Migration and Evolution of giant ExoPlanets (MEEP). I. Nine Newly Confirmed Hot Jupiters from the TESS Mission

Creators: Schulte, Jack; Rodriguez, Joseph E.; Bieryla, Allyson; Quinn, Samuel N.; Collins, Karen A.; Yee, Samuel W.; Nine, Andrew C.; Soares-Furtado, Melinda; Latham, David W.; Eastman, Jason D.; Barkaoui, Khalid; Ciardi, David R.; Dragomir, Diana; Everett, Mark E.; Giacalone, Steven; Mireles, Ismael; Murgas, Felipe; Narita, Norio; Shporer, Avi; Strakhov, Ivan A.; Striegel, Stephanie; Vaňko, Martin; Vowell, Noah; Wang, Gavin; Ziegler, Carl; Bellaver, Michael; Benni, Paul; Bergeron, Serge; Boffin, Henri M. J.; Briceño, César; Clark, Catherine A.; Collins, Kevin I.; de Leon, Jerome P.; Dressing, Courtney D.; Evans, Phil; Esparza-Borges, Emma; Fedewa, Jeremy; Fukui, Akihiko; Gan, Tianjun; Gerasimov, Ivan S.; Hartman, Joel D.; Gill, Holden; Gillon, Michaël; Horne, Keith; Horta, Ferran Grau; Howell, Steve B.; Isogai, Keisuke; Jehin, Emmanuël; Jenkins, Jon M.; Karjalainen, Raine; Kielkopf, John F.; Lester, Kathryn V.; Littlefield, Colin; Lund, Michael B.; Mann, Andrew W.; McCormack, Mason; Michaels, Edward J.; Painter, Shane; Palle, Enric; Parviainen, Hannu; Peterson, David-Michael; Pozuelos, Francisco J.; Raup, Zachary; Reed, Phillip; Relles, Howard M.; Ricker, George R.; Savel, Arjun B.; Schwarz, Richard P.; Seager, S.; Sefako, Ramotholo; Srdoc, Gregor; Stockdale, Chris; Sullivan, Hannah; Timmermans, Mathilde; Winn, Joshua N.

Abstract

Hot Jupiters were many of the first exoplanets discovered in the 1990s, but in the decades since their discovery the mysteries surrounding their origins have remained. Here we present nine new hot Jupiters (TOI-1855 b, TOI-2107 b, TOI-2368 b, TOI-3321 b, TOI-3894 b, TOI-3919 b, TOI-4153 b, TOI-5232 b, and TOI-5301 b) discovered by NASA's TESS mission and confirmed using ground-based imaging and spectroscopy. These discoveries are the first in a series of papers named the Migration and Evolution of giant ExoPlanets survey and are part of an ongoing effort to build a complete sample of hot Jupiters orbiting FGK stars, with a limiting Gaia G-band magnitude of 12.5. This effort aims to use homogeneous detection and analysis techniques to generate a set of precisely measured stellar and planetary properties that is ripe for statistical analysis. The nine planets presented in this work occupy a range of masses (0.55M_J < M_P < 3.88M_J) and sizes (0.967R_J < R_P < 1.438R_J) and orbit stars that have an effective temperature in the range of 5360 K < T_eff < 6860 K with Gaia G-band magnitudes ranging from 11.1 to 12.7. Two of the planets in our sample have detectable orbital eccentricity: TOI-3919 b (𝑒 = 0.259_(−0.036)^(+0.033)) and TOI-5301 b (𝑒 = 0.33_(−0.10)^(+0.11)). These eccentric planets join a growing sample of eccentric hot Jupiters that are consistent with high-eccentricity tidal migration, one of the three most prominent theories explaining hot Jupiter formation and evolution.

Copyright and License

© 2024. 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.

Acknowledgement

We thank the anonymous reviewer for helpful comments that improved the quality of this paper. Many of the data used in this paper are available on the Mikulski Archive for Space Telescopes (MAST) and can be accessed at 10.17909/t9-nmc8-f686 (TESS-SPOC 2 minutes light curves), doi:10.17909/0cp4-2j79 (TESS-SPOC full-frame images), 10.17909/t9-r086-e880 (TESS QLP light curves), and 10.17909/t9-2tc5-a751 (TESS data validation files). This research has made use of the Vizier catalog access tool, CDS, Strasbourg, France (DOI 10.26093/cds/vizier). The original description of the Vizier service was published in 2000, A&AS 143, 23. This research has made use of the NASA Exoplanet Archive and the Exoplanet Follow-up Observation Program (ExoFOP; DOI: 10.26134/ExoFOP5) website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. E.P. acknowledges funding from the Spanish Ministry of Economics and Competitiveness through project PGC2021-125627OB-C32. TRAPPIST-South is funded by the Belgian National Fund for Scientific Research (F.R.S.-FNRS) under grant PDR T.0120.21, with the participation of the Swiss National Science Fundation (SNF). M.G. and E.J. are FNRS Senior Research Associates. The postdoctoral fellowship of K.B. is funded by F.R.S.-FNRS grant T.0109.20 and by the Francqui Foundation. This work is partly supported by JSPS KAKENHI grant Nos. JP17H04574, JP18H05439, JP20K14521, and JP21K13955 and JST CREST grant No. JPMJCR1761. This article includes 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 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 (2022A-543544, PI: Yee), administered by the NASA Exoplanet Science Institute. 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. The research of M.V. was supported by the Slovak Research and Development Agency, under contract No. APVV-20-0148. Some of the observations in this paper made use of the High-Resolution Imaging instrument Alopeke/Zorro and were obtained under Gemini LLP proposal No. GN/S-2021A-LP-105. Alopeke/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. Alopeke/Zorro was mounted on the Gemini North/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). 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 (MCTI/LNA) do Brasil, the US National Science Foundation's NOIRLab, the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). This publication benefits from the support of the French Community of Belgium in the context of the FRIA doctoral grant awarded to M.T. We acknowledge financial support from the Agencia Estatal de Investigación of the Ministerio de Ciencia e Innovación MCIN/AEI/10.13039/501100011033 and the ERDF "A way of making Europe" through project PID2021-125627OB-C32, and from the Centre of Excellence "Severo Ochoa" award to the Instituto de Astrofisica de Canarias. P.A.R. acknowledges support from the National Science Foundation under grant No. 1952545. R.K. acknowledges the support by Inter-transfer grant No. LTT-20015. F.J.P. acknowledges financial support from the grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033 and through projects PID2019-109522GB-C52 and PID2022-137241NB-C43. 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. This paper made use of data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST) operated by the Space Telescope Science Institute (STScI). Funding for the TESS mission is provided by NASA's Science Mission Directorate. H.P. acknowledges support by the Spanish Ministry of Science and Innovation with the Ramon y Cajal fellowship No. RYC2021-031798-I. C.A.C. acknowledges that this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004).

Facilities

TESS - , FLWO 1.5 m (TRES) - , SMARTS 1.5 m (CHIRON) - , SOAR 4.1 m (Goodman, HRCam) - The Southern Astrophysical Research Telescope, LCOGT - Las Cumbres Observatory Global Telescope, NAOJ-Okayama 1.88 m (MuSCAT2) - , TCS 1.52 m (MuSCAT) - , FLWO 1.2 m (KeplerCam) - , WIYN 3.5 m (NEID, NESSI) - Wisconsin-Indiana-Yale-NOAO Telescope, Shane 3 m (ShARCS) - Lick Observatory's 3m Shane Telescope, Palomar 5 m (PHARO) - , SAI 2.5 m - , Gemini North 8 m ('Alopeke) - , Gemini South 8 m (Zorro) - , Keck 10 m (NIRC2) - , TRAPPIST-South 0.6m -

Software References

EXOFASTv2 (Eastman et al. 2019), lightkurve (Lightkurve Collaboration et al. 1812), AstroImageJ (Collins et al. 2017), TAPIR (Jensen 2013), astropy (Astropy Collaboration et al. 2013, 2018), numpy (Harris et al. 2020), matplotlib (Hunter 2007), pandas (The pandas development Team 2023), scipy (Virtanen et al. 2020)

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