The Kepler follow-up observation program. I. A catalog of companions to Kepler stars from high-resolution imaging
Article
Article Title | The Kepler follow-up observation program. I. A catalog of companions to Kepler stars from high-resolution imaging |
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ERA Journal ID | 1048 |
Article Category | Article |
Authors | Furlan, E. (Author), Ciardi, D. R. (Author), Everett, M. E. (Author), Saylors, M. (Author), Teske, J. K. (Author), Horch, E. P. (Author), Howell, S. B. (Author), van Belle, G. T. (Author), Hirsch, L. A. (Author), Gautier, T. N. (Author), Adams, E. R. (Author), Barrado, D. (Author), Cartier, K. M. S. (Author), Dressing, C. D. (Author), Dupree, A. K. (Author), Gilliland, R. L. (Author), Lillo-Box, J. (Author), Lucas, P. W. (Author) and Wang, J. (Author) |
Journal Title | The Astronomical Journal |
Journal Citation | 153 (2) |
Article Number | 71 |
Number of Pages | 33 |
Year | 2017 |
Publisher | IOP Publishing |
Place of Publication | United States |
ISSN | 0004-6256 |
1538-3881 | |
Digital Object Identifier (DOI) | https://doi.org/10.3847/1538-3881/153/2/71 |
Web Address (URL) | https://iopscience.iop.org/article/10.3847/1538-3881/153/2/71 |
Abstract | We present results from high-resolution, optical to near-IR imaging of host stars of Kepler Objects of Interest (KOIs), identified in the original Kepler field. Part of the data were obtained under the Kepler imaging follow-up observation program over six years (2009-2015). Almost 90% of stars that are hosts to planet candidates or confirmed planets were observed. We combine measurements of companions to KOI host stars from different bands to create a comprehensive catalog of projected separations, position angles, and magnitude differences for all detected companion stars (some of which may not be bound). Our compilation includes 2297 companions around 1903 primary stars. From high-resolution imaging, we find that ∼10% (∼30%) of the observed stars have at least one companion detected within 1″ (4″). The true fraction of systems with close (≲4″) companions is larger than the observed one due to the limited sensitivities of the imaging data. We derive correction factors for planet radii caused by the dilution of the transit depth: assuming that planets orbit the primary stars or the brightest companion stars, the average correction factors are 1.06 and 3.09, respectively. The true effect of transit dilution lies in between these two cases and varies with each system. Applying these factors to planet radii decreases the number of KOI planets with radii smaller than 2 R⊕ by ∼2%-23% and thus affects planet occurrence rates. This effect will also be important for the yield of small planets from future transit missions such as TESS. |
Keywords | binaries; general; catalogs; planets and satellites; detection; surveys; techniques; high angular resolution; techniques; photometric |
Contains Sensitive Content | Does not contain sensitive content |
ANZSRC Field of Research 2020 | 510109. Stellar astronomy and planetary systems |
Public Notes | For access to this article, please click on the URL link provided. |
Byline Affiliations | California Institute of Technology (Caltech), United States |
National Optical Astronomy Observatory, United States | |
National Aeronautics and Space Administration (NASA), United States | |
Carnegie Institution of Washington, United States | |
Southern Connecticut State University, United States | |
Lowell Observatory, United States | |
University of California, United States | |
Planetary Science Institute, United States | |
European Space Astronomy Centre, Spain | |
Pennsylvania State University, United States | |
Center for Astrophysics Harvard and Smithsonian, United States | |
European Southern Observatory (ESO), Chile | |
University of Hertfordshire, United Kingdom | |
Institution of Origin | University of Southern Queensland |
https://research.usq.edu.au/item/q434v/the-kepler-follow-up-observation-program-i-a-catalog-of-companions-to-kepler-stars-from-high-resolution-imaging
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