TESS giants transiting giants V – two hot Jupiters orbiting red giant hosts

Creators: Pereira, Filipe¹; Grunblatt, Samuel K.^{2, 3, 4}; Psaridi, Angelica⁵; Campante, Tiago L.¹; Cunha, Margarida S.¹; Santos, Nuno C.¹; Bossini, Diego¹; Thorngren, Daniel⁴; Hellier, Coel⁶; Bouchy, François⁵; Lendl, Monika⁵; Mounzer, Dany⁵; Udry, Stéphane⁵; Beard, Corey⁷; Brinkman, Casey L.⁸; Isaacson, Howard^{9, 10}; Quinn, Samuel N.¹¹; Tyler, Dakotah¹²; Zhou, George¹⁰; Howell, Steve B.¹³; Howard, Andrew W.¹⁴; Jenkins, Jon M.¹³; Seager, Sara¹⁵; Vanderspek, Roland K.¹⁵; Winn, Joshua N.¹⁶; Saunders, Nicholas⁸; Huber, Daniel^{8, 17}

1. University of Porto
2. American Museum of Natural History
3. Flatiron Institute
4. Johns Hopkins University
5. University of Geneva
6. Keele University
7. University of California, Irvine
8. University of Hawaii at Manoa
9. University of California, Berkeley
10. University of Southern Queensland
11. Harvard-Smithsonian Center for Astrophysics
12. University of California, Los Angeles
13. Ames Research Center
14. California Institute of Technology
15. Massachusetts Institute of Technology
16. Princeton University
17. University of Sydney

Abstract

In this work, we present the discovery and confirmation of two hot Jupiters orbiting red giant stars, TOI-4377 b and TOI-4551 b, observed by Transiting Exoplanet Survey Satellite in the Southern ecliptic hemisphere and later followed-up with radial-velocity (RV) observations. For TOI-4377 b, we report a mass of 0.957_(−0.087)_(+0.089) MJ and a inflated radius of 1.348 ± 0.081 R_J orbiting an evolved intermediate-mass star (1.36 M_⊙ and 3.52 R_⊙; TIC 394918211) on a period of of 4.378 d. For TOI-4551 b, we report a mass of 1.49 ± 0.13 M_J and a radius that is not obviously inflated of 1.058_(−0.062)_(+0.110) RJ⁠, also orbiting an evolved intermediate-mass star (1.31 M_⊙ and 3.55 R_⊙; TIC 204650483) on a period of 9.956 d. We place both planets in context of known systems with hot Jupiters orbiting evolved hosts, and note that both planets follow the observed trend of the known stellar incident flux-planetary radius relation observed for these short-period giants. Additionally, we produce planetary interior models to estimate the heating efficiency with which stellar incident flux is deposited in the planet’s interior, estimating values of 1.91±0.48 per cent and 2.19±0.45 per cent for TOI-4377 b and TOI-4551 b, respectively. These values are in line with the known population of hot Jupiters, including hot Jupiters orbiting main-sequence hosts, which suggests that the radii of our planets have re-inflated in step with their parent star’s brightening as they evolved into the post-main sequence. Finally, we evaluate the potential to observe orbital decay in both systems.

Copyright and License

This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.

Acknowledgement

This work was supported by FCT—Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020—Programa Operacional Competitividade e Internacionalização by these grants: UIDB/04434/2020 and UIDP/04434/2020. SKG acknowledges support from the National Aeronautics and Space Administration under grants 80NSSC19K0593 and 80NSSC21K0781 issued through the TESS Guest Investigator Program. TLC is supported by FCT in the form of a work contract (CEECIND/00476/2018). MSC acknowledges the support from the FCT through a work contract (CEECIND/02619/2017). Co-funded by the European Union (ERC, FIERCE, 101052347). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. ML acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. SQ acknowledges support from the TESS GI Program under award 80NSSC21K1056 and from the TESS mission via subaward s3449 from MIT. We thank the Swiss National Science Foundation (SNSF) and the Geneva University for their continuous support to our planet low-mass companion search programs. This work was been in particular carried out within the framework of the Swiss National Centre for Competence in Research (NCCR) PlanetS supported by the Swiss National Science Foundation (SNSF) under grants 51NF40_182901 and 51NF40_205606. ML and BA acknowledge support of the Swiss National Science Foundation under grant no. PCEFP2_194576. This publication makes use of The Data and Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva (CH) dedicated to extrasolar planet data visualization, exchange, and analysis. DACE is a platform of NCCR PlanetS and is available at https://dace.unige.ch. Some of the observations in this paper made use of the High-Resolution Imaging instrument Zorro and were obtained under Gemini LLP proposal number: GN/S-2021A-LP-105. 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 paper made use of data collected by the TESS mission and are publicly available from the MAST operated by the Space Telescope Science Institute (STScI). Funding for the TESS mission is provided by NASA’s Science Mission Directorate. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS SPOC. 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. DH acknowledges support from the Alfred P. Sloan Foundation, the National Aeronautics and Space Administration (80NSSC21K0652), and the Australian Research Council (FT200100871).

Software References

This research made use of open-source software, namely: exoplanet (Foreman-Mackey et al. 2021a, b) and its dependencies (Astropy Collaboration 2013, 2018; Kipping 2013; Salvatier, Wiecki & Fonnesbeck 2016; The Theano Development Team et al. 2016; Foreman-Mackey et al. 2017; Foreman-Mackey 2018; Kumar et al. 2019; Luger et al. 2019; Agol, Luger & Foreman-Mackey 2020), Tesscut (Brasseur et al. 2019), astropy (Astropy Collaboration 2013, 2018), eleanor (Feinstein et al. 2019), transitleastsquares (Hippke & Heller 2019), and vespa (Morton 2012, 2015).

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