Assessing the effect of stellar companions from high-resolution imaging of Kepler objects of interest
Article
Article Title | Assessing the effect of stellar companions from high-resolution imaging of Kepler objects of interest |
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ERA Journal ID | 1048 |
Article Category | Article |
Authors | Hirsch, Lea A. (Author), Ciardi, David R. (Author), Howard, Andrew W. (Author), Everett, Mark E. (Author), Furlan, Elise (Author), Saylors, Mindy (Author), Horch, Elliott P. (Author), Howell, Steve B. (Author), Teske, Johanna (Author) and Marcy, Geoffrey W. (Author) |
Journal Title | The Astronomical Journal |
Journal Citation | 153 (3) |
Article Number | 117 |
Number of Pages | 17 |
Year | 2017 |
Publisher | IOP Publishing |
Place of Publication | United States |
ISSN | 0004-6256 |
1538-3881 | |
Digital Object Identifier (DOI) | https://doi.org/10.3847/1538-3881/153/3/117 |
Web Address (URL) | https://iopscience.iop.org/article/10.3847/1538-3881/153/3/117 |
Abstract | We report on 176 close (<2″) stellar companions detected with high-resolution imaging near 170 hosts of Kepler Objects of Interest (KOIs). These Kepler targets were prioritized for imaging follow-up based on the presence of small planets, so most of the KOIs in these systems (176 out of 204) have nominal radii <6R. Each KOI in our sample was observed in at least two filters with adaptive optics, speckle imaging, lucky imaging, or the Hubble Space Telescope. Multi-filter photometry provides color information on the companions, allowing us to constrain their stellar properties and assess the probability that the companions are physically bound. We find that 60%-80% of companions within 1″ are bound, and the bound fraction is >90% for companions within 0.″5; the bound fraction decreases with increasing angular separation. This picture is consistent with simulations of the binary and background stellar populations in the Kepler field. We also reassess the planet radii in these systems, converting the observed differential magnitudes to a contamination in the Kepler bandpass and calculating the planet radius correction factor, X R = R p(true)/R p(single). Under the assumption that planets in bound binaries are equally likely to orbit the primary or secondary, we find a mean radius correction factor for planets in stellar multiples of X R = 1.65. If stellar multiplicity in the Kepler field is similar to the solar neighborhood, then nearly half of all Kepler planets may have radii underestimated by an average of 65%, unless vetted using high-resolution imaging or spectroscopy. |
Keywords | binaries; visual; planets and satellites; detection; planets and satellites; fundamental parameters; techniques; high angular resolution |
Contains Sensitive Content | Does not contain sensitive content |
ANZSRC Field of Research 2020 | 519999. Other physical sciences not elsewhere classified |
Public Notes | For access to this article, please click on the URL link provided. |
Byline Affiliations | University of California, United States |
National Aeronautics and Space Administration (NASA), United States | |
California Institute of Technology (Caltech), United States | |
National Optical Astronomy Observatory, United States | |
Southern Connecticut State University, United States | |
Carnegie Institution of Washington, United States | |
Institution of Origin | University of Southern Queensland |
https://research.usq.edu.au/item/q4349/assessing-the-effect-of-stellar-companions-from-high-resolution-imaging-of-kepler-objects-of-interest
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