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

Yee, Samuel W. and Winn, Joshua N. and Hartman, Joel D. and Rodriguez, Joseph E. and Zhou, George and Quinn, Samuel N. and Latham, David W. and Bieryla, Allyson and Collins, Karen A. and Addison, Brett C. and Angelo, Isabel and Barkaoui, Khalid and Benni, Paul and Boyle, Andrew W. and Brahm, Rafael and Butler, R. Paul and Ciardi, David R. and Collins, Kevin I. and Conti, Dennis M. and Crane, Jeffrey D. and Dai, Fei and Dressing, Courtney D. and Eastman, Jason D. and Essack, Zahra and Forés-Toribio, Raquel and Furlan, Elise and Gan, Tianjun and Giacalone, Steven and Gill, Holden and Girardin, Eric and Henning, Thomas and Henze, Christopher E. and Hobson, Melissa J. and Horner, Jonathan and Howard, Andrew W. and Howell, Steve B. and Huang, Chelsea X. and Isaacson, Howard and Jenkins, Jon M. and Jensen, Eric L. N. and Jordán, Andrés and Kane, Stephen R. and Kielkopf, John F. and Lasota, Slawomir and Levine, Alan M. and Lubin, Jack and Mann, Andrew W. and Massey, Bob and McLeod, Kim K. and Mengel, Matthew W. and Muñoz, Jose A. and Murgas, Felipe and Palle, Enric and Plavchan, Peter and Popowicz, Adam and Radford, Don J. and Ricker, George R. and Rowden, Pamela and Safonov, Boris S. and Savel, Arjun B. and Schwarz, Richard P. and Seager, S. and Sefako, Ramotholo and Shporer, Avi and Srdoc, Gregor and Strakhov, Ivan S. and Teske, Johanna K. and Tinney, C. G. and Tyler, Dakotah and Wittenmyer, Robert A. and Zhang, Hui and Ziegler, Carl (2022) The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets. Astronomical Journal, 164 (2). Art. No. 70. ISSN 0004-6256. doi:10.3847/1538-3881/ac73ff.

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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.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Yee, Samuel W.0000-0001-7961-3907
Winn, Joshua N.0000-0002-4265-047X
Hartman, Joel D.0000-0001-8732-6166
Rodriguez, Joseph E.0000-0001-8812-0565
Zhou, George0000-0002-4891-3517
Quinn, Samuel N.0000-0002-8964-8377
Latham, David W.0000-0001-9911-7388
Bieryla, Allyson0000-0001-6637-5401
Collins, Karen A.0000-0001-6588-9574
Addison, Brett C.0000-0003-3216-0626
Angelo, Isabel0000-0002-9751-2664
Barkaoui, Khalid0000-0003-1464-9276
Benni, Paul0000-0001-6981-8722
Boyle, Andrew W.0000-0001-6037-2971
Brahm, Rafael0000-0002-9158-7315
Butler, R. Paul0000-0003-1305-3761
Ciardi, David R.0000-0002-5741-3047
Collins, Kevin I.0000-0003-2781-3207
Conti, Dennis M.0000-0003-2239-0567
Crane, Jeffrey D.0000-0002-5226-787X
Dai, Fei0000-0002-8958-0683
Dressing, Courtney D.0000-0001-8189-0233
Eastman, Jason D.0000-0003-3773-5142
Essack, Zahra0000-0002-2482-0180
Forés-Toribio, Raquel0000-0002-6482-2180
Furlan, Elise0000-0001-9800-6248
Gan, Tianjun0000-0002-4503-9705
Giacalone, Steven0000-0002-8965-3969
Gill, Holden0000-0001-6171-7951
Girardin, Eric0000-0002-5443-3640
Henning, Thomas0000-0002-1493-300X
Henze, Christopher E.0000-0003-3216-0626
Hobson, Melissa J.0000-0002-5945-7975
Horner, Jonathan0000-0002-1160-7970
Howard, Andrew W.0000-0001-8638-0320
Howell, Steve B.0000-0002-2532-2853
Huang, Chelsea X.0000-0003-0918-7484
Isaacson, Howard0000-0002-0531-1073
Jenkins, Jon M.0000-0002-4715-9460
Jensen, Eric L. N.0000-0002-4625-7333
Jordán, Andrés0000-0002-5389-3944
Kane, Stephen R.0000-0002-7084-0529
Kielkopf, John F.0000-0003-0497-2651
Lasota, Slawomir0000-0002-7830-6822
Levine, Alan M.0000-0001-8172-0453
Lubin, Jack0000-0001-8342-7736
Mann, Andrew W.0000-0003-3654-1602
Massey, Bob0000-0001-8879-7138
McLeod, Kim K.0000-0001-9504-1486
Mengel, Matthew W.0000-0002-7830-6822
Muñoz, Jose A.0000-0001-9833-2959
Murgas, Felipe0000-0001-9087-1245
Palle, Enric0000-0003-0987-1593
Plavchan, Peter0000-0002-8864-1667
Popowicz, Adam0000-0003-3184-5228
Radford, Don J.0000-0002-3940-2360
Ricker, George R.0000-0003-2058-6662
Rowden, Pamela0000-0002-4829-7101
Safonov, Boris S.0000-0003-1713-3208
Savel, Arjun B.0000-0002-2454-768X
Schwarz, Richard P.0000-0001-8227-1020
Seager, S.0000-0002-3940-2360
Sefako, Ramotholo0000-0003-3904-6754
Shporer, Avi0000-0002-1836-3120
Tinney, C. G.0000-0002-7595-0970
Tyler, Dakotah0000-0003-0298-4667
Wittenmyer, Robert A.0000-0001-9957-9304
Zhang, Hui0000-0003-3491-6394
Ziegler, Carl0000-0002-0619-7639
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 ( 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).
Group:Astronomy Department, Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
W. M. Keck FoundationUNSPECIFIED
Australian Research CouncilLE160100001
Australian Research CouncilDP180100972
Australian Research CouncilDP220100365
Mt. Cuba Astronomical FoundationUNSPECIFIED
University of Southern QueenslandUNSPECIFIED
University of New South Wales, SydneyUNSPECIFIED
Massachusetts Institute of Technology (MIT)UNSPECIFIED
Nanjing UniversityUNSPECIFIED
George Mason UniversityUNSPECIFIED
University of LouisvilleUNSPECIFIED
University of California, RiversideUNSPECIFIED
University of FloridaUNSPECIFIED
University of Texas at AustinUNSPECIFIED
David and Lucile Packard FoundationUNSPECIFIED
John Templeton FoundationUNSPECIFIED
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
Subject Keywords:Exoplanets; Hot Jupiters; Transits; Exoplanet astronomy; Exoplanet detection methods
Issue or Number:2
Classification Code:Unified Astronomy Thesaurus concepts: Exoplanets (498); Hot Jupiters (753); Transits (1711); Exoplanet astronomy (486); Exoplanet detection methods (489)
Record Number:CaltechAUTHORS:20220728-730049000
Persistent URL:
Official Citation:Samuel W. Yee et al 2022 AJ 164 70
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:115941
Deposited By: George Porter
Deposited On:29 Jul 2022 21:01
Last Modified:29 Jul 2022 21:01

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