TY - JOUR
T1 - TOI-3235 b
T2 - A Transiting Giant Planet around an M4 Dwarf Star
AU - Hobson, Melissa J.
AU - Jordán, Andrés
AU - Bryant, E. M.
AU - Brahm, R.
AU - Bayliss, D.
AU - Hartman, J. D.
AU - Bakos, G. I.
AU - Henning, Th
AU - Almenara, Jose Manuel
AU - Barkaoui, Khalid
AU - Benkhaldoun, Zouhair
AU - Bonfils, Xavier
AU - Bouchy, François
AU - Charbonneau, David
AU - Cointepas, Marion
AU - Collins, Karen A.
AU - Eastman, Jason D.
AU - Ghachoui, Mourad
AU - Gillon, Michaël
AU - Goeke, Robert F.
AU - Horne, Keith
AU - Irwin, Jonathan M.
AU - Jehin, Emmanuel
AU - Jenkins, Jon M.
AU - Latham, David W.
AU - Moldovan, Dan
AU - Murgas, Felipe
AU - Pozuelos, Francisco J.
AU - Ricker, George R.
AU - Schwarz, Richard P.
AU - Seager, S.
AU - Srdoc, Gregor
AU - Striegel, Stephanie
AU - Timmermans, Mathilde
AU - Vanderburg, Andrew
AU - Vanderspek, Roland
AU - Winn, Joshua N.
N1 - Funding Information:
Based on data collected under the ExTrA project at the ESO La Silla Paranal Observatory. ExTrA is a project of Institut de Planétologie et d’Astrophysique de Grenoble (IPAG/CNRS/UGA), funded by the European Research Council under the ERC Grant Agreement No. 337591-ExTrA. This work has been supported by a grant from Labex OSUG@2020 (Investissements d’avenir—ANR10 LABX56). This work has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation. This work has been carried out within the framework of the National Centre of Competence in Research PlanetS supported by the Swiss National Science Foundation under grants 51NF40_182901 and 51NF40_205606. The authors acknowledge the financial support of the SNSF.
Funding Information:
This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). The specific observations analyzed can be accessed via 10.17909/mdsd-2297 . Funding for the TESS mission is provided by NASA’s Science Mission directorate.
Funding Information:
The MEarth Team gratefully acknowledges funding from the David and Lucile Packard Fellowship for Science and Engineering (awarded to D.C.). This material is based upon work supported by the National Science Foundation under grants AST-0807690, AST-1109468, AST-1004488 (Alan T. Waterman Award), and AST-1616624, and upon work supported by the National Aeronautics and Space Administration under grant No. 80NSSC18K0476 issued through the XRP Program. This work is made possible by 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.
Funding Information:
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. M.G. is F.R.S.-FNRS Research Director and E.J. is F.R.S.-FNRS Senior Research Associate. Observations were carried out from ESO La Silla Observatory.
Funding Information:
A.J., R.B., and M.H. acknowledge support from ANID—Millennium Science Initiative—ICN12_009. A.J. acknowledges additional support from FONDECYT project 1210718. R.B. acknowledges support from FONDECYT Project 1120075 and from project IC120009 “Millennium Institute of Astrophysics (MAS)” of the Millennium Science Initiative. This work was funded by the Data Observatory Foundation.
Funding Information:
The contributions at the Mullard Space Science Laboratory by E.M.B. have been supported by STFC through the consolidated grant ST/W001136/1.
Funding Information:
The postdoctoral fellowship of K.B. is funded by F.R.S.-FNRS grant T.0109.20 and by the Francqui Foundation.
Funding Information:
This publication benefits from the support of the French Community of Belgium in the context of the FRIA Doctoral grant awarded to M.T.
Funding Information:
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.
Publisher Copyright:
© 2023. The Author(s). Published by the American Astronomical Society.
PY - 2023/3/1
Y1 - 2023/3/1
N2 - We present the discovery of TOI-3235 b, a short-period Jupiter orbiting an M dwarf with a stellar mass close to the critical mass at which stars transition from partially to fully convective. TOI-3235 b was first identified as a candidate from TESS photometry and confirmed with radial velocities from ESPRESSO and ground-based photometry from HATSouth, MEarth-South, TRAPPIST-South, LCOGT, and ExTrA. We find that the planet has a mass of 0.665 ± 0.025 M J and a radius of 1.017 ± 0.044 R J. It orbits close to its host star, with an orbital period of 2.5926 days but has an equilibrium temperature of ≈ 604 K, well below the expected threshold for radius inflation of hot Jupiters. The host star has a mass of 0.3939 ± 0.0030 M ☉, a radius of 0.3697 ± 0.0018 R ☉, an effective temperature of 3389 K, and a J-band magnitude of 11.706 ± 0.025. Current planet formation models do not predict the existence of gas giants such as TOI-3235 b around such low-mass stars. With a high transmission spectroscopy metric, TOI-3235 b is one of the best-suited giants orbiting M dwarfs for atmospheric characterization.
AB - We present the discovery of TOI-3235 b, a short-period Jupiter orbiting an M dwarf with a stellar mass close to the critical mass at which stars transition from partially to fully convective. TOI-3235 b was first identified as a candidate from TESS photometry and confirmed with radial velocities from ESPRESSO and ground-based photometry from HATSouth, MEarth-South, TRAPPIST-South, LCOGT, and ExTrA. We find that the planet has a mass of 0.665 ± 0.025 M J and a radius of 1.017 ± 0.044 R J. It orbits close to its host star, with an orbital period of 2.5926 days but has an equilibrium temperature of ≈ 604 K, well below the expected threshold for radius inflation of hot Jupiters. The host star has a mass of 0.3939 ± 0.0030 M ☉, a radius of 0.3697 ± 0.0018 R ☉, an effective temperature of 3389 K, and a J-band magnitude of 11.706 ± 0.025. Current planet formation models do not predict the existence of gas giants such as TOI-3235 b around such low-mass stars. With a high transmission spectroscopy metric, TOI-3235 b is one of the best-suited giants orbiting M dwarfs for atmospheric characterization.
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U2 - 10.3847/2041-8213/acbd9a
DO - 10.3847/2041-8213/acbd9a
M3 - Article
AN - SCOPUS:85150771785
SN - 2041-8205
VL - 946
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
IS - 1
M1 - L4
ER -