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Published March 2023 | Published
Journal Article Open

The TESS Grand Unified Hot Jupiter Survey. II. Twenty New Giant Planets


NASA's Transiting Exoplanet Survey Satellite (TESS) mission promises to improve our understanding of hot Jupiters by providing an all-sky, magnitude-limited sample of transiting hot Jupiters suitable for population studies. Assembling such a sample requires confirming hundreds of planet candidates with additional follow-up observations. Here we present 20 hot Jupiters that were detected using TESS data and confirmed to be planets through photometric, spectroscopic, and imaging observations coordinated by the TESS Follow-up Observing Program. These 20 planets have orbital periods shorter than 7 days and orbit relatively bright FGK stars (10.9 G P = 6.6 days), may be on a moderately eccentric orbit (e = 0.18 ± 0.06), while observations of the other targets are consistent with them being on circular orbits. We measured the projected stellar obliquity of TOI-1937A b, a hot Jupiter on a 22.4 hr orbit with the Rossiter–McLaughlin effect, finding the planet's orbit to be well aligned with the stellar spin axis (∣λ∣ = 4.°0 ± 3.°5). We also investigated the possibility that TOI-1937 is a member of the NGC 2516 open cluster but ultimately found the evidence for cluster membership to be ambiguous. These objects are part of a larger effort to build a complete sample of hot Jupiters to be used for future demographic and detailed characterization work.

Additional Information

© 2023. 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. We thank the anonymous reviewer for helpful comments that improved this manuscript. This paper includes data collected by the TESS mission that are publicly available from the Mikulski Archive for Space Telescopes (MAST). The raw TESS data can be accessed at 10.17909/t9-nmc8-f686 (SPOC 2 minutes light curves), 10.17909/t9-wpz1-8s54 (TESS-SPOC FFI light curves), 10.17909/t9-r086-e880 (QLP light curves), and 10.17909/t9-ayd0-k727 (CDIPS light curves). The Data Validation reports are available at 10.17909/t9-2tc5-a751 and 10.17909/t9-yjj5-4t42. 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 SPOC. 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 (ExoFOP 2019; NExScI 2022). This research made use of Lightkurve, a Python package for Kepler and TESS data analysis (Lightkurve Collaboration et al. 2018). We acknowledge that the work reported on in this paper was substantially performed using the Princeton Research Computing resources at Princeton University, which is a consortium of groups led by the Princeton Institute for Computational Science and Engineering (PICSciE) and Office of Information Technology's Research Computing. 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. IDs 2021B-0162, 2022A-543544, 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. 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 are honored to be permitted to conduct astronomical research on Iolkam Duâag (Kitt Peak), a mountain with particular significance to the Tohono Oâodham. 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 (http://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. 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. J.H. acknowledges funding from NASA grant 80NSSC21K0335. This work was supported by an LSSTC Catalyst Fellowship awarded by LSST Corporation to T.D. with funding from the John Templeton Foundation grant ID No. 62192. K.K.M. acknowledges support from the New York Community Trustâs Fund for Astrophysical Research. N.L.-B. thanks the NASA Massachusetts Space Grant for support. A.A.B., N.A.M., and B.S.S. acknowledge the support of the Ministry of Science and Higher Education of the Russian Federation under the grant 075-15-2020-780 (N13.1902.21.0039). A.P. acknowledges grant BK-246/RAu-11/2022. The research leading to these results has received funding from the ARC grant for Concerted Research Actions, financed by the Wallonia-Brussels Federation. TRAPPIST is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, FNRS) under the grant PDR T.0120.21. TRAPPIST-North is a project funded by the University of Liege (Belgium), in collaboration with Cadi Ayyad University of Marrakech (Morocco). M. Gillon is F.R.S.-FNRS Research Director. E.J. is F.R.S.-FNRS Senior Research Associate. This publication benefits from the support of the French Community of Belgium in the context of the FRIA Doctoral Grant awarded to M.T. Facilities: TESS - , Keck:I (HIRES) - , Magellan:Clay (PFS) - , WIYN (NEID - , NESSI) - , CTIO:1.5 m (CHIRON) - , FLWO:1.5m (TRES) - , FLWO:1.2m (KeplerCam) - , LCOGT - , TRAPPIST-North - , WASP - , CMO:2.5 m (SPP) - , Gemini:Gillett ('Alopeke) - , Gemini:South (Zorro) - , Hale (PHARO) - , SOAR (HRCam) - , Shane (ShARCS). - Software: astropy (Astropy Collaboration et al. 2013, 2018), lightkurve (Lightkurve Collaboration et al. 2018), EXOFASTv2 (Eastman et al. 2013, 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 (McKinney 2010; pandas development team 2020), matplotlib (Hunter 2007).

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August 22, 2023
August 22, 2023