi and Becker, Juliette and Swift, Jonathan J. and Fuller, Jim and Hinkley, Sasha and Pineda, J. Sebastian and Bottom, Michael and Howard, Andrew W. and von Braun, Kaspar and Baranec, Christoph and Riddle, Reed and Tendulkar, Shriharsh P. and Bui, Khanh and Dekany, Richard and Johnson, John Asher (2013) Characterizing the Cool KOIs. V. KOI-256: A Mutually Eclipsing Post-common Envelope Binary. Astrophysical Journal, 767 (2). Art. No. 111. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20130521-132637224

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Abstract

We report that Kepler Object of Interest 256 (KOI-256) is a mutually eclipsing post-common envelope binary (ePCEB), consisting of a cool white dwarf (M_★ = 0.592 ± 0.089 M_☉, R_★ = 0.01345 ± 0.00091 R_☉, T_(eff) = 7100 ± 700 K) and an active M3 dwarf (M_★ = 0.51 ± 0.16 M_☉, R_★ = 0.540 ± 0.014 R_☉, T_(eff) = 3450 ± 50 K) with an orbital period of 1.37865 ± 0.00001 days. KOI-256 is listed as hosting a transiting planet-candidate by Borucki et al. and Batalha et al.; here we report that the planet-candidate transit signal is in fact the occultation of a white dwarf as it passes behind the M dwarf. We combine publicly-available long- and short-cadence Kepler light curves with ground-based measurements to robustly determine the system parameters. The occultation events are readily apparent in the Kepler light curve, as is spin-orbit synchronization of the M dwarf, and we detect the transit of the white dwarf in front of the M dwarf halfway between the occultation events. The size of the white dwarf with respect to the Einstein ring during transit (R_(Ein) = 0.00473 ± 0.00055 R ☉) causes the transit depth to be shallower than expected from pure geometry due to gravitational lensing. KOI-256 is an old, long-period ePCEB and serves as a benchmark object for studying the evolution of binary star systems as well as white dwarfs themselves, thanks largely to the availability of near-continuous, ultra-precise Kepler photometry.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/767/2/111DOIArticle
http://iopscience.iop.org/0004-637X/767/2/111/PublisherArticle
ORCID:
AuthorORCID
Muirhead, Philip S.0000-0002-0638-8822
Shporer, Avi0000-0002-1836-3120
Becker, Juliette0000-0002-7733-4522
Swift, Jonathan J.0000-0002-9486-818X
Fuller, Jim0000-0002-4544-0750
Hinkley, Sasha0000-0001-8074-2562
Pineda, J. Sebastian0000-0002-4489-0135
Bottom, Michael0000-0003-1341-5531
Howard, Andrew W.0000-0001-8638-0320
von Braun, Kaspar0000-0002-5823-4630
Baranec, Christoph0000-0002-1917-9157
Riddle, Reed0000-0002-0387-370X
Tendulkar, Shriharsh P.0000-0003-2548-2926
Additional Information:© 2013 American Astronomical Society. Received 2013 January 2; accepted 2013 March 7; published 2013 April 2. We would like to thank Eric Agol, Jean-Michel Désert, Dong Lai, Dylan Morgan, Tony Piro and Andrew West for their insightful communications about this system. We would like to thank the anonymous referee for the thoughtful and constructive comments. We would like to thank the staff at Palomar Observatory for providing support during our many observation runs, including Bruce Baker, Mike Doyle, Jamey Eriksen, Carolyn Heffner, John Henning, Steven Kunsman, Dan McKenna, Jean Mueller, Kajsa Peffer, Kevin Rykoski, and Greg van Idsinga. J. Becker would like to thank Mr. and Mrs. Kenneth Adelman for providing funding for her 2012 Alain Porter Memorial SURF Fellowship. A portion of this work was supported by the National Science Foundation under grant No. AST-1203023. The Robo-AO system is supported by collaborating partner institutions, the California Institute of Technology and the Inter-University Centre for Astronomy and Astrophysics, by the National Science Foundation under grant Nos. AST-0906060 and AST-0960343, by a grant from the Mt. Cuba Astronomical Foundation and by a gift from Samuel Oschin. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has within the indigenous Hawaiian community. Facilities: GALEX, Keck:I (HIRES), Keck:II (ESI), Kepler, PO:1.5m (Robo-AO), Hale (TripleSpec, WIRC)
Funders:
Funding AgencyGrant Number
Alain Porter Memorial SURF FellowshipUNSPECIFIED
NSFAST-1203023
Inter-University Centre for Astronomy and AstrophysicsUNSPECIFIED
NSFAST-0906060
NSFAST-0960343
Mt. Cuba Astronomical FoundationUNSPECIFIED
Samuel OschinUNSPECIFIED
Caltech Summer Undergraduate Research Fellowship (SURF)UNSPECIFIED
NASANAS5-26555
NASANNX09AF08G
W. M. Keck FoundationUNSPECIFIED
Subject Keywords:binaries: eclipsing; binaries: spectroscopic; stars: abundances; stars: activity; stars: fundamental parameters; stars: individual (KOI-256); stars: late-type; stars: low-mass; stars: rotation
Issue or Number:2
Record Number:CaltechAUTHORS:20130521-132637224
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20130521-132637224
Official Citation:Characterizing the Cool KOIs. V. KOI-256: A Mutually Eclipsing Post-common Envelope Binary Philip S. Muirhead et al. 2013 ApJ 767 111
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:38612
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:21 May 2013 21:08
Last Modified:03 Oct 2019 04:58

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