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

The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets

Creators

  • 1. ROR icon Princeton University
  • 2. ROR icon Michigan State University
  • 3. ROR icon University of Southern Queensland
  • 4. ROR icon Harvard-Smithsonian Center for Astrophysics
  • 5. ROR icon University of California, Los Angeles
  • 6. ROR icon University of Liège
  • 7. ROR icon Massachusetts Institute of Technology
  • 8. ROR icon Instituto de Astrofísica de Canarias
  • 9. ROR icon NASA Exoplanet Science Institute
  • 10. ROR icon Millennium Institute of Astrophysics
  • 11. ROR icon Carnegie Institution for Science
  • 12. ROR icon George Mason University
  • 13. ROR icon American Association of Variable Star Observers
  • 14. ROR icon California Institute of Technology
  • 15. ROR icon University of California, Berkeley
  • 16. ROR icon University of Valencia
  • 17. ROR icon Tsinghua University
  • 18. ROR icon Max Planck Institute for Astronomy
  • 19. ROR icon Ames Research Center
  • 20. ROR icon Swarthmore College
  • 21. ROR icon University of California, Riverside
  • 22. ROR icon University of Louisville
  • 23. ROR icon Silesian University of Technology
  • 24. ROR icon University of North Carolina at Chapel Hill
  • 25. ROR icon Wellesley College
  • 26. ROR icon University of La Laguna
  • 27. ROR icon Royal Astronomical Society
  • 28. ROR icon Lomonosov Moscow State University
  • 29. ROR icon University of Maryland, College Park
  • 30. ROR icon South African Radio Astronomy Observatory
  • 31. ROR icon UNSW Sydney
  • 32. ROR icon Shanghai Astronomical Observatory
  • 33. ROR icon Stephen F. Austin State University

Abstract

Hot Jupiters—short-period giant planets—were the first extrasolar planets to be discovered, but many questions about their origin remain. NASA's Transiting Exoplanet Survey Satellite (TESS), an all-sky search for transiting planets, presents an opportunity to address these questions by constructing a uniform sample of hot Jupiters for demographic study through new detections and unifying the work of previous ground-based transit surveys. As the first results of an effort to build this large sample of planets, we report here the discovery of 10 new hot Jupiters (TOI-2193A b, TOI-2207b, TOI-2236b, TOI-2421b, TOI-2567b, TOI-2570b, TOI-3331b, TOI-3540A b, TOI-3693b, TOI-4137b). All of the planets were identified as planet candidates based on periodic flux dips observed by TESS, and were subsequently confirmed using ground-based time-series photometry, high-angular-resolution imaging, and high-resolution spectroscopy coordinated with the TESS Follow-up Observing Program. The 10 newly discovered planets orbit relatively bright F and G stars (G < 12.5, T_(eff) between 4800 and 6200 K). The planets' orbital periods range from 2 to 10 days, and their masses range from 0.2 to 2.2 Jupiter masses. TOI-2421b is notable for being a Saturn-mass planet and TOI-2567b for being a "sub-Saturn," with masses of 0.322 ± 0.073 and 0.195 ± 0.030 Jupiter masses, respectively. We also measured a detectably eccentric orbit (e = 0.17 ± 0.05) for TOI-2207b, a planet on an 8 day orbit, while placing an upper limit of e < 0.052 for TOI-3693b, which has a 9 day orbital period. The 10 planets described here represent an important step toward using TESS to create a large and statistically useful sample of hot Jupiters.

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 2022 March 23; revised 2022 May 18; accepted 2022 May 21; published 2022 July 27. We thank the anonymous reviewer whose comments helped improve the manuscript. S.W.Y. thanks Gummi Stefansson for helpful conversations regarding the NEID observations. This paper includes data collected by the TESS mission that are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by NASA's Science Mission Directorate. 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. We also acknowledge the use of data from 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. This research made use of Lightkurve, a Python package for Kepler and TESS data analysis (Lightkurve Collaboration et al. 2018). Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Keck telescope time was granted by NOIRLab (Prop. ID 2021B-0162, PI: Yee) through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. 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. This paper contains data taken with the NEID instrument, which was funded by the NASA-NSF Exoplanet Observational Research (NN-EXPLORE) partnership and built by Pennsylvania State University. NEID is installed on the WIYN telescope, which is operated by the National Optical Astronomy Observatory, and the NEID archive is operated by the NASA Exoplanet Science Institute at the California Institute of Technology. NN-EXPLORE is managed by the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration. The data presented herein were obtained at the WIYN Observatory from telescope time allocated to NN-EXPLORE through the scientific partnership of the National Aeronautics and Space Administration, the National Science Foundation, and NOIRLab. This work was supported by a NASA WIYN PI Data Award, administered by the NASA Exoplanet Science Institute. The authors thank Sarah Logsdon and Heidi Schweiker for help with the NEID observations. The authors are honored to be permitted to conduct astronomical research on Iolkam Du'ag (Kitt Peak), a mountain with particular significance to the Tohono O'odham. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. This research has used data from the CTIO/SMARTS 1.5 m telescope, which is operated as part of the SMARTS Consortium by RECONS (www.recons.org) members Todd Henry, Hodari James, Wei-Chun Jao, and Leonardo Paredes. At the telescope, observations were carried out by Roberto Aviles and Rodrigo Hinojosa. The CHIRON data were obtained from telescope time allocated under the NN-EXPLORE program with support from the National Aeronautics and Space Administration. Some of the data presented herein were obtained at the Minerva–Australis facility from telescope time allocated under the NN-EXPLORE program with support from the National Aeronautics and Space Administration. Minerva–Australis is supported by Australian Research Council LIEF grant LE160100001, Discovery grants DP180100972 and DP220100365, Mount Cuba Astronomical Foundation, and institutional partners University of Southern Queensland, UNSW Sydney, MIT, Nanjing University, George Mason University, University of Louisville, University of California Riverside, University of Florida, and The University of Texas at Austin. We respectfully acknowledge the traditional custodians of all lands throughout Australia, and recognize their continued cultural and spiritual connection to the land, waterways, cosmos, and community. We pay our deepest respects to all Elders, ancestors and descendants of the Giabal, Jarowair, and Kambuwal nations, upon whose lands the Minerva–Australis facility at Mt. Kent is situated. This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. This paper makes use of data from the MEarth Project, which is a collaboration between Harvard University and the Smithsonian Astrophysical Observatory. The MEarth Project acknowledges funding from the David and Lucile Packard Fellowship for Science and Engineering, the National Science Foundation under grants AST-0807690, AST-1109468, AST-1616624 and AST-1004488 (Alan T. Waterman Award), the National Aeronautics and Space Administration under grant No. 80NSSC18K0476 issued through the XRP Program, and the John Templeton Foundation. Adam Popowicz and Slawomir Lasota were responsible for data processing and automation of observations at SUTO observatories and were financed by grant BK-246/RAu-11/2022. A.J. acknowledges support from ANID—Millennium Science Initiative—ICN12_009 and FONDECYT project 1210718. J.H. acknowledges support from NASA grants 80NSSC19K0386, 80NSSC19K1728, and 80NSSC21K0335. Facilities: TESS, MAST, Gaia, Keck: I (HIRES), WIYN (NEID), Magellan: Clay (PFS), CTIO: 1.5 m (CHIRON), Max Planck: 2.2 m (FEROS), FLWO: 1.5 m (TRES), LCOGT, Gemini. Software: astropy (Astropy Collaboration et al. 2013, 2018), lightkurve (Lightkurve Collaboration et al. 2018), EXOFASTv2 (Eastman et al. 2019), SpecMatch-Emp (Yee et al. 2017), SpecMatch-Synth (Petigura 2015), AstroImageJ (Collins et al. 2017), TAPIR (Jensen 2013), numpy (Harris et al. 2020), scipy (Virtanen et al. 2020), pandas (pandas development team 2020; Wes McKinney 2010), matplotlib (Hunter 2007).

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Published - Yee_2022_AJ_164_70.pdf

Accepted Version - 2205.09728.pdf

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Additional details

Identifiers

Eprint ID
115941
Resolver ID
CaltechAUTHORS:20220728-730049000

Related works

Describes
https://arxiv.org/abs/2205.09728 (URL)

Funding

NASA/JPL/Caltech
W. M. Keck Foundation
Australian Research Council
LE160100001
Australian Research Council
DP180100972
Australian Research Council
DP220100365
Mt. Cuba Astronomical Foundation
University of Southern Queensland
University of New South Wales, Sydney
Massachusetts Institute of Technology (MIT)
Nanjing University
George Mason University
University of Louisville
University of California, Riverside
University of Florida
University of Texas at Austin
David and Lucile Packard Foundation
NSF
AST-0807690
NSF
AST-1109468
NSF
AST-1616624
NSF
AST-1004488
NASA
80NSSC18K0476
John Templeton Foundation
Ministry of Science and Higher Education (Poland)
BK-246/RAu-11/2022
Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)
ICN12_009
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)
1210718
NASA
80NSSC19K0386
NASA
80NSSC19K1728
NASA
80NSSC21K0335

Dates

Created
2022-07-29
Created from EPrint's datestamp field
Updated
2022-07-29
Created from EPrint's last_modified field

Caltech Custom Metadata

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