Validation of 13 Hot and Potentially Terrestrial TESS Planets

Creators: Giacalone, Steven; Dressing, Courtney D.; Hedges, Christina; Kostov, Veselin B.; Collins, Karen A.; Jensen, Eric L. N.; Yahalomi, Daniel A.; Bieryla, Allyson; Ciardi, David R.; Howell, Steve B.; Lillo-Box, Jorge; Barkaoui, Khalid; Winters, Jennifer G.; Matthews, Elisabeth; Livingston, John H.; Quinn, Samuel N.; Safonov, Boris S.; Cadieux, Charles; Furlan, E.; Crossfield, Ian J. M.; Mandell, Avi M.; Gilbert, Emily A.; Kruse, Ethan; Quintana, Elisa V.; Ricker, George R.; Seager, S.; Winn, Joshua N.; Jenkins, Jon M.; Duffy Adkins, Britt; Baker, David; Barclay, Thomas; Barrado, David; Batalha, Natalie M.; Belinski, Alexander A.; Benkhaldoun, Zouhair; Buchhave, Lars A.; Cacciapuoti, Luca; Chontos, Ashley; Christiansen, Jessie L.; Cloutier, Ryan; Collins, Kevin I.; Conti, Dennis M.; Cutting, Neil; Dixon, Scott; Doyon, René; El Mufti, Mohammed; Esparza-Borges, Emma; Essack, Zahra; Fukui, Akihiko; Gan, Tianjun; Gary, Kaz; Ghachoui, Mourad; Gillon, Michaël; Girardin, Eric; Glidden, Ana; Gonzales, Erica J.; Guerra, Pere; Horch, Elliott P.; Hełminiak, Krzysztof G.; Howard, Andrew W.; Huber, Daniel; Irwin, Jonathan M.; Isopi, Giovanni; Jehin, Emmanuël; Kagetani, Taiki; Kane, Stephen R.; Kawauchi, Kiyoe; Kielkopf, John F.; Lewin, Pablo; Luker, Lindy; Lund, Michael B.; Mallia, Franco; Mao, Shude; Massey, Bob; Matson, Rachel A.; Mireles, Ismael; Mori, Mayuko; Murgas, Felipe; Narita, Norio; O'Dwyer, Tanner; Petigura, Erik A.; Polanski, Alex S.; Pozuelos, Francisco J.; Palle, Enric; Parviainen, Hannu; Plavchan, Peter P.; Relles, Howard M.; Robertson, Paul; Rose, Mark E.; Rowden, Pamela; Roy, Arpita; Savel, Arjun B.; Schlieder, Joshua E.; Schnaible, Chloe; Schwarz, Richard P.; Sefako, Ramatholo; Selezneva, Aleksandra; Skinner, Brett; Stockdale, Chris; Strakhov, Ivan A.; Tan, Thiam-Guan; Torres, Guillermo; Tronsgaard, René; Twicken, Joseph D.; Vermilion, David; Waite, Ian A.; Walter, Bradley; Wang, Gavin; Ziegler, Carl; Zou, Yujie

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Abstract

The James Webb Space Telescope will be able to probe the atmospheres and surface properties of hot, terrestrial planets via emission spectroscopy. We identify 18 potentially terrestrial planet candidates detected by the Transiting Exoplanet Survey Satellite (TESS) that would make ideal targets for these observations. These planet candidates cover a broad range of planet radii (R_p ∼ 0.6–2.0 R_⊕) and orbit stars of various magnitudes (K_s = 5.78–10.78, V = 8.4–15.69) and effective temperatures (T_(eff) ∼ 3000–6000 K). We use ground-based observations collected through the TESS Follow-up Observing Program (TFOP) and two vetting tools—DAVE and TRICERATOPS—to assess the reliabilities of these candidates as planets. We validate 13 planets: TOI-206 b, TOI-500 b, TOI-544 b, TOI-833 b, TOI-1075 b, TOI-1411 b, TOI-1442 b, TOI-1693 b, TOI-1860 b, TOI-2260 b, TOI-2411 b, TOI-2427 b, and TOI-2445 b. Seven of these planets (TOI-206 b, TOI-500 b, TOI-1075 b, TOI-1442 b, TOI-2260 b, TOI-2411 b, and TOI-2445 b) are ultra-short-period planets. TOI-1860 is the youngest (133 ± 26 Myr) solar twin with a known planet to date. TOI-2260 is a young (321 ± 96 Myr) G dwarf that is among the most metal-rich ([Fe/H] = 0.22 ± 0.06 dex) stars to host an ultra-short-period planet. With an estimated equilibrium temperature of ∼2600 K, TOI-2260 b is also the fourth hottest known planet with R_p < 2 R_⊕.

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 2021 July 30; revised 2021 December 8; accepted 2021 December 13; published 2022 January 28. We thank the NASA TESS Guest Investigator Program for supporting this work through grant 80NSSC18K1583 (awarded to C.D.D.). S.G. and C.D.D. also appreciate and acknowledge support from the Hellman Fellows Fund, the Alfred P. Sloan Foundation, the David and Lucile Packard Foundation, and the NASA Exoplanets Research Program (XRP) through grant 80NSSC20K0250. We acknowledge the use of public TESS Alert data from the 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. 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 the National Optical Astronomy Observatory. NESSI was funded by the NASA Exoplanet Exploration Program and the NASA Ames Research Center. NESSI was built at the Ames Research Center by S.B.H., Nic Scott, E.P.H., and Emmett Quigley. The authors are honored to be permitted to conduct observations on Iolkam Du'ag (Kitt Peak), a mountain within the Tohono O'odham Nation with particular significance to the Tohono O'odham people. MEarth is funded by the David and Lucile Packard Fellowship for Science and Engineering, the National Science Foundation under grants AST-0807690, AST-1109468, AST-1004488 (Alan T. Waterman Award) and AST-1616624, and the John Templeton Foundation. This publication was made possible through the support of 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. 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. D.H. acknowledges support from the Alfred P. Sloan Foundation, the National Aeronautics and Space Administration (80NSSC18K1585, 80NSSC19K0379), and the National Science Foundation (AST-1717000). Some of the observations in the paper made use of the High-Resolution Imaging instrument(s) 'Alopeke (and/or Zorro). 'Alopeke (and/or Zorro) was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by S.B.H., Nic Scott, E.P.H., and Emmett Quigley. Data were reduced using a software pipeline originally written by E. P. Horch and Mark Everett. 'Alopeke (and/or Zorro) was mounted on the Gemini North (and/or 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). These observations were collected under program GN-2019B-LP-101. Observations acquired with Gemini-S/DSSI were collected as a part of program GS-2018A-Q-202 (PI: J. Winters). Some of the results in this paper are based on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. A.A.B., B.S.S., and I.A.S. acknowledge the support of the Ministry of Science and Higher Education of the Russian Federation under grant 075-15-2020-780 (N13.1902.21.0039). This paper is partially based on observations made at the CMO SAI MSU with the support of the M.V. Lomonosov Moscow State University Program of Development. Based on observations at Cerro Tololo Inter-American Observatory at NSF's NOIRLab (NOIRLab Prop. IDs 2019A-0294, 2019B-0302, 2020A-0390, 2020B-0262, 2021A-0268; PI: S. Quinn), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. This research has been supported by RECONS (www.recons.org) members Todd Henry, Hodari James, Leonardo Paredes, and Wei-Chun Jao, who provided data as part of the CHIRON program on the CTIO/SMARTS 1.5 m, which is operated as part of the SMARTS Consortium. 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, with the participation of the Swiss National Science Foundation (SNF). M. Gillon and E.J. are F.R.S.-FNRS Senior Research Associate. This work is partly supported by JSPS KAKENHI grant Nos. JP20K14518, JP17H04574, and JP18H05439, grant-in-Aid for JSPS Fellows, grant No. JP20J21872, JST PRESTO grant No. JPMJPR1775, JST CREST grant No. JPMJCR1761, and the Astrobiology Center of National Institutes of Natural Sciences (NINS) (grant No. AB031010). This paper is based on observations made with the MuSCAT2 instrument, developed by ABC, at Telescopio Carlos Sánchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. This paper is based on observations made with the MuSCAT3 instrument, developed by the Astrobiology Center and under financial supports by JSPS KAKENHI (JP18H05439) and JST PRESTO (JPMJPR1775), at Faulkes Telescope North on Maui, HI, operated by the Las Cumbres Observatory. This work makes use of observations from the LCOGT network. Work by J.N.W. was supported by the Heising-Simons Foundation. We thank Rhodes Hart for his contributions to this paper. Facilities: TESS - , CAO:2.2 m (AstraLux) - , WIYN (NESSI) - , SOAR (HRCam) - , Shane (ShARCS) - , Hale (PHARO) - , Gemini:Gillett ('Alopeke) - , Gemini:South (Zorro and DSSI) - , Keck:II (NIRC2) - , FLWO:1.5 m (TRES) - , NOT (FIES) - , CTIO:1.5 m (CHIRON) - , Keck:I (HIRES) - , MEearth - , LCOGT - , OMM:1.6 (PESTO) - , OAO:1.88 m (MuSCAT) - , TRAPPIST - , SAAO:0.5 m - , Sanchez (MuSCAT2). - Software: exoplanet (Foreman-Mackey et al. 2021), lightkurve (Lightkurve Collaboration et al. 1812), DAVE (Kostov et al. 2019), TRICERATOPS(Giacalone & Dressing 2020; Giacalone et al. 2021), Tapir (Jensen 2013), AstroImageJ (Collins et al. 2017).

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