Orbital Refinement and Stellar Properties for the HD 9446, HD 43691, and HD 179079 Planetary Systems
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Final Published Version
Author
Hill, Michelle L.Močnik, Teo
Kane, Stephen R.
Henry, Gregory W.
Pepper, Joshua
Hinkel, Natalie R.
Dalba, Paul A.
Fulton, Benjamin J.
Stassun, Keivan G.

Rosenthal, Lee J.
Howard, Andrew W.

Howell, Steve B.
Everett, Mark E.
Boyajian, Tabetha S.
Fischer, Debra A.

Rodriguez, Joseph E.
Beatty, Thomas G.
James, David J.
Affiliation
Univ Arizona, Dept Astron & Steward ObservIssue Date
2020-05Keywords
Radial velocityTransit photometry
Photometry
Stellar photometry
Ephemerides
Exoplanets
Exoplanet dynamics
Spectral energy distribution
Proper motions
Metadata
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IOP PUBLISHING LTDCitation
Michelle L. Hill et al 2020 AJ 159 197Journal
ASTRONOMICAL JOURNALRights
© 2020. The American Astronomical Society. All rights reserved.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
The Transit Ephemeris Refinement and Monitoring Survey is a project that aims to detect transits of intermediate-long period planets by refining orbital parameters of the known radial velocity planets using additional data from ground-based telescopes, calculating a revised transit ephemeris for the planet, then monitoring the planet host star during the predicted transit window. Here we present the results from three systems that had high probabilities of transiting planets: HD 9446 b and c, HD 43691 b, and HD 179079 b. We provide new radial velocity (RV) measurements that are then used to improve the orbital solution for the known planets. We search the RV data for indications of additional planets in orbit and find that HD 9446 shows a strong linear trend of 4.8 sigma. Using the newly refined planet orbital solutions, which include a new best-fit solution for the orbital period of HD 9446 c, and an improved transit ephemerides, we found no evidence of transiting planets in the photometry for each system. Transits of HD 9446 b can be ruled out completely and transits HD 9446 c and HD 43691 b can be ruled out for impact parameters up to b = 0.5778 and b = 0.898, respectively, due to gaps in the photometry. A transit of HD 179079 b cannot be ruled out, however, due to the relatively small size of this planet compared to the large star and thus low signal to noise. We determine properties of the three host stars through spectroscopic analysis and find through photometric analysis that HD 9446 exhibits periodic variability.ISSN
0004-6256EISSN
1538-3881Version
Final published versionae974a485f413a2113503eed53cd6c53
10.3847/1538-3881/ab7d33