CaltechAUTHORS
  A Caltech Library Service

The Five Planets in the Kepler-296 Binary System All Orbit the Primary: A Statistical and Analytical Analysis

Barclay, Thomas and Quintana, Elisa V. and Adams, Fred C. and Ciardi, David R. and Huber, Daniel and Foreman-Mackey, Daniel and Montet, Benjamin T. and Caldwell, Douglas (2015) The Five Planets in the Kepler-296 Binary System All Orbit the Primary: A Statistical and Analytical Analysis. Astrophysical Journal, 809 (1). Art. No. 7. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20151016-154325352

[img] PDF - Published Version
See Usage Policy.

957Kb
[img] PDF - Submitted Version
See Usage Policy.

1295Kb

Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20151016-154325352

Abstract

Kepler-296 is a binary star system with two M-dwarf components separated by 0 2. Five transiting planets have been confirmed to be associated with the Kepler-296 system; given the evidence to date, however, the planets could in principle orbit either star. This ambiguity has made it difficult to constrain both the orbital and physical properties of the planets. Using both statistical and analytical arguments, this paper shows that all five planets are highly likely to orbit the primary star in this system. We performed a Markov-Chain Monte Carlo simulation using a five transiting planet model, leaving the stellar density and dilution with uniform priors. Using importance sampling, we compared the model probabilities under the priors of the planets orbiting either the brighter or the fainter component of the binary. A model where the planets orbit the brighter component, Kepler-296A, is strongly preferred by the data. Combined with our assertion that all five planets orbit the same star, the two outer planets in the system, Kepler-296 Ae and Kepler-296 Af, have radii of 1.53 ± 0.26 and 1.80 ± 0.31 R⊕, respectively, and receive incident stellar fluxes of 1.40 ± 0.23 and 0.62 ± 0.10 times the incident flux the Earth receives from the Sun. This level of irradiation places both planets within or close to the circumstellar habitable zone of their parent star.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/809/1/7 DOIArticle
http://iopscience.iop.org/article/10.1088/0004-637X/809/1/7/metaPublisherArticle
http://arxiv.org/abs/1505.01845arXivDiscussion Paper
ORCID:
AuthorORCID
Barclay, Thomas0000-0001-7139-2724
Adams, Fred C.0000-0002-8167-1767
Ciardi, David R.0000-0002-5741-3047
Huber, Daniel0000-0001-8832-4488
Foreman-Mackey, Daniel0000-0002-9328-5652
Montet, Benjamin T.0000-0001-7516-8308
Caldwell, Douglas0000-0003-1963-9616
Additional Information:© 2015 The American Astronomical Society. Received 2015 March 7; accepted 2015 May 7; published 2015 August 4. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission Directorate. We would like to express our gratitude to all those who have worked on the Kepler pipeline over the many years of the Kepler mission. Some Kepler data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute (STScI). 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. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. This work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Some of the data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. 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 Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. E.V.Q. is supported by a NASA Senior Fellowship at the Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. B.T.M. is supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE1144469. D.H. acknowledges support by the Australian Research Council's Discovery Projects funding scheme (project number DE140101364) and support by the National Aeronautics and Space Administration under Grant NNX14AB92G issued through the Kepler Participating Scientist Program.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASANAS5-26555
NASANNX09AF08G
W. M. Keck FoundationUNSPECIFIED
NASA Senior FellowshipUNSPECIFIED
NSF Graduate Research FellowshipDGE1144469
Australian Research Council (ARC)DE140101364
NASANNX14AB92G
Subject Keywords:binaries: general – methods: data analysis – methods: statistical – planetary systems – stars: individual (Kepler-296, KIC 11497958, KOI-1422) – techniques: photometric
Issue or Number:1
Record Number:CaltechAUTHORS:20151016-154325352
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20151016-154325352
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:61237
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:16 Oct 2015 22:51
Last Modified:09 Mar 2020 13:19

Repository Staff Only: item control page