TY - JOUR
T1 - TESS Giants Transiting Giants. II. the Hottest Jupiters Orbiting Evolved Stars
AU - Grunblatt, Samuel K.
AU - Saunders, Nicholas
AU - Sun, Meng
AU - Chontos, Ashley
AU - Soares-Furtado, Melinda
AU - Eisner, Nora
AU - Pereira, Filipe
AU - Komacek, Thaddeus
AU - Huber, Daniel
AU - Collins, Karen
AU - Wang, Gavin
AU - Stockdale, Chris
AU - Quinn, Samuel N.
AU - Tronsgaard, Rene
AU - Zhou, George
AU - Nowak, Grzegorz
AU - Deeg, Hans J.
AU - Ciardi, David R.
AU - Boyle, Andrew
AU - Rice, Malena
AU - Dai, Fei
AU - Blunt, Sarah
AU - Van Zandt, Judah
AU - Beard, Corey
AU - Akana Murphy, Joseph M.
AU - Dalba, Paul A.
AU - Lubin, Jack
AU - Polanski, Alex
AU - Brinkman, Casey Lynn
AU - Howard, Andrew W.
AU - Buchhave, Lars A.
AU - Angus, Ruth
AU - Ricker, George R.
AU - Jenkins, Jon M.
AU - Wohler, Bill
AU - Goeke, Robert F.
AU - Levine, Alan M.
AU - Colon, Knicole D.
AU - Huang, Chelsea X.
AU - Kunimoto, Michelle
AU - Shporer, Avi
AU - Latham, David W.
AU - Seager, Sara
AU - Vanderspek, Roland K.
AU - Winn, Joshua N.
N1 - Funding Information:
We thank Howard Isaacson and Daniel Foreman-Mackey for helpful discussions. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency’s scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. S.G., N.S., and D.H. acknowledge support by the National Aeronautics and Space Administration under grant 80NSSC19K0593 issued through the TESS Guest Investigator Program. D.H. acknowledges support from the Alfred P. Sloan Foundation and the National Aeronautics and Space Administration (80NSSC21K0652), and the National Science Foundation (80NSSC21K0652). N.S., A.C., and M.R. acknowledge support from the National Science Foundation through the Graduate Research Fellowship Program under grants 1842402 and DGE-1752134. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. M.S. acknowledges funding support from NSF ACI-1663696 and AST-1716436. T.D.K. acknowledges support from the 51 Pegasi b fellowship in Planetary Astronomy sponsored by the Heising-Simons Foundation. P.D. is supported by a National Science Foundation (NSF) Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1903811. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Funding for the TESS mission is provided by NASA’s Science Mission Directorate.
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/3/1
Y1 - 2022/3/1
N2 - Giant planets on short-period orbits are predicted to be inflated and eventually engulfed by their host stars. However, the detailed timescales and stages of these processes are not well known. Here, we present the discovery of three hot Jupiters (P < 10 days) orbiting evolved, intermediate-mass stars (M ⋆ ≈ 1.5 M ⊙, 2 R ⊙ < R ⋆ < 5 R ⊙). By combining TESS photometry with ground-based photometry and radial velocity measurements, we report masses and radii for these three planets of between 0.4 and 1.8 M J and 0.8 and 1.8 R J. TOI-2337b has the shortest period (P = 2.99432 ± 0.00008 days) of any planet discovered around a red giant star to date. Both TOI-4329b and TOI-2669b appear to be inflated, but TOI-2337b does not show any sign of inflation. The large radii and relatively low masses of TOI-4329b and TOI-2669b place them among the lowest density hot Jupiters currently known, while TOI-2337b is conversely one of the highest. All three planets have orbital eccentricities of below 0.2. The large spread in radii for these systems implies that planet inflation has a complex dependence on planet mass, radius, incident flux, and orbital properties. We predict that TOI-2337b has the shortest orbital decay timescale of any planet currently known, but do not detect any orbital decay in this system. Transmission spectroscopy of TOI-4329b would provide a favorable opportunity for the detection of water, carbon dioxide, and carbon monoxide features in the atmosphere of a planet orbiting an evolved star, and could yield new information about planet formation and atmospheric evolution.
AB - Giant planets on short-period orbits are predicted to be inflated and eventually engulfed by their host stars. However, the detailed timescales and stages of these processes are not well known. Here, we present the discovery of three hot Jupiters (P < 10 days) orbiting evolved, intermediate-mass stars (M ⋆ ≈ 1.5 M ⊙, 2 R ⊙ < R ⋆ < 5 R ⊙). By combining TESS photometry with ground-based photometry and radial velocity measurements, we report masses and radii for these three planets of between 0.4 and 1.8 M J and 0.8 and 1.8 R J. TOI-2337b has the shortest period (P = 2.99432 ± 0.00008 days) of any planet discovered around a red giant star to date. Both TOI-4329b and TOI-2669b appear to be inflated, but TOI-2337b does not show any sign of inflation. The large radii and relatively low masses of TOI-4329b and TOI-2669b place them among the lowest density hot Jupiters currently known, while TOI-2337b is conversely one of the highest. All three planets have orbital eccentricities of below 0.2. The large spread in radii for these systems implies that planet inflation has a complex dependence on planet mass, radius, incident flux, and orbital properties. We predict that TOI-2337b has the shortest orbital decay timescale of any planet currently known, but do not detect any orbital decay in this system. Transmission spectroscopy of TOI-4329b would provide a favorable opportunity for the detection of water, carbon dioxide, and carbon monoxide features in the atmosphere of a planet orbiting an evolved star, and could yield new information about planet formation and atmospheric evolution.
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U2 - 10.3847/1538-3881/ac4972
DO - 10.3847/1538-3881/ac4972
M3 - Article
AN - SCOPUS:85125856761
SN - 0004-6256
VL - 163
JO - Astronomical Journal
JF - Astronomical Journal
IS - 3
M1 - 120
ER -