TOI-4562b: A Highly Eccentric Temperate Jupiter Analog Orbiting a Young Field Star

Creators: Heitzmann, Alexis; Zhou, George; Quinn, Samuel N.; Huang, Chelsea X.; Dong, Jiayin; Bouma, L. G.; Dawson, Rebekah I.; Marsden, Stephen C.; Wright, Duncan; Petit, Pascal; Collins, Karen A.; Barkaoui, Khalid; Wittenmyer, Robert A.; Gillen, Edward; Brahm, Rafael; Hobson, Melissa; Hellier, Coel; Ziegler, Carl; Briceño, César; Law, Nicholas; Mann, Andrew W.; Howell, Steve B.; Gnilka, Crystal L.; Littlefield, Colin; Latham, David W.; Lissauer, Jack J.; Newton, Elisabeth R.; Krolikowski, Daniel M.; Kerr, Ronan; Rampalli, Rayna; Douglas, Stephanie T.; Eisner, Nora L.; Guedj, Nathalie; Sun, Guoyou; Smit, Martin; Huten, Marc; Eschweiler, Thorsten; Abe, Lyu; Guillot, Tristan; Ricker, George; Vanderspek, Roland; Seager, Sara; Jenkins, Jon M.; Ting, Eric B.; Winn, Joshua N.; Ciardi, David R.; Vanderburg, Andrew M.; Burke, Christopher J.; Rodriguez, David R.; Daylan, Tansu

Abstract

We report the discovery of TOI-4562b (TIC-349576261), a Jovian planet orbiting a young F7V-type star, younger than the Praesepe/Hyades clusters (<700 Myr). This planet stands out because of its unusually long orbital period for transiting planets with known masses (P_(orb) = 225.11781_(-0.00022)^(+0.00025) days) and because it has a substantial eccentricity (e = 0.76_(-0.02)^(+0.02)). The location of TOI-4562 near the southern continuous viewing zone of TESS allowed observations throughout 25 sectors, enabling an unambiguous period measurement from TESS alone. Alongside the four available TESS transits, we performed follow-up photometry using the South African Astronomical Observatory node of the Las Cumbres Observatory and spectroscopy with the CHIRON spectrograph on the 1.5 m SMARTS telescope. We measure a radius of 1.118_(+0.013)^(-0.014) R_J and a mass of 2.30_(-0.47)^(+0.48) M_J for TOI-4562b. The radius of the planet is consistent with contraction models describing the early evolution of the size of giant planets. We detect tentative transit timing variations at the ∼20 minutes level from five transit events, favoring the presence of a companion that could explain the dynamical history of this system if confirmed by future follow-up observations. With its current orbital configuration, tidal timescales are too long for TOI-4562b to become a hot Jupiter via high-eccentricity migration though it is not excluded that interactions with the possible companion could modify TOI-4562b's eccentricity and trigger circularization. The characterization of more such young systems is essential to set constraints on models describing giant-planet evolution.

Additional Information

© 2023. 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. We respectfully acknowledge the traditional custodians of the lands on which we conducted this research and throughout Australia. We recognize their continued cultural and spiritual connection to the land, waterways, cosmos and community. We pay our deepest respects to all Elders, present and emerging people of the Giabal, Jarowair and Kambuwal nations, upon whose lands the MINERVA-Australis facility at Mount Kent is located. This research has been supported by an Australian Government Research Training Program Scholarship. G.Z. thanks the support of the ARC DECRA program DE210101893. G.Z. and S.Q. thank the support of the TESS Guest Investigator Program G03007. C.H. thanks the support of the ARC DECRA program DE200101840. E.G. gratefully acknowledges support from the David and Claudia Harding Foundation in the form of a Winton Exoplanet Fellowship. This work was supported by an LSSTC Catalyst Fellowship awarded by LSST Corporation to TD with funding from the John Templeton Foundation grant ID # 62192. This research has used data from the CTIO/SMARTS 1.5 m telescope, which is operated as part of the SMARTS Consortium by RECONS This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. 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 research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. 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 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. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). 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 Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University and the Eberly College of Science. R.B. and M.H. acknowledge support from ANID—Millennium Science Initiative—ICN12_009. N.E. thanks everyone who takes part in the Planet Hunters TESS citizen science project, which contributes to finding new and exciting planetary systems. Facilities: TESS - , Exoplanet Archive - , CTIO 1.5 m - , LCOGT - , Gemini: Zorro - , CTIO SOAR - , ESO 2.2 m. - Software: AstroImageJ (Collins et al. 2017), astropy(Astropy Collaboration et al. 2013, 2018), baffles (Stanford-Moore et al. 2020), batman (Kreidberg 2015), celerite(Foreman-Mackey et al. 2017), emcee (Foreman-Mackey et al. 2013), pyastronomy (Czesla et al. 2019), comove (https://github.com/adamkraus/Comove), pyphot (https://mfouesneau.github.io/pyphot/), radvel (Fulton et al. 2018), scikit-learn (Pedregosa et al. 2011), minimint (https://zenodo.org/record/4900576), numpy (Harris et al. 2020), matplotlib (Hunter 2007), astropy (Astropy Collaboration et al. 2013, 2018), unred (https://github.com/pbrus/unredden-stars), pandas (pandas development team,T 2020), corner (Foreman-Mackey 2016).

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