TY - JOUR
T1 - The HD 217107 planetary system
T2 - Twenty years of radial velocity measurements
AU - Giovinazzi, Mark R.
AU - Blake, Cullen H.
AU - Eastman, Jason D.
AU - Wright, Jason
AU - McCrady, Nate
AU - Wittenmyer, Rob
AU - Johnson, John A.
AU - Plavchan, Peter
AU - Sliski, David H.
AU - Wilson, Maurice L.
AU - Johnson, Samson A.
AU - Horner, Jonathan
AU - Kane, Stephen R.
AU - Houghton, Audrey
AU - García-Mejía, Juliana
AU - Glaser, Joseph P.
N1 - Funding Information:
Correspondence National Science Foundation Australian Research Council Nancy Grace Roman programs ExEP NASA) EPSCOR David & Lucile Packard Foundation Mt. Cuba Astronomical Foundation
Funding Information:
George Mason University, NASA Exoplanet Exploration Program, Pennsylvania Space Grant Consortium, Eberly College of Science, Pennsylvania State University, NASA MT‐13‐EPSCoR‐0011, Graduate Research Fellowships, , Grant/Award Numbers: AAG 1716202; 1608203; 1516242; , Grant/Award Numbers: LE140100050; Nancy Grace Roman Fellowship, , , National Aeronautics and Space Administration (, Grant/Award Numbers: NNX13AM97A; , Funding information National Science Foundation Australian Research Council Nancy Grace Roman programs ExEP NASA) EPSCOR David & Lucile Packard Foundation Mt. Cuba Astronomical Foundation
Funding Information:
MINERVA is a collaboration among the Harvard‐Smithsonian Center for Astrophysics, The Pennsylvania State University, the University of Montana, the University of Southern Queensland, and the University of Pennsylvania. MINERVA is made possible by generous contributions from its collaborating institutions and , , the National Aeronautics and Space Administration (, , (EPSCOR grant NNX13AM97A, Blake is partially supported by a Nancy Grace Roman Fellowship); (ARC LIEF grant LE140100050); and the (NSF grants 1516242 and 1608203 and Graduate Research Fellowships awarded to Giovinazzi and Wilson). Funding for MINERVA data analysis software development is provided through a subaward under a NASA award, NASA MT‐13‐EPSCoR‐0011. This work was partially supported by funding from the Center for Exoplanets and Habitable Worlds, which is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. Plavchan is supported in part by the NASA Exoplanet Exploration Program, NSF grant AAG 1716202, and George Mason University startup funds. We are grateful to Dr. Gillian Nave and R. Paul Butler for providing Fourier Transform Spectrometer (FTS) measurements of our iodine gas cell. We thank Dr. Matt Holman for answering questions about orbital precession and Dr. Ben Pope for assistance with light curves. Any opinions, findings, and conclusions or recommendations expressed are those of the authors and do not necessarily reflect the views of the National Science Foundation. We thank the referee, Dr. Artie Hatzes, for helpful and encouraging feedback on this manuscript. Mt. Cuba Astronomical Foundation The David & Lucile Packard Foundation NASA) EPSCOR ExEP and Nancy Grace Roman programs The Australian Research Council National Science Foundation K2
Funding Information:
information George Mason University, NASA Exoplanet Exploration Program, Pennsylvania Space Grant Consortium, Eberly College of Science, Pennsylvania State University, NASA MT-13-EPSCoR-0011, Graduate Research Fellowships, National Science Foundation, Grant/Award Numbers: AAG 1716202; 1608203; 1516242; Australian Research Council, Grant/Award Numbers: LE140100050; Nancy Grace Roman Fellowship, Nancy Grace Roman programs, ExEP, National Aeronautics and Space Administration (NASA) EPSCOR, Grant/Award Numbers: NNX13AM97A; David & Lucile Packard Foundation, Mt. Cuba Astronomical FoundationMINERVA is a collaboration among the Harvard-Smithsonian Center for Astrophysics, The Pennsylvania State University, the University of Montana, the University of Southern Queensland, and the University of Pennsylvania. MINERVA is made possible by generous contributions from its collaborating institutions and Mt. Cuba Astronomical Foundation, The David & Lucile Packard Foundation, the National Aeronautics and Space Administration (NASA) EPSCOR, ExEP, and Nancy Grace Roman programs (EPSCOR grant NNX13AM97A, Blake is partially supported by a Nancy Grace Roman Fellowship); The Australian Research Council (ARC LIEF grant LE140100050); and the National Science Foundation (NSF grants 1516242 and 1608203 and Graduate Research Fellowships awarded to Giovinazzi and Wilson). Funding for MINERVA data analysis software development is provided through a subaward under a NASA award, NASA MT-13-EPSCoR-0011. This work was partially supported by funding from the Center for Exoplanets and Habitable Worlds, which is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. Plavchan is supported in part by the NASA Exoplanet Exploration Program, NSF grant AAG 1716202, and George Mason University startup funds. We are grateful to Dr. Gillian Nave and R. Paul Butler for providing Fourier Transform Spectrometer (FTS) measurements of our iodine gas cell. We thank Dr. Matt Holman for answering questions about orbital precession and Dr. Ben Pope for assistance with K2 light curves. Any opinions, findings, and conclusions or recommendations expressed are those of the authors and do not necessarily reflect the views of the National Science Foundation. We thank the referee, Dr. Artie Hatzes, for helpful and encouraging feedback on this manuscript.
Publisher Copyright:
© 2020 Wiley-VCH GmbH
PY - 2020/11
Y1 - 2020/11
N2 - The hot Jupiter HD 217107 b was one of the first exoplanets detected using the radial velocity (RV) method, originally reported in the literature in 1999. Today, precise RV measurements of this system span more than 20 years, and there is clear evidence of a longer-period companion, HD 217107 c. Interestingly, both the short-period planet (Pb ∼ 7.13 d) and long-period planet (Pc ∼ 5059 d) have significantly eccentric orbits (eb ∼ 0.13 and ec ∼ 0.40). We present 42 additional RV measurements of this system obtained with the MINERVA telescope array and carry out a joint analysis with previously published RV measurements from four different facilities. We confirm and refine the previously reported orbit of the long-period companion. HD 217107 b is one of a relatively small number of hot Jupiters with an eccentric orbit, opening up the possibility of detecting the precession of the planetary orbit due to general relativistic effects and perturbations from other planets in the system. In this case, the argument of periastron, ω, is predicted to change at the level of ∼0.8∘ century−1. Despite the long time baseline of our observations and the high quality of the RV measurements, we are only able to constrain the precession to be (Formula presented.) century−1. We discuss the limitations of detecting the subtle effects of precession in exoplanet orbits using RV data.
AB - The hot Jupiter HD 217107 b was one of the first exoplanets detected using the radial velocity (RV) method, originally reported in the literature in 1999. Today, precise RV measurements of this system span more than 20 years, and there is clear evidence of a longer-period companion, HD 217107 c. Interestingly, both the short-period planet (Pb ∼ 7.13 d) and long-period planet (Pc ∼ 5059 d) have significantly eccentric orbits (eb ∼ 0.13 and ec ∼ 0.40). We present 42 additional RV measurements of this system obtained with the MINERVA telescope array and carry out a joint analysis with previously published RV measurements from four different facilities. We confirm and refine the previously reported orbit of the long-period companion. HD 217107 b is one of a relatively small number of hot Jupiters with an eccentric orbit, opening up the possibility of detecting the precession of the planetary orbit due to general relativistic effects and perturbations from other planets in the system. In this case, the argument of periastron, ω, is predicted to change at the level of ∼0.8∘ century−1. Despite the long time baseline of our observations and the high quality of the RV measurements, we are only able to constrain the precession to be (Formula presented.) century−1. We discuss the limitations of detecting the subtle effects of precession in exoplanet orbits using RV data.
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U2 - 10.1002/asna.202013830
DO - 10.1002/asna.202013830
M3 - Article
AN - SCOPUS:85092332817
VL - 341
SP - 870
EP - 878
JO - Astronomische Nachrichten
JF - Astronomische Nachrichten
SN - 0004-6337
IS - 9
ER -