TOI-3235 b: a transiting giant planet around an M4 dwarf star

Melissa J. Hobson; Andrés Jordán; E. M. Bryant; R. Brahm; D. Bayliss; J. D. Hartman; G. Á. Bakos; Th. Henning; Jose Manuel Almenara; Khalid Barkaoui; Zouhair Benkhaldoun; Xavier Bonfils; François Bouchy; David Charbonneau; Marion Cointepas; Karen A. Collins; Jason D. Eastman; Mourad Ghachoui; Michaël Gillon; Robert F. Goeke; Keith Horne; Jonathan M. Irwin; Emmanuel Jehin; Jon M. Jenkins; David W. Latham; Dan Moldovan; Felipe Murgas; Francisco J. Pozuelos; George R. Ricker; Richard P. Schwarz; S. Seager; Gregor Srdoc; Stephanie Striegel; Mathilde Timmermans; Andrew Vanderburg; Roland Vanderspek; Joshua N. Winn

doi:10.3847/2041-8213/acbd9a

TOI-3235 b: a transiting giant planet around an M4 dwarf star

Melissa J. Hobson^*, Andrés Jordán, E. M. Bryant, R. Brahm, D. Bayliss, J. D. Hartman, G. Á. Bakos, Th. Henning, Jose Manuel Almenara, Khalid Barkaoui, Zouhair Benkhaldoun, Xavier Bonfils, François Bouchy, David Charbonneau, Marion Cointepas, Karen A. Collins, Jason D. Eastman, Mourad Ghachoui, Michaël Gillon, Robert F. GoekeKeith Horne, Jonathan M. Irwin, Emmanuel Jehin, Jon M. Jenkins, David W. Latham, Dan Moldovan, Felipe Murgas, Francisco J. Pozuelos, George R. Ricker, Richard P. Schwarz, S. Seager, Gregor Srdoc, Stephanie Striegel, Mathilde Timmermans, Andrew Vanderburg, Roland Vanderspek, Joshua N. Winn

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

Abstract

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.

Original language	English
Article number	L4
Number of pages	10
Journal	Astrophysical Journal Letters
Volume	946
Issue number	1
Early online date	21 Mar 2023
DOIs	https://doi.org/10.3847/2041-8213/acbd9a
Publication status	Published - 21 Mar 2023

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Hobson, M. J., Jordán, A., Bryant, E. M., Brahm, R., Bayliss, D., Hartman, J. D., Bakos, G. Á., Henning, T., Almenara, J. M., Barkaoui, K., Benkhaldoun, Z., Bonfils, X., Bouchy, F., Charbonneau, D., Cointepas, M., Collins, K. A., Eastman, J. D., Ghachoui, M., Gillon, M., ... Winn, J. N. (2023). TOI-3235 b: a transiting giant planet around an M4 dwarf star. Astrophysical Journal Letters, 946(1), Article L4. https://doi.org/10.3847/2041-8213/acbd9a

@article{b7406a692e884baeb7860c445c110bf8,

title = "TOI-3235 b: a transiting giant planet around an M4 dwarf star",

abstract = "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 MJ and a radius of 1.017 ± 0.044 RJ. 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.",

author = "Hobson, {Melissa J.} and Andr{\'e}s Jord{\'a}n and Bryant, {E. M.} and R. Brahm and D. Bayliss and Hartman, {J. D.} and Bakos, {G. {\'A}.} and Th. Henning and Almenara, {Jose Manuel} and Khalid Barkaoui and Zouhair Benkhaldoun and Xavier Bonfils and Fran{\c c}ois Bouchy and David Charbonneau and Marion Cointepas and Collins, {Karen A.} and Eastman, {Jason D.} and Mourad Ghachoui and Micha{\"e}l Gillon and Goeke, {Robert F.} and Keith Horne and Irwin, {Jonathan M.} and Emmanuel Jehin and Jenkins, {Jon M.} and Latham, {David W.} and Dan Moldovan and Felipe Murgas and Pozuelos, {Francisco J.} and Ricker, {George R.} and Schwarz, {Richard P.} and S. Seager and Gregor Srdoc and Stephanie Striegel and Mathilde Timmermans and Andrew Vanderburg and Roland Vanderspek and Winn, {Joshua N.}",

note = "Funding: 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. 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. 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. The postdoctoral fellowship of K.B. is funded by F.R.S.-FNRS grant T.0109.20 and by the Francqui Foundation.",

year = "2023",

month = mar,

day = "21",

doi = "10.3847/2041-8213/acbd9a",

language = "English",

volume = "946",

journal = "Astrophysical Journal Letters",

issn = "2041-8205",

publisher = "American Astronomical Society",

number = "1",

}

Hobson, MJ, Jordán, A, Bryant, EM, Brahm, R, Bayliss, D, Hartman, JD, Bakos, GÁ, Henning, T, Almenara, JM, Barkaoui, K, Benkhaldoun, Z, Bonfils, X, Bouchy, F, Charbonneau, D, Cointepas, M, Collins, KA, Eastman, JD, Ghachoui, M, Gillon, M, Goeke, RF, Horne, K, Irwin, JM, Jehin, E, Jenkins, JM, Latham, DW, Moldovan, D, Murgas, F, Pozuelos, FJ, Ricker, GR, Schwarz, RP, Seager, S, Srdoc, G, Striegel, S, Timmermans, M, Vanderburg, A, Vanderspek, R & Winn, JN 2023, 'TOI-3235 b: a transiting giant planet around an M4 dwarf star', Astrophysical Journal Letters, vol. 946, no. 1, L4. https://doi.org/10.3847/2041-8213/acbd9a

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. Á.

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: 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. 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. 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. The postdoctoral fellowship of K.B. is funded by F.R.S.-FNRS grant T.0109.20 and by the Francqui Foundation.

PY - 2023/3/21

Y1 - 2023/3/21

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 MJ and a radius of 1.017 ± 0.044 RJ. 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 MJ and a radius of 1.017 ± 0.044 RJ. 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.

U2 - 10.3847/2041-8213/acbd9a

DO - 10.3847/2041-8213/acbd9a

M3 - Article

SN - 2041-8205

VL - 946

JO - Astrophysical Journal Letters

JF - Astrophysical Journal Letters

IS - 1

M1 - L4

ER -

TOI-3235 b: a transiting giant planet around an M4 dwarf star

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