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Published June 2017 | Published + Submitted
Journal Article Open

No difference in orbital parameters of RV-detected giant planets between 0.1 and 5 au in single vs multi-stellar systems

Abstract

Our Keck/NIRC2 imaging survey searches for stellar companions around 144 systems with radial velocity (RV) detected giant planets to determine whether stellar binaries influence the planets' orbital parameters. This survey, the largest of its kind to date, finds eight confirmed binary systems and three confirmed triple systems. These include three new multi-stellar systems (HD 30856, HD 86081, and HD 207832) and three multi-stellar systems with newly confirmed common proper motion (HD 43691, HD 116029, and HD 164509). We combine these systems with seven RV planet-hosting multi-stellar systems from the literature in order to test for differences in the properties of planets with semimajor axes ranging between 0.1 and 5 au in single versus multi-stellar systems. We find no evidence that the presence or absence of stellar companions alters the distribution of planet properties in these systems. Although the observed stellar companions might influence the orbits of more distant planetary companions in these systems, our RV observations currently provide only weak constraints on the masses and orbital properties of planets beyond 5 au. In order to aid future efforts to characterize long-period RV companions in these systems, we publish our contrast curves for all 144 targets. Using four years of astrometry for six hierarchical triple star systems hosting giant planets, we fit the orbits of the stellar companions in order to characterize the orbital architecture in these systems. We find that the orbital plane of the secondary and tertiary companions are inconsistent with an edge-on orbit in four out of six cases.

Additional Information

© 2017 The American Astronomical Society. Received 2017 February 11; revised 2017 April 5; accepted 2017 April 6; published 2017 May 4. We would like to thank John A Johnson, Christopher Spalding, and Benjamin Montet for helpful discussions. We also appreciate the useful suggestions from the anonymous referee and the statistics editor. This work was supported by NASA grant NNX14AD24G. H.N. is grateful for funding support from the Natural Sciences and Engineering Research Council of Canada and the NASA Earth and Space Science Fellowship Program grant NNX15AR12H. H.A.K. acknowledges support from the Sloan Foundation. E.L.N. and S.C.B. are supported by NASA grant NNX14AJ80G. This work was based on observations at the W. M. Keck Observatory granted by the California Institute of Technology. We thank the observers who contributed to the measurements reported here and acknowledge the efforts of the Keck Observatory staff. We extend special thanks to those of Hawaiian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. Facility: Keck:II - KECK II Telescope. Software: Astropy (Astropy Collaboration et al. 2013), OFTI (Blunt et al. 2017), emcee (Foreman-Mackey et al. 2013), corner.py (Foreman-Mackey 2016).

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Published - Ngo_2017_AJ_153_242.pdf

Submitted - 1704.02326.pdf

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August 19, 2023
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