CaltechAUTHORS
Published March 2022 | Version Accepted Version + Published
Journal Article Open

TESS Giants Transiting Giants. II. The Hottest Jupiters Orbiting Evolved Stars

Creators

  • 1. ROR icon American Museum of Natural History
  • 2. ROR icon University of Hawaii at Manoa
  • 3. ROR icon University of Wisconsin–Madison
  • 4. ROR icon University of Oxford
  • 5. ROR icon University of Porto
  • 6. ROR icon University of Maryland, College Park
  • 7. ROR icon University of Chicago
  • 8. ROR icon Harvard-Smithsonian Center for Astrophysics
  • 9. ROR icon Technical University of Denmark
  • 10. ROR icon University of Southern Queensland
  • 11. ROR icon Instituto de Astrofísica de Canarias
  • 12. ROR icon University of La Laguna
  • 13. ROR icon NASA Exoplanet Science Institute
  • 14. ROR icon Yale University
  • 15. ROR icon California Institute of Technology
  • 16. ROR icon University of California, Los Angeles
  • 17. ROR icon University of California, Irvine
  • 18. ROR icon University of California, Santa Cruz
  • 19. ROR icon University of California, Riverside
  • 20. ROR icon University of Kansas
  • 21. ROR icon Columbia University
  • 22. ROR icon Massachusetts Institute of Technology
  • 23. ROR icon Ames Research Center
  • 24. ROR icon Search for Extraterrestrial Intelligence
  • 25. ROR icon Goddard Space Flight Center
  • 26. ROR icon Princeton University

Abstract

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.

Additional Information

© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2021 December 1; revised 2022 January 6; accepted 2022 January 7; published 2022 February 9. 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. Software: This work relied heavily on open source software tools, and we would like to thank the developers for their contributions to the astronomy community. For data access and detrending, this research made use of lightkurve, a Python package for Kepler and TESS data analysis (Lightkurve Collaboration et al. 2018), TESSCut, a MAST tool for extracting observations from TESS FFIs (Brasseur et al. 2019), and eleanor, a pipeline for producing and detrending TESS FFI light curves (Feinstein et al. 2019). The analysis portion of this research relied on astropy (Astropy Collaboration et al. 2013,astropy2018), as well as exoplanet (Foreman-Mackey et al. 2020) and its dependencies (Agol et al. 2020; Foreman-Mackey et al. 2020; Kipping 2013; Luger et al. 2019; Salvatier et al. 2016; Theano Development Team 2016).

Attached Files

Published - Grunblatt_2022_AJ_163_120.pdf

Accepted Version - 2201.04140.pdf

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Additional details

Identifiers

Eprint ID
113348
Resolver ID
CaltechAUTHORS:20220209-266122000

Related works

Describes
https://arxiv.org/abs/2201.04140 (URL)

Funding

W. M. Keck Foundation
NASA
80NSSC19K0593
Alfred P. Sloan Foundation
NASA
80NSSC21K0652
NSF Graduate Research Fellowship
DGE-1842402
NSF Graduate Research Fellowship
DGE-1752134
NSF
ACI-1663696
NSF
AST-1716436
Heising-Simons Foundation
51 Pegasi b Fellowship
NSF Astronomy and Astrophysics Fellowship
AST-1903811
NASA/JPL/Caltech

Dates

Created
2022-02-09
Created from EPrint's datestamp field
Updated
2022-02-09
Created from EPrint's last_modified field

Caltech Custom Metadata

Caltech groups
Infrared Processing and Analysis Center (IPAC) , Astronomy Department