The Kepler follow-up observation program. I. A catalog of companions to Kepler stars from high-resolution imaging

Furlan, E. and Ciardi, D. R. and Everett, M. E. and Saylors, M. and Teske, J. K. and Horch, E. P. and Howell, S. B. and van Belle, G. T. and Hirsch, L. A. and Gautier, T. N. and Adams, E. R. and Barrado, D. and Cartier, K. M. S. and Dressing, C. D. and Dupree, A. K. and Gilliland, R. L. and Lillo-Box, J. and Lucas, P. W. and Wang, J. (2017) The Kepler follow-up observation program. I. A catalog of companions to Kepler stars from high-resolution imaging. The Astronomical Journal, 153 (2). ISSN 0004-6256

[img]
Preview
Text (Published Version)
Ciardi_2017_PV.pdf

Download (9Mb) | Preview

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.


Statistics for USQ ePrint 32187
Statistics for this ePrint Item
Item Type: Article (Commonwealth Reporting Category C)
Refereed: Yes
Item Status: Live Archive
Additional Information: Access to published version in accordance with the copyright policy of the publisher.
Faculty / Department / School: No Faculty
Date Deposited: 30 Oct 2017 00:20
Last Modified: 08 Nov 2017 03:38
Uncontrolled Keywords: binaries; general; catalogs; planets and satellites; detection; surveys; techniques; high angular resolution; techniques; photometric
Fields of Research : 02 Physical Sciences > 0201 Astronomical and Space Sciences > 020110 Stellar Astronomy and Planetary Systems
Identification Number or DOI: 10.3847/1538-3881/153/2/71
URI: http://eprints.usq.edu.au/id/eprint/32187

Actions (login required)

View Item Archive Repository Staff Only