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

Ngo, Henry and Knutson, Heather A. and Bryan, Marta L. and Blunt, Sarah and Nielsen, Eric L. and Batygin, Konstantin and Bowler, Brendan P. and Crepp, Justin R. and Hinkley, Sasha and Howard, Andrew W. and Mawet, Dimitri (2017) No difference in orbital parameters of RV-detected giant planets between 0.1 and 5 au in single vs multi-stellar systems. Astronomical Journal, 153 (6). Art. No. 242. ISSN 1538-3881. https://resolver.caltech.edu/CaltechAUTHORS:20170518-103324368

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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.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-3881/aa6cacDOIArticle
http://iopscience.iop.org/article/10.3847/1538-3881/aa6cac/metaPublisherArticle
http://arxiv.org/abs/1704.02326arXivDiscussion Paper
ORCID:
AuthorORCID
Ngo, Henry0000-0001-5172-4859
Knutson, Heather A.0000-0002-0822-3095
Bryan, Marta L.0000-0002-6076-5967
Blunt, Sarah0000-0002-3199-2888
Nielsen, Eric L.0000-0001-6975-9056
Batygin, Konstantin0000-0002-7094-7908
Bowler, Brendan P.0000-0003-2649-2288
Crepp, Justin R.0000-0003-0800-0593
Hinkley, Sasha0000-0001-8074-2562
Howard, Andrew W.0000-0001-8638-0320
Mawet, Dimitri0000-0002-8895-4735
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).
Group:Astronomy Department
Funders:
Funding AgencyGrant Number
NASANNX14AD24G
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
NASA Earth and Space Science FellowshipNNX15AR12H
Alfred P. Sloan FoundationUNSPECIFIED
NASANNX14AJ80G
Subject Keywords:binaries: close – binaries: eclipsing – methods: observational – planetary systems – planets and satellites: dynamical evolution and stability – techniques: high angular resolution
Issue or Number:6
Record Number:CaltechAUTHORS:20170518-103324368
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170518-103324368
Official Citation:Henry Ngo et al 2017 AJ 153 242
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:77568
Collection:CaltechAUTHORS
Deposited By: Joy Painter
Deposited On:18 May 2017 17:41
Last Modified:09 Mar 2020 13:18

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