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An Eccentric Massive Jupiter Orbiting a Subgiant on a 9.5-day Period Discovered in the Transiting Exoplanet Survey Satellite Full Frame Images The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Rodriguez, Joseph A. et al. "An Eccentric Massive Jupiter Orbiting a Subgiant on a 9.5-day Period Discovered in the Transiting Exoplanet Survey Satellite Full Frame Images." Astronomical Journal 157, 5 (April 2019): 191 © 2019 American Astronomical Society As Published http://dx.doi.org/10.3847/1538-3881/ab11d9 Publisher American Astronomical Society Version Final published version Citable link https://hdl.handle.net/1721.1/125237 Terms of Use Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. The Astronomical Journal, 157:191 (13pp), 2019 May https://doi.org/10.3847/1538-3881/ab11d9 © 2019. The American Astronomical Society. All rights reserved. An Eccentric Massive Jupiter Orbiting a Subgiant on a 9.5-day Period Discovered in the Transiting Exoplanet Survey Satellite Full Frame Images Joseph E. Rodriguez1 , Samuel N. Quinn1 , Chelsea X. Huang2,29 , Andrew Vanderburg3,30 , Kaloyan Penev4 , Rafael Brahm5,6,7 , Andrés Jordán6,7 , Mma Ikwut-Ukwa1, Shelly Tsirulik1, David W. Latham1 , Keivan G. Stassun8,9 , Avi Shporer2 , Carl Ziegler10 , Elisabeth Matthews2, Jason D. Eastman1 , B. Scott Gaudi11 , Karen A. Collins1 , Natalia Guerrero2, Howard M. Relles1, Thomas Barclay12,13 , Natalie M. Batalha14, Perry Berlind1, Allyson Bieryla1 , L. G. Bouma15 , Patricia T. Boyd12 , Jennifer Burt2,29 , Michael L. Calkins1 , Jessie Christiansen16 , David R. Ciardi16, Knicole D. Colón12 , Dennis M. Conti17, Ian J. M. Crossfield2, Tansu Daylan2,31 , Jason Dittmann2,32, Diana Dragomir2,33 , Scott Dynes2, Néstor Espinoza18,34,35 , Gilbert A. Esquerdo1, Zahra Essack19, Aylin Garcia Soto19, Ana Glidden2,19 , Maximilian N. Günther2,29 , Thomas Henning18, Jon M. Jenkins20 , John F. Kielkopf21, Akshata Krishnamurthy22, Nicholas M. Law23 , Alan M. Levine2, Pablo Lewin24, Andrew W. Mann23 , Edward H. Morgan2 , Robert L. Morris20,25, Ryan J. Oelkers8 , Martin Paegert1 , Joshua Pepper26 , Elisa V. Quintana12, George R. Ricker2, Pamela Rowden27, Sara Seager2,19,22, Paula Sarkis18 , Joshua E. Schlieder12 , Lizhou Sha2 , Andrei Tokovinin28 , Guillermo Torres1 , Roland K. Vanderspek2 , Steven Villanueva, Jr.2,36 , Jesus Noel Villaseñor2, Joshua N. Winn15 , Bill Wohler20,25, Ian Wong19,32 , Daniel A. Yahalomi1, Liang Yu2 , Zhuchang Zhan19 , and George Zhou1,33 1 Center for Astrophysics |Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA; [email protected] 2 Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 3 Department of Astronomy, The University of Texas at Austin, Austin, TX 78712, USA 4 Department of Physics, The University of Texas at Dallas, 800 West Campbell Road, Richardson, TX 75080-3021 USA 5 Center of Astro-Engineering UC, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile 6 Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, Macul, Santiago, Chile 7 Millennium Institute for Astrophysics, Chile 8 Department of Physics and Astronomy, Vanderbilt University, Nashville, TN 37235, USA 9 Department of Physics, Fisk University, 1000 17th Avenue North, Nashville, TN 37208, USA 10 Dunlap Institute for Astronomy and Astrophysics, University of Toronto, Ontario M5S 3H4, Canada 11 Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA 12 Exoplanets and Stellar Astrophysics Laboratory, Code 667, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 13 University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, USA 14 Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA 15 Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ, 08544, USA 16 Caltech/IPAC—NASA Exoplanet Science Institute 1200 E. California Avenue, Pasadena, CA 91125, USA 17 American Association of Variable Star Observers, 49 Bay State Road, Cambridge, MA 02138, USA 18 Max-Planck-Institut für Astronomie, Königstuhl 17, Heidelberg D-69117, Germany 19 Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 20 NASA Ames Research Center, Moffett Field, CA, 94035, USA 21 Department of Physics and Astronomy, University of Louisville, Louisville, KY 40292, USA 22 Department of Aeronautics and Astronautics, MIT, 77 Massachusetts Avenue, Cambridge, MA 02139, USA 23 Department of Physics and Astronomy, University of North Carolina at Chapel Hill, Chapel Hill, NC 27599, USA 24 Maury Lewin Astronomical Observatory, Glendora, CA 91741, USA 25 SETI Institute, Mountain View, CA 94043, USA 26 Department of Physics, Lehigh University, 16 Memorial Drive East, Bethlehem, PA 18015, USA 27 School of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK 28 Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile Received 2019 January 28; revised 2019 March 15; accepted 2019 March 18; published 2019 April 29 Abstract We report the discovery of TOI-172 b from the Transiting Exoplanet Survey Satellite (TESS) mission, a massive hot Jupiter transiting a slightly evolved G star with a 9.48-day orbital period. This is the first planet to be confirmed from analysis of only the TESS full frame images, because the host star was not chosen as a two-minute cadence target. From a global analysis of the TESS photometry and follow-up observations carried out by the TESS Follow- up Observing Program Working Group, TOI-172 (TIC 29857954) is a slightly evolved star with an effective = ± = +0.065 = +0.047 temperature of Teff 5645 50 K, a mass of Må 1.128-0.061 Me, radius of Rå 1.777-0.044 Re, a surface = +0.027 +1.6 ( ) gravity of log gå 3.993-0.028, and an age of 7.4-1.5 Gyr. Its planetary companion TOI-172 b has a radius of = +0.032 = +0.22 ( +0.0093) RP 0.965-0.029 RJ, a mass of MP 5.42-0.20 MJ, and is on an eccentric orbit e = 0.3806-0.0090 . TOI-172 b is 29 Juan Carlos Torres Fellow. 30 NASA Sagan Fellow. 31 Kavli Fellow. 32 51 Pegasi b Fellow. 33 NASA Hubble Fellow. 34 Bernoulli fellow. 35 Gruber fellow. 36 Pappalardo Fellow. 1 The Astronomical Journal, 157:191 (13pp), 2019 May Rodriguez et al. one of the few known massive giant planets on a highly eccentric short-period orbit. Future study of the atmosphere of this planet and its system architecture offer opportunities to understand the formation and evolution of similar systems. Key words: planetary systems – planets and satellites: detection – stars: individual (TIC 29857954) Supporting material: data behind figure, machine-readable table 1. Introduction analyzing the eccentricities and orbital architectures of these systems. For example, the orbits of dynamically young hot In only three decades, the field of exoplanets has rapidly Jupiters tend to be more eccentric on average, as would be expanded from its infancy to one of the largest and fastest research expected if at least a fraction of them have undergone eccentric areas in astrophysics. This is largely due to the success of both migration (Quinn et al. 2014; Bonomo et al. 2017).Atthesame ground-based and space-based efforts to discover new planets time, the paucity of highly eccentric migrating Jupiters places an using the transit and radial velocity (RV) techniques. With the fi fi upper limit on the prevalence of HEM in the production of these con rmation of thousands of new planets and the identi cation of systems (Dawson et al. 2015). The presence of additional giant a few thousand more candidates, no survey has been more planets exterior to hot Jupiters but inside the ice line is hard to influential to the field than the Kepler mission (Boruckietal. ( ) ) ( ) reconcile with migration via HEM Schlaufman & Winn 2016 , 2010 .AstheKepler and repurposed K2 Howell et al. 2014 though trends with host-star metallicity hint that disk migration missions have completed, we are now entering the next major and subsequent planet–planet scattering could account for much fi chapter in the eld of exoplanets with the recent launch of the of the hot Jupiter population (Dawson & Murray-Clay 2013). ( ) Transiting Exoplanet Survey Satellite TESS;Rickeretal.2015 . Indeed, it appears that no single migration channel can produce Interestingly, we are still attempting to understand one of the the known population; a recent review of the relevant literature fi rst types of planets ever discovered, hot Jupiters. It is suggests that the combination of two such mechanisms might be commonly believed that close-in giant planets formed farther able to explain the observations (Dawson & Johnson 2018). out in the protoplanetary disk and, through various mechan- Additional study of the dynamically young planets—and their isms, migrated inward. These highly irradiated, Jovian-sized orbital architectures—can refine our understanding of how these planets orbit with periods 10 days, and typically do not have migration mechanisms work together to produce the population of nearby planetary companions (Steffen et al. 2012; Huang et al. giant planets that we observe. 2016), suggesting that they might disrupt planet formation and In this paper, we present the discovery in TESS full frame the orbits of any existing inner planets as they move inward. images leading to follow-up photometry, and precision RV However, the discovery of two small planets bracketing the measurements of a dynamically young, massive Jupiter in a known hot Jupiter, WASP-47b (Becker et al. 2015), suggests ∼9.5-day eccentric orbit (0.38) around a subgiant. Addition- that some giant planets can migrate in a dynamically quiet ally, the evolutionary state of TOI-172 provides a reliable age.

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