A long-period transiting substellar companion in the super-Jupiters to brown dwarfs mass regime and a prototypical warm-Jupiter detected by TESS

Matias I. Jones; Yared Reinarz; Rafael Brahm; Marcelo Tala Pinto; Jan Eberhardt; Felipe Rojas; Amaury H. M. J. Triaud; Arvind F. Gupta; Carl Ziegler; Melissa J. Hobson; Andrés Jordán; Thomas Henning; Trifon Trifonov; Martin Schlecker; Nestor Espinoza; Pascal Torres-Miranda; Paula Sarkis; Solène Ulmer-Moll; Monika Lendl; Murat Uzundag; Maximiliano Moyano; Katharine Hesse; Douglas A. Caldwell; Avi Shporer; Michael B. Lund; Jon M. Jenkins; Sara Seager; Joshua N. Winn; George R. Ricker; Christopher J. Burke; Pedro Figueira; Angelica Psaridi; Khaled Al Moulla; Dany Mounzer; Matthew R. Standing; David V. Martin; Georgina Dransfield; Thomas Baycroft; Diana Dragomir; Gavin Boyle; Vincent Suc; Andrew W. Mann; Mathilde Timmermans; Elsa Ducrot; Matthew J. Hooton; Sebastián Zúñiga-Fernández; Daniel Sebastian; Michael Gillon; Didier Queloz; Joe Carson; Jack J. Lissauer

doi:10.1051/0004-6361/202348147

A long-period transiting substellar companion in the super-Jupiters to brown dwarfs mass regime and a prototypical warm-Jupiter detected by TESS

Matias I. Jones, Yared Reinarz, Rafael Brahm, Marcelo Tala Pinto, Jan Eberhardt, Felipe Rojas, Amaury H. M. J. Triaud, Arvind F. Gupta, Carl Ziegler, Melissa J. Hobson, Andrés Jordán, Thomas Henning, Trifon Trifonov, Martin Schlecker, Nestor Espinoza, Pascal Torres-Miranda, Paula Sarkis, Solène Ulmer-Moll, Monika Lendl, Murat UzundagMaximiliano Moyano, Katharine Hesse, Douglas A. Caldwell, Avi Shporer, Michael B. Lund, Jon M. Jenkins, Sara Seager, Joshua N. Winn, George R. Ricker, Christopher J. Burke, Pedro Figueira, Angelica Psaridi, Khaled Al Moulla, Dany Mounzer, Matthew R. Standing, David V. Martin, Georgina Dransfield, Thomas Baycroft, Diana Dragomir, Gavin Boyle, Vincent Suc, Andrew W. Mann, Mathilde Timmermans, Elsa Ducrot, Matthew J. Hooton, Sebastián Zúñiga-Fernández, Daniel Sebastian, Michael Gillon, Didier Queloz, Joe Carson, Jack J. Lissauer

Physics and Astronomy

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Abstract

We report on the confirmation and follow-up characterization of two long-period transiting substellar companions on low-eccentricity orbits around TIC 4672985 and TOI-2529, whose transit events were detected by the TESS space mission. Ground-based photometric and spectroscopic follow up from different facilities, confirmed the substellar nature of TIC 4672985 b, a massive gas giant, in the transition between the super-Jupiters and brown-dwarfs mass regime. From the joint analysis we derived the following orbital parameters: P = 69.0480^+0.0004_−0.0005 d, M_p = 12.74^+1.01_−1.01M_J, R_p =1.026^+0.065_−0.067R_J and e = 0.018^+0.004_−0.004 . In addition, the RV time series revealed a significant trend at the ∼ 350 m s⁻¹ yr⁻¹level, which is indicative of the presence of a massive outer companion in the system. TIC 4672985 b is a unique example of a transiting substellar companion with a mass above the deuterium-burning limit, located beyond 0.1 AU and in a nearly circular orbit. These planetary properties are difficult to reproduce from canonical planet formation and evolution models. For TOI-2529 b, we obtained the following orbital parameters: P = 64.5949^+0.0003_−0.0003 d, M_p =2.340^+0.197_−0.195 M_J, R_p = 1.030^+0.050_−0.050R_J and e = 0.021^+0.024_−0.015 , making this object a new example of a growing population of transiting warm giant planets.

Original language	English
Article number	A192
Number of pages	16
Journal	Astronomy and Astrophysics
Volume	683
DOIs	https://doi.org/10.1051/0004-6361/202348147
Publication status	Published - 20 Mar 2024

Bibliographical note

Acknowledgments:
The results reported herein benefited from collaborations and/or information exchange within NASA’s Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA’s Science Mission Directorate under Agreement No. 80NSSC21K0593 for the program “Alien Earths”. We thank the Swiss National Science Foundation (SNSF) and the Geneva University for their continuous support to the planet search programs. This work has been in particular carried out in the frame of the National Centre for Competence in Research PlanetS supported by the SNSF under grants 51NF40_182901 and 51NF40_205606 This publication made use of The Data & Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva dedicated to extrasolar planets data visualisation, exchange and analysis. DACE is a platform of NCCR PlanetS and is available at https://dace.unige.ch. This paper made use of data collected by the TESS mission and are publicly available from the Mikulski Archive for Space Telescopes (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 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 paper is based on data collected by the SPECULOOS-South Observatory at the ESO Paranal Observatory in Chile. 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 and Francqui Foundations, from the Belgian Scientific Research Foundation (F.R.S.-FNRS; grant n° T.0109.20), from the University of Liege, and from the ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. The Cambridge contribution is supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). The Birmingham contribution to SPECULOOS is in part funded by the European Union s Horizon 2020 research and innovation programme (grant’s agreement n° 803193/BEBOP), from the MERAC foundation, and from the Science and Technology Facilities Council (STFC; grant n° ST/S00193X/1, and ST/W000385/1). This publication benefits from the support of the French Community of Belgium in the context of the FRIA Doctoral Grant awarded to MT. M.L. acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. M.R.S. acknowledges support from the UK Science and Technology Facilities Council (ST/T000295/1) and support from the European Space Agency as an ESA Research Fellow. M.T.P. acknowledges the support of the Fondecyt-ANID Post-doctoral fellowship No. 3210253. T.T. acknowledges support by the DFG Research Unit FOR 2544 “Blue Planets around Red Stars” project No. KU 3625/2-1. T.T. further acknowledges support by the BNSF program “VIHREN-2021” project No. KP-06-DV/5. D.D. acknowledges support from the NASA Exoplanet Research Program grant 18-2XRP18_2-0136, and from the TESS Guest Investigator Program grants 80NSSC22K0185 and 80NSSC23K0769. J.C. acknowledges support of the South Carolina Space Grant Consortium. R.B. acknowledges support from FONDECYT project 11200751 and from project IC120009 “Millennium Institute of Astrophysics (MAS)” of the Millenium Science Initiative. M.U. gratefully acknowledges funding from the Research Foundation Flanders (FWO) by means of a junior postdoctoral fellowship (grant agreement No. 1247624N).

Keywords

techniques: photometric
techniques: radial velocities
planets and satellites: composition
planets and satellites: detection
planets and satellites: formation
planets and satellites: gaseous planets

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Jones, M. I., Reinarz, Y., Brahm, R., Pinto, M. T., Eberhardt, J., Rojas, F., Triaud, A. H. M. J., Gupta, A. F., Ziegler, C., Hobson, M. J., Jordán, A., Henning, T., Trifonov, T., Schlecker, M., Espinoza, N., Torres-Miranda, P., Sarkis, P., Ulmer-Moll, S., Lendl, M., ... Lissauer, J. J. (2024). A long-period transiting substellar companion in the super-Jupiters to brown dwarfs mass regime and a prototypical warm-Jupiter detected by TESS. Astronomy and Astrophysics, 683, Article A192. https://doi.org/10.1051/0004-6361/202348147

@article{8083f8aee93f442aa7ea7d88089a2686,

title = "A long-period transiting substellar companion in the super-Jupiters to brown dwarfs mass regime and a prototypical warm-Jupiter detected by TESS",

abstract = "We report on the confirmation and follow-up characterization of two long-period transiting substellar companions on low-eccentricity orbits around TIC 4672985 and TOI-2529, whose transit events were detected by the TESS space mission. Ground-based photometric and spectroscopic follow up from different facilities, confirmed the substellar nature of TIC 4672985 b, a massive gas giant, in the transition between the super-Jupiters and brown-dwarfs mass regime. From the joint analysis we derived the following orbital parameters: P = 69.0480+0.0004−0.0005 d, Mp = 12.74+1.01−1.01 MJ, Rp =1.026+0.065−0.067 RJ and e = 0.018+0.004−0.004 . In addition, the RV time series revealed a significant trend at the ∼ 350 m s−1 yr−1level, which is indicative of the presence of a massive outer companion in the system. TIC 4672985 b is a unique example of a transiting substellar companion with a mass above the deuterium-burning limit, located beyond 0.1 AU and in a nearly circular orbit. These planetary properties are difficult to reproduce from canonical planet formation and evolution models. For TOI-2529 b, we obtained the following orbital parameters: P = 64.5949+0.0003−0.0003 d, Mp =2.340+0.197−0.195 MJ, Rp = 1.030+0.050−0.050 RJ and e = 0.021+0.024−0.015 , making this object a new example of a growing population of transiting warm giant planets.",

keywords = "techniques: photometric, techniques: radial velocities, planets and satellites: composition, planets and satellites: detection, planets and satellites: formation, planets and satellites: gaseous planets",

author = "Jones, {Matias I.} and Yared Reinarz and Rafael Brahm and Pinto, {Marcelo Tala} and Jan Eberhardt and Felipe Rojas and Triaud, {Amaury H. M. J.} and Gupta, {Arvind F.} and Carl Ziegler and Hobson, {Melissa J.} and Andr{\'e}s Jord{\'a}n and Thomas Henning and Trifon Trifonov and Martin Schlecker and Nestor Espinoza and Pascal Torres-Miranda and Paula Sarkis and Sol{\`e}ne Ulmer-Moll and Monika Lendl and Murat Uzundag and Maximiliano Moyano and Katharine Hesse and Caldwell, {Douglas A.} and Avi Shporer and Lund, {Michael B.} and Jenkins, {Jon M.} and Sara Seager and Winn, {Joshua N.} and Ricker, {George R.} and Burke, {Christopher J.} and Pedro Figueira and Angelica Psaridi and Moulla, {Khaled Al} and Dany Mounzer and Standing, {Matthew R.} and Martin, {David V.} and Georgina Dransfield and Thomas Baycroft and Diana Dragomir and Gavin Boyle and Vincent Suc and Mann, {Andrew W.} and Mathilde Timmermans and Elsa Ducrot and Hooton, {Matthew J.} and Sebasti{\'a}n Z{\'u}{\~n}iga-Fern{\'a}ndez and Daniel Sebastian and Michael Gillon and Didier Queloz and Joe Carson and Lissauer, {Jack J.}",

note = "Acknowledgments: The results reported herein benefited from collaborations and/or information exchange within NASA{\textquoteright}s Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA{\textquoteright}s Science Mission Directorate under Agreement No. 80NSSC21K0593 for the program “Alien Earths”. We thank the Swiss National Science Foundation (SNSF) and the Geneva University for their continuous support to the planet search programs. This work has been in particular carried out in the frame of the National Centre for Competence in Research PlanetS supported by the SNSF under grants 51NF40_182901 and 51NF40_205606 This publication made use of The Data & Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva dedicated to extrasolar planets data visualisation, exchange and analysis. DACE is a platform of NCCR PlanetS and is available at https://dace.unige.ch. This paper made use of data collected by the TESS mission and are publicly available from the Mikulski Archive for Space Telescopes (MAST) operated by the Space Telescope Science Institute (STScI). Funding for the TESS mission is provided by NASA{\textquoteright}s Science Mission Directorate. We acknowledge the use of public TESS 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 paper is based on data collected by the SPECULOOS-South Observatory at the ESO Paranal Observatory in Chile. The ULiege s contribution to SPECULOOS has received funding from the European Research Council under the European Union{\textquoteright}s Seventh Framework Programme (FP/2007-2013) (grant Agreement nº 336480/SPECULOOS), from the Balzan Prize and Francqui Foundations, from the Belgian Scientific Research Foundation (F.R.S.-FNRS; grant n° T.0109.20), from the University of Liege, and from the ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. The Cambridge contribution is supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). The Birmingham contribution to SPECULOOS is in part funded by the European Union s Horizon 2020 research and innovation programme (grant{\textquoteright}s agreement n° 803193/BEBOP), from the MERAC foundation, and from the Science and Technology Facilities Council (STFC; grant n° ST/S00193X/1, and ST/W000385/1). This publication benefits from the support of the French Community of Belgium in the context of the FRIA Doctoral Grant awarded to MT. M.L. acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. M.R.S. acknowledges support from the UK Science and Technology Facilities Council (ST/T000295/1) and support from the European Space Agency as an ESA Research Fellow. M.T.P. acknowledges the support of the Fondecyt-ANID Post-doctoral fellowship No. 3210253. T.T. acknowledges support by the DFG Research Unit FOR 2544 “Blue Planets around Red Stars” project No. KU 3625/2-1. T.T. further acknowledges support by the BNSF program “VIHREN-2021” project No. KP-06-DV/5. D.D. acknowledges support from the NASA Exoplanet Research Program grant 18-2XRP18_2-0136, and from the TESS Guest Investigator Program grants 80NSSC22K0185 and 80NSSC23K0769. J.C. acknowledges support of the South Carolina Space Grant Consortium. R.B. acknowledges support from FONDECYT project 11200751 and from project IC120009 “Millennium Institute of Astrophysics (MAS)” of the Millenium Science Initiative. M.U. gratefully acknowledges funding from the Research Foundation Flanders (FWO) by means of a junior postdoctoral fellowship (grant agreement No. 1247624N).",

year = "2024",

month = mar,

day = "20",

doi = "10.1051/0004-6361/202348147",

language = "English",

volume = "683",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Jones, MI, Reinarz, Y, Brahm, R, Pinto, MT, Eberhardt, J, Rojas, F, Triaud, AHMJ, Gupta, AF, Ziegler, C, Hobson, MJ, Jordán, A, Henning, T, Trifonov, T, Schlecker, M, Espinoza, N, Torres-Miranda, P, Sarkis, P, Ulmer-Moll, S, Lendl, M, Uzundag, M, Moyano, M, Hesse, K, Caldwell, DA, Shporer, A, Lund, MB, Jenkins, JM, Seager, S, Winn, JN, Ricker, GR, Burke, CJ, Figueira, P, Psaridi, A, Moulla, KA, Mounzer, D, Standing, MR, Martin, DV, Dransfield, G, Baycroft, T, Dragomir, D, Boyle, G, Suc, V, Mann, AW, Timmermans, M, Ducrot, E, Hooton, MJ, Zúñiga-Fernández, S, Sebastian, D, Gillon, M, Queloz, D, Carson, J & Lissauer, JJ 2024, 'A long-period transiting substellar companion in the super-Jupiters to brown dwarfs mass regime and a prototypical warm-Jupiter detected by TESS', Astronomy and Astrophysics, vol. 683, A192. https://doi.org/10.1051/0004-6361/202348147

TY - JOUR

T1 - A long-period transiting substellar companion in the super-Jupiters to brown dwarfs mass regime and a prototypical warm-Jupiter detected by TESS

AU - Jones, Matias I.

AU - Reinarz, Yared

AU - Brahm, Rafael

AU - Pinto, Marcelo Tala

AU - Eberhardt, Jan

AU - Rojas, Felipe

AU - Triaud, Amaury H. M. J.

AU - Gupta, Arvind F.

AU - Ziegler, Carl

AU - Hobson, Melissa J.

AU - Jordán, Andrés

AU - Henning, Thomas

AU - Trifonov, Trifon

AU - Schlecker, Martin

AU - Espinoza, Nestor

AU - Torres-Miranda, Pascal

AU - Sarkis, Paula

AU - Ulmer-Moll, Solène

AU - Lendl, Monika

AU - Uzundag, Murat

AU - Moyano, Maximiliano

AU - Hesse, Katharine

AU - Caldwell, Douglas A.

AU - Shporer, Avi

AU - Lund, Michael B.

AU - Jenkins, Jon M.

AU - Seager, Sara

AU - Winn, Joshua N.

AU - Ricker, George R.

AU - Burke, Christopher J.

AU - Figueira, Pedro

AU - Psaridi, Angelica

AU - Moulla, Khaled Al

AU - Mounzer, Dany

AU - Standing, Matthew R.

AU - Martin, David V.

AU - Dransfield, Georgina

AU - Baycroft, Thomas

AU - Dragomir, Diana

AU - Boyle, Gavin

AU - Suc, Vincent

AU - Mann, Andrew W.

AU - Timmermans, Mathilde

AU - Ducrot, Elsa

AU - Hooton, Matthew J.

AU - Zúñiga-Fernández, Sebastián

AU - Sebastian, Daniel

AU - Gillon, Michael

AU - Queloz, Didier

AU - Carson, Joe

AU - Lissauer, Jack J.

N1 - Acknowledgments: The results reported herein benefited from collaborations and/or information exchange within NASA’s Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA’s Science Mission Directorate under Agreement No. 80NSSC21K0593 for the program “Alien Earths”. We thank the Swiss National Science Foundation (SNSF) and the Geneva University for their continuous support to the planet search programs. This work has been in particular carried out in the frame of the National Centre for Competence in Research PlanetS supported by the SNSF under grants 51NF40_182901 and 51NF40_205606 This publication made use of The Data & Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva dedicated to extrasolar planets data visualisation, exchange and analysis. DACE is a platform of NCCR PlanetS and is available at https://dace.unige.ch. This paper made use of data collected by the TESS mission and are publicly available from the Mikulski Archive for Space Telescopes (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 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 paper is based on data collected by the SPECULOOS-South Observatory at the ESO Paranal Observatory in Chile. 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 and Francqui Foundations, from the Belgian Scientific Research Foundation (F.R.S.-FNRS; grant n° T.0109.20), from the University of Liege, and from the ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. The Cambridge contribution is supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). The Birmingham contribution to SPECULOOS is in part funded by the European Union s Horizon 2020 research and innovation programme (grant’s agreement n° 803193/BEBOP), from the MERAC foundation, and from the Science and Technology Facilities Council (STFC; grant n° ST/S00193X/1, and ST/W000385/1). This publication benefits from the support of the French Community of Belgium in the context of the FRIA Doctoral Grant awarded to MT. M.L. acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. M.R.S. acknowledges support from the UK Science and Technology Facilities Council (ST/T000295/1) and support from the European Space Agency as an ESA Research Fellow. M.T.P. acknowledges the support of the Fondecyt-ANID Post-doctoral fellowship No. 3210253. T.T. acknowledges support by the DFG Research Unit FOR 2544 “Blue Planets around Red Stars” project No. KU 3625/2-1. T.T. further acknowledges support by the BNSF program “VIHREN-2021” project No. KP-06-DV/5. D.D. acknowledges support from the NASA Exoplanet Research Program grant 18-2XRP18_2-0136, and from the TESS Guest Investigator Program grants 80NSSC22K0185 and 80NSSC23K0769. J.C. acknowledges support of the South Carolina Space Grant Consortium. R.B. acknowledges support from FONDECYT project 11200751 and from project IC120009 “Millennium Institute of Astrophysics (MAS)” of the Millenium Science Initiative. M.U. gratefully acknowledges funding from the Research Foundation Flanders (FWO) by means of a junior postdoctoral fellowship (grant agreement No. 1247624N).

PY - 2024/3/20

Y1 - 2024/3/20

N2 - We report on the confirmation and follow-up characterization of two long-period transiting substellar companions on low-eccentricity orbits around TIC 4672985 and TOI-2529, whose transit events were detected by the TESS space mission. Ground-based photometric and spectroscopic follow up from different facilities, confirmed the substellar nature of TIC 4672985 b, a massive gas giant, in the transition between the super-Jupiters and brown-dwarfs mass regime. From the joint analysis we derived the following orbital parameters: P = 69.0480+0.0004−0.0005 d, Mp = 12.74+1.01−1.01 MJ, Rp =1.026+0.065−0.067 RJ and e = 0.018+0.004−0.004 . In addition, the RV time series revealed a significant trend at the ∼ 350 m s−1 yr−1level, which is indicative of the presence of a massive outer companion in the system. TIC 4672985 b is a unique example of a transiting substellar companion with a mass above the deuterium-burning limit, located beyond 0.1 AU and in a nearly circular orbit. These planetary properties are difficult to reproduce from canonical planet formation and evolution models. For TOI-2529 b, we obtained the following orbital parameters: P = 64.5949+0.0003−0.0003 d, Mp =2.340+0.197−0.195 MJ, Rp = 1.030+0.050−0.050 RJ and e = 0.021+0.024−0.015 , making this object a new example of a growing population of transiting warm giant planets.

AB - We report on the confirmation and follow-up characterization of two long-period transiting substellar companions on low-eccentricity orbits around TIC 4672985 and TOI-2529, whose transit events were detected by the TESS space mission. Ground-based photometric and spectroscopic follow up from different facilities, confirmed the substellar nature of TIC 4672985 b, a massive gas giant, in the transition between the super-Jupiters and brown-dwarfs mass regime. From the joint analysis we derived the following orbital parameters: P = 69.0480+0.0004−0.0005 d, Mp = 12.74+1.01−1.01 MJ, Rp =1.026+0.065−0.067 RJ and e = 0.018+0.004−0.004 . In addition, the RV time series revealed a significant trend at the ∼ 350 m s−1 yr−1level, which is indicative of the presence of a massive outer companion in the system. TIC 4672985 b is a unique example of a transiting substellar companion with a mass above the deuterium-burning limit, located beyond 0.1 AU and in a nearly circular orbit. These planetary properties are difficult to reproduce from canonical planet formation and evolution models. For TOI-2529 b, we obtained the following orbital parameters: P = 64.5949+0.0003−0.0003 d, Mp =2.340+0.197−0.195 MJ, Rp = 1.030+0.050−0.050 RJ and e = 0.021+0.024−0.015 , making this object a new example of a growing population of transiting warm giant planets.

KW - techniques: photometric

KW - techniques: radial velocities

KW - planets and satellites: composition

KW - planets and satellites: detection

KW - planets and satellites: formation

KW - planets and satellites: gaseous planets

U2 - 10.1051/0004-6361/202348147

DO - 10.1051/0004-6361/202348147

M3 - Article

SN - 0004-6361

VL - 683

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A192

ER -

A long-period transiting substellar companion in the super-Jupiters to brown dwarfs mass regime and a prototypical warm-Jupiter detected by TESS

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Bibliographical note

Keywords

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