TESS discovery of a sub-Neptune orbiting a mid-M dwarf TOI-2136

Creators: Gan, Tianjun; Soubkiou, Abderahmane; Wang, Sharon X.; Benkhaldoun, Zouhair; Mao, Shude; Artigau, Étienne; Fouqué, Pascal; Arnold, Luc; Giacalone, Steven; Theissen, Christopher A.; Aganze, Christian; Burgasser, Adam; Collins, Karen A.; Shporer, Avi; Barkaoui, Khalid; Ghachoui, Mourad; Howell, Steve B.; Lamman, Claire; Demangeon, Olivier D. S.; Burdanov, Artem; Cadieux, Charles; Chouqar, Jamila; Collins, Kevin I.; Cook, Neil J.; Delrez, Laetitia; Demory, Brice-Olivier; Doyon, René; Dransfield, Georgina; Dressing, Courtney D.; Ducrot, Elsa; Fan, Jiahao; Garcia, Lionel; Gill, Holden; Gillon, Michaël; Gnilka, Crystal L.; Gómez Maqueo Chew, Yilen; Günther, Maximilian N.; Henze, Christopher E.; Huang, Chelsea X.; Jehin, Emmanuel; Jensen, Eric L. N.; Lin, Zitao; Manset, Nadine; McCormac, James; Murray, Catriona A.; Niraula, Prajwal; Pedersen, Peter P.; Pozuelos, Francisco J.; Queloz, Didier; Rackham, Benjamin V.; Savel, Arjun B.; Schanche, Nicole; Schwarz, Richard P.; Sebastian, Daniel; Thompson, Samantha; Timmermans, Mathilde; Triaud, Amaury H. M. J.; Vezie, Michael; Wells, Robert D.; de Wit, Julien; Ricker, George R.; Vanderspek, Roland; Latham, David W.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.

Abstract

We present the discovery of TOI-2136 b, a sub-Neptune planet transiting a nearby M4.5V-type star every 7.85 d, identified through photometric measurements from the Transiting Exoplanet Survey Satellite (TESS) mission. The host star is located 33 pc away with a radius of R* = 0.34 ± 0.02 R_⊙, a mass of 0.34 ± 0.02 M_⊙⁠, and an effective temperature of 3342 ± 100 K. We estimate its stellar rotation period to be 75 ± 5 d based on archival long-term photometry. We confirm and characterize the planet based on a series of ground-based multiwavelength photometry, high-angular-resolution imaging observations, and precise radial velocities from Canada–France–Hawaii Telescope (CFHT)/SpectroPolarimètre InfraROUge (SPIRou). Our joint analysis reveals that the planet has a radius of 2.20 ± 0.17 R_⊕ and a mass of 6.4 ± 2.4 M_⊕. The mass and radius of TOI-2136 b are consistent with a broad range of compositions, from water-ice to gas-dominated worlds. TOI-2136 b falls close to the radius valley for M dwarfs predicted by thermally driven atmospheric mass-loss models, making it an interesting target for future studies of its interior structure and atmospheric properties.

Additional Information

© 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Received: 21 February 2022. Revision received: 27 April 2022. Accepted: 20 May 2022. Published: 30 May 2022. Corrected and typeset: 29 June 2022. We are grateful to Coel Hellier for the insights regarding the WASP data. We thank Ryan Cloutier for useful discussions. We also thank Elise Furlan for the contributions to the speckle data. This work is partly supported by the National Science Foundation of China (Grant Nos 11390372, 11761131004, and12133005 to SM and TG). ASo was supported by a grant from the MOBILE 2 BE project, coordinated by the University of Porto in the framework of the European Programme Erasmus plus. BVR thanks the Heising-Simons Foundation for support. YGMC is supported by UNAM-PAPIIT-IG101321. CXH's work is supported by ARC DECRA Grant. ODSD is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by FCT. This research uses data obtained through the China's Telescope Access Program (TAP), which has been funded by the TAP member institutes. This work uses observations obtained with SPIRou, an international project led by Institut de Recherche en Astrophysique et Planetologie, Toulouse, France. 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. We further acknowledge that Lick Observatory sits on the unceded ancestral homelands of the Chochenyo and Tamyen Ohlone peoples, including the Alson and Socostac tribes, who were the original inhabitants of the area that includes Mt. Hamilton. This publication benefits from the support of the French Community of Belgium in the context of the FRIA Doctoral Grant awarded to MT. The research leading to these results has received funding from the ARC grant for Concerted Research Actions, financed by the Federation Wallonia-Brussels. TRAPPIST is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, FNRS) under the grant PDR T.0120.21. TRAPPIST-North is a project funded by the University of Liège (Belgium), in collaboration with Cadi Ayyad University of Marrakech (Morocco). MG and EJ are F.R.S.-FNRS Senior Research Associate. CL is supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE1745303. Some of the observations in the paper made use of the High-Resolution Imaging instrument 'Alopeke obtained under Gemini LLP Proposal Number: GN/S-2021A-LP-105. 'Alopeke 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 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). 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. The ULiege's contribution to SPECULOOS has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013) (grant agreement no. 336480/SPECULOOS), from the Balzan Prize Foundation, from the Belgian Scientific Research Foundation (F.R.S. - FNRS; grant no. T.0109.20), from the University of Liège, and from the ARC grant for Concerted Research Actions financed by the Federation Wallonia-Brussels. LD is an F.R.S. - FNRS Post-doctoral Researcher. VVG is F.R.S - FNRS Research Associate. This work is supported by a grant from the Simons Foundation (PI: Queloz, grant number 327127). JdW and MT gratefully acknowledge financial support from the Heising-Simons Foundation, Dr Colin Masson, and Dr Peter A. Gilman for Artemis, the first telescope of the SPECULOOS network situated in Tenerife, Spain. MNG acknowledges support from the European Space Agency (ESA) as an ESA Research Fellow. This work is supported by the Swiss National Science Foundation (PP00P2-163967, PP00P2-190080 and the National Centre for Competence in Research PlanetS). This work has received fund from the European Research Council (ERC) under the European Union's Horizon 2020 Framework Programme (grant agreement no. 803193/BEBOP), from the MERAC Foundation, and from the Science and Technology Facilities Council (STFC; grant no. ST/S00193X/1). This work was supported by Fundação para a Ciência e a Tecnologia (FCT) and Fundo Europeu de Desenvolvimento Regional (FEDER) via COMPETE2020 through the research grants UIDB/04434/2020, UIDP/04434/2020, PTDC/FIS-AST/32113/2017, POCI-01-0145-FEDER-032113, PTDC/FIS-AST/28953/2017, and POCI-01-0145-FEDER-028953. The National Geographic Society – Palomar Observatory Sky Atlas (POSS-I) was made by the California Institute of Technology with grants from the National Geographic Society. Funding for the TESS mission is provided by NASA Science Mission Directorate. We acknowledge the use of TESS public 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 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). 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 made use of TPFPLOTTER by J. Lillo-Box (publicly available in www.github.com/jlillo/tpfplotter), which also made use of the PYTHON packages ASTROPY, LIGHTKURVE, MATPLOTLIB, and NUMPY. Based on observations obtained at the Canada–France–Hawaii Telescope (CFHT) that is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. The observations at the CFHT were performed with care and respect from the summit of Maunakea that is a significant cultural and historic site. DATA AVAILABILITY. This paper includes photometric data collected by the TESS mission and ground instruments, which are publicly available in ExoFOP, at https://exofop.ipac.caltech.edu/tess/target.php?id = 336128819. All spectroscopy data underlying this paper are listed in the Appendix. All of the high-resolution speckle imaging data are available at the NASA Exoplanet Archive with no proprietary period.

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