TESS Discovery of a Super-Earth and Three Sub-Neptunes Hosted by the Bright, Sun-like Star HD 108236

Creators: Daylan, Tansu; Pinglé, Kartik; Wright, Jasmine; Günther, Maximilian N.; Stassun, Keivan G.; Kane, Stephen R.; Vanderburg, Andrew; Jontof-Hutter, Daniel; Rodriguez, Joseph E.; Shporer, Avi; Huang, Chelsea X.; Mikal-Evans, Thomas; Badenas-Agusti, Mariona; Collins, Karen A.; Rackham, Benjamin V.; Quinn, Samuel N.; Cloutier, Ryan; Collins, Kevin I.; Guerra, Pere; Jensen, Eric L. N.; Kielkopf, John F.; Massey, Bob; Schwarz, Richard P.; Charbonneau, David; Lissauer, Jack J.; Irwin, Jonathan M.; Baştürk, Özgür; Fulton, Benjamin; Soubkiou, Abderahmane; Zouhair, Benkhaldoun; Howell, Steve B.; Ziegler, Carl; Briceño, César; Law, Nicholas; Mann, Andrew W.; Scott, Nic; Furlan, Elise; Ciardi, David R.; Matson, Rachel; Hellier, Coel; Anderson, David R.; Butler, R. Paul; Crane, Jeffery D.; Teske, Joanna K.; Schectman, Stephen A.; Kristiansen, Martti H.; Terentev, Ivan A.; Schwengeler, Hans Martin; Ricker, George R.; Vanderspek, Roland; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Berta-Thompson, Zachory K.; Bouma, Luke G.; Fong, William; Furesz, Gabor; Henze, Christopher E.; Morgan, Edward H.; Quintana, Elisa; Ting, Eric B.; Twicken, Joseph D.

Abstract

We report the discovery and validation of four extrasolar planets hosted by the nearby, bright, Sun-like (G3V) star HD 108236 using data from the Transiting Exoplanet Survey Satellite (TESS). We present transit photometry, reconnaissance, and precise Doppler spectroscopy, as well as high-resolution imaging, to validate the planetary nature of the objects transiting HD 108236, also known as the TESS Object of Interest (TOI) 1233. The innermost planet is a possibly rocky super-Earth with a period of 3.79523^(+0.00047)_(−0.00044) days and has a radius of 1.586 ± 0.098 R_⊕. The outer planets are sub-Neptunes, with potential gaseous envelopes, having radii of 2.068^(+0.10)_(−0.091) R_⊕, 2.72 ± 0.11 R_⊕, and 3.12^(+0.13)_(−0.12) R_⊕ and periods of 6.20370^(+0.00064)_(−0.00052) days, 14.17555^(+0.00099)_(−0.0011) days, and 19.5917^(+0.0022)_(−0.0020) days, respectively. With V and K_s magnitudes of 9.2 and 7.6, respectively, the bright host star makes the transiting planets favorable targets for mass measurements and, potentially, for atmospheric characterization via transmission spectroscopy. HD 108236 is the brightest Sun-like star in the visual (V) band known to host four or more transiting exoplanets. The discovered planets span a broad range of planetary radii and equilibrium temperatures and share a common history of insolation from a Sun-like star (R_★ = 0.888 ± 0.017 R_⊙, T_(eff) = 5730 ± 50 K), making HD 108236 an exciting, opportune cosmic laboratory for testing models of planet formation and evolution.

Additional Information

© 2021 The American Astronomical Society. Received 2020 April 23; revised 2020 November 19; accepted 2020 December 29; published 2021 January 25. This paper includes data collected by the TESS mission, which 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 Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has also 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. 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. The MEarth Team gratefully acknowledges funding from the David and Lucile Packard Fellowship for Science and Engineering (awarded to D.C.). This material is based on work supported by the National Science Foundation under grants AST-0807690, AST-1109468, AST-1004488 (Alan T. Waterman Award), and AST-1616624. This work is made possible by a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. This material is based on work supported by the National Aeronautics and Space Administration under grant No. 80NSSC18K0476 issued through the XRP Program. Some of the observations in the paper made use of the High-Resolution Imaging instrument Zorro. Zorro was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Zorro was mounted on the Gemini South telescope of the international Gemini Observatory, a program of NSF's OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation, on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). This work makes use of observations from the LCOGT network. Based in part on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia e Inovações do Brasil (MCTI/LNA), the US National Science Foundation's NOIRLab, the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). Support for this work was provided by NASA through grant 18-XRP18_2-0048. T.D. acknowledges support from MIT's Kavli Institute as a Kavli postdoctoral fellow. M.N.G. acknowledges support from MIT's Kavli Institute as a Torres postdoctoral fellow. Contributions from K.P. and J.W. were made through the Harvard-MIT Science Research Mentoring Program (Graur 2018), led by Clara Sousa-Silva, through the 51 Pegasi b Fellowship, and Or Graur. Support for this program is provided by the National Science Foundation under award AST-1602595, City of Cambridge, the John G. Wolbach Library, Cambridge Rotary, Heising-Simons Foundation, and generous individuals. We thank Edward Bryant and the NGTS (Wheatley et al. 2018) team for their HD 108236 observation attempts. Facilities: TESS - , LCOGT - Las Cumbres Observatory Global Telescope, Magellan II - , SMARTS - , Gemini - , SOAR. - Software: python (van Rossum 1995), matplotlib (Hunter 2007), seaborn (https://seaborn.pydata.org/index.html), numpy (van der Walt et al. 2011), scipy (Jones et al. 2001), allesfitter (Günther & Daylan 2019, 2020; J. T. Teske et al. 2021, in preparation), ellc (Maxted 2016), EXOFASTv2 (Eastman et al. 2019), emcee (Foreman-Mackey et al. 2013), celerite (Foreman-Mackey et al. 2017), corner (Foreman-Mackey 2016). dynesty (Speagle 2020), AstroImageJ (Collins et al. 2017), Tapir (Jensen 2013), exoplanet (Foreman-Mackey et al. 2020), Transit Least Squares (Hippke & Heller 2019), astroquery (Ginsburg et al. 2019), Lightkurve (Lightkurve Collaboration et al. 2018), pymc3 (Salvatier et al. 2016).

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