Evidence for transit-timing variations of the 11 Myr exoplanet TOI-1227 b

J.M. Almenara; X. Bonfils; T. Guillot; M. Timmermans; R.F. Díaz; J. Venturini; A.C. Petit; T. Forveille; O. Suarez; D. Mekarnia; A.H.M.J. Triaud; L. Abe; P. Bendjoya; F. Bouchy; J. Bouvier; L. Delrez; G. Dransfield; E. Ducrot; M. Gillon; M.J. Hooton; E. Jehin; A.W. Mann; R. Mardling; F. Murgas; A. Leleu; M. Lendl; D. Queloz; S. Seager; J. Winn; S. Zuñiga Fernández

doi:10.1051/0004-6361/202348492

Evidence for transit-timing variations of the 11 Myr exoplanet TOI-1227 b

J.M. Almenara, X. Bonfils, T. Guillot, M. Timmermans, R.F. Díaz, J. Venturini, A.C. Petit, T. Forveille, O. Suarez, D. Mekarnia, A.H.M.J. Triaud, L. Abe, P. Bendjoya, F. Bouchy, J. Bouvier, L. Delrez, G. Dransfield, E. Ducrot, M. Gillon, M.J. HootonE. Jehin, A.W. Mann, R. Mardling, F. Murgas, A. Leleu, M. Lendl, D. Queloz, S. Seager, J. Winn, S. Zuñiga Fernández

Physics and Astronomy

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Abstract

TOI-1227 b is an 11 Myr old validated transiting planet in the middle of its contraction phase, with a current radius of 0.85 R_J. It orbits a low-mass pre-main sequence star (0.170 M_⊙, 0.56 R_⊙) every 27.4 days. The magnetic activity of its young host star induces radial velocity jitter and prevents good measurements of the planetary mass. We gathered additional transit observations of TOI-1227 b with space- and ground-based telescopes, and we detected highly significant transit-timing variations (TTVs). Their amplitude is about 40 minutes and their dominant timescale is longer than 3.7 years. Their most probable origin is dynamical interactions with additional planets in the system. We modeled the TTVs with inner and outer perturbers near first and second order resonances; several orbital configurations provide an acceptable fit. More data are needed to determine the actual orbital configuration and eventually measure the planetary masses. These TTVs and an updated transit chromaticity analysis reinforce the evidence that TOI-1227 b is a planet.

Original language	English
Article number	A96
Number of pages	12
Journal	Astronomy and Astrophysics
Volume	683
DOIs	https://doi.org/10.1051/0004-6361/202348492
Publication status	Published - 12 Mar 2024

Bibliographical note

Acknowledgments:
We are grateful to the ESO/La Silla staff for their continuous support of ExTrA and to the wintering staff at Concordia Station in Antarctica who look after ASTEP during the long austral winter night. We acknowledge funding from the European Research Council under the ERC Grant Agreement n. 337591-ExTrA. This paper includes data collected with the TESS mission, obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the TESS mission is provided by the NASA Explorer Program. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5_26555. We acknowledge the use of public TESS data from the 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 work makes use of observations from the Las Cumbres Observatory global telescope network. Simulations in this paper made use of the REBOUND code which can be downloaded freely at http://github.com/hannorein/rebound. We thank the Swiss National Science Foundation (SNSF) and the Geneva University for their continuous support to our planet search programs. 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. 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 no. T.0109.20), from the University of Liège, 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 research is in part funded by the European Union’s Horizon 2020 research and innovation programme (grant’s agreement no. 803193/BEBOP), from the MERAC foundation, and from the Science and Technology Facilities Council (STFC; grant no. ST/S00193X/1, and ST/W000385/1). This is also based on data collected by the TRAPPIST-South telescope at the ESO La Silla Observatory. TRAPPIST is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, FNRS) under the grant FRFC 2.5.594.09.F, with the participation of the Swiss National Science Fundation (SNF). E.J. is a Senior Research Scientist at FNRS. This paper uses data obtained with the ASTEP telescope, at Concordia Station in Antarctica. ASTEP benefited from the support of the French and Italian polar agencies IPEV and PNRA in the framework of the Concordia station program, from OCA, INSU, Idex UCAJEDI (ANR- 15-IDEX-01) and ESA through the Science Faculty of the European Space Research and Technology Centre (ESTEC). The Birmingham contribution to ASTEP is supported by the European Union’s Horizon 2020 research and innovation programme (grant’s agreement no. 803193/BEBOP), and from the Science and Technology Facilities Council (STFC; grant no. ST/S00193X/1, and ST/W002582/1). This research has made use of the Spanish Virtual Observatory (https://svo. cab.inta-csic.es) project funded by MCIN/AEI/10.13039/501100011033/ through grant PID2020-112949GB-I00. This work was supported by the "Programme National de Physique Stellaire" (PNPS) and “Programme National de Planétology” of CNRS/INSU co-funded by CEA and CNES. M.L. acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. J.V. acknowledges support from the Swiss National Science Foundation (SNSF) under grant PZ00P2_208945.

Keywords

techniques: photometric
stars: individual: TOI-1227
stars: low-mass
planetary systems
stars: pre-main sequence

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Almenara, J. M., Bonfils, X., Guillot, T., Timmermans, M., Díaz, R. F., Venturini, J., Petit, A. C., Forveille, T., Suarez, O., Mekarnia, D., Triaud, A. H. M. J., Abe, L., Bendjoya, P., Bouchy, F., Bouvier, J., Delrez, L., Dransfield, G., Ducrot, E., Gillon, M., ... Zuñiga Fernández, S. (2024). Evidence for transit-timing variations of the 11 Myr exoplanet TOI-1227 b. Astronomy and Astrophysics, 683, Article A96. https://doi.org/10.1051/0004-6361/202348492

@article{fe2bf501148a4d61be82273c4ae95577,

title = "Evidence for transit-timing variations of the 11 Myr exoplanet TOI-1227 b",

abstract = "TOI-1227 b is an 11 Myr old validated transiting planet in the middle of its contraction phase, with a current radius of 0.85 RJ. It orbits a low-mass pre-main sequence star (0.170 M⊙, 0.56 R⊙) every 27.4 days. The magnetic activity of its young host star induces radial velocity jitter and prevents good measurements of the planetary mass. We gathered additional transit observations of TOI-1227 b with space- and ground-based telescopes, and we detected highly significant transit-timing variations (TTVs). Their amplitude is about 40 minutes and their dominant timescale is longer than 3.7 years. Their most probable origin is dynamical interactions with additional planets in the system. We modeled the TTVs with inner and outer perturbers near first and second order resonances; several orbital configurations provide an acceptable fit. More data are needed to determine the actual orbital configuration and eventually measure the planetary masses. These TTVs and an updated transit chromaticity analysis reinforce the evidence that TOI-1227 b is a planet.",

keywords = "techniques: photometric, stars: individual: TOI-1227, stars: low-mass, planetary systems, stars: pre-main sequence",

author = "J.M. Almenara and X. Bonfils and T. Guillot and M. Timmermans and R.F. D{\'i}az and J. Venturini and A.C. Petit and T. Forveille and O. Suarez and D. Mekarnia and A.H.M.J. Triaud and L. Abe and P. Bendjoya and F. Bouchy and J. Bouvier and L. Delrez and G. Dransfield and E. Ducrot and M. Gillon and M.J. Hooton and E. Jehin and A.W. Mann and R. Mardling and F. Murgas and A. Leleu and M. Lendl and D. Queloz and S. Seager and J. Winn and {Zu{\~n}iga Fern{\'a}ndez}, S.",

note = "Acknowledgments: We are grateful to the ESO/La Silla staff for their continuous support of ExTrA and to the wintering staff at Concordia Station in Antarctica who look after ASTEP during the long austral winter night. We acknowledge funding from the European Research Council under the ERC Grant Agreement n. 337591-ExTrA. This paper includes data collected with the TESS mission, obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the TESS mission is provided by the NASA Explorer Program. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5_26555. We acknowledge the use of public TESS data from the 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 work makes use of observations from the Las Cumbres Observatory global telescope network. Simulations in this paper made use of the REBOUND code which can be downloaded freely at http://github.com/hannorein/rebound. We thank the Swiss National Science Foundation (SNSF) and the Geneva University for their continuous support to our planet search programs. 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. This paper is based on data collected by the SPECULOOS-South Observatory at the ESO Paranal Observatory in Chile. The ULiege{\textquoteright}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 no. T.0109.20), from the University of Li{\`e}ge, 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 research is in part funded by the European Union{\textquoteright}s Horizon 2020 research and innovation programme (grant{\textquoteright}s agreement no. 803193/BEBOP), from the MERAC foundation, and from the Science and Technology Facilities Council (STFC; grant no. ST/S00193X/1, and ST/W000385/1). This is also based on data collected by the TRAPPIST-South telescope at the ESO La Silla Observatory. TRAPPIST is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, FNRS) under the grant FRFC 2.5.594.09.F, with the participation of the Swiss National Science Fundation (SNF). E.J. is a Senior Research Scientist at FNRS. This paper uses data obtained with the ASTEP telescope, at Concordia Station in Antarctica. ASTEP benefited from the support of the French and Italian polar agencies IPEV and PNRA in the framework of the Concordia station program, from OCA, INSU, Idex UCAJEDI (ANR- 15-IDEX-01) and ESA through the Science Faculty of the European Space Research and Technology Centre (ESTEC). The Birmingham contribution to ASTEP is supported by the European Union{\textquoteright}s Horizon 2020 research and innovation programme (grant{\textquoteright}s agreement no. 803193/BEBOP), and from the Science and Technology Facilities Council (STFC; grant no. ST/S00193X/1, and ST/W002582/1). This research has made use of the Spanish Virtual Observatory (https://svo. cab.inta-csic.es) project funded by MCIN/AEI/10.13039/501100011033/ through grant PID2020-112949GB-I00. This work was supported by the {"}Programme National de Physique Stellaire{"} (PNPS) and “Programme National de Plan{\'e}tology” of CNRS/INSU co-funded by CEA and CNES. M.L. acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. J.V. acknowledges support from the Swiss National Science Foundation (SNSF) under grant PZ00P2_208945.",

year = "2024",

month = mar,

day = "12",

doi = "10.1051/0004-6361/202348492",

language = "English",

volume = "683",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Almenara, JM, Bonfils, X, Guillot, T, Timmermans, M, Díaz, RF, Venturini, J, Petit, AC, Forveille, T, Suarez, O, Mekarnia, D, Triaud, AHMJ, Abe, L, Bendjoya, P, Bouchy, F, Bouvier, J, Delrez, L, Dransfield, G, Ducrot, E, Gillon, M, Hooton, MJ, Jehin, E, Mann, AW, Mardling, R, Murgas, F, Leleu, A, Lendl, M, Queloz, D, Seager, S, Winn, J & Zuñiga Fernández, S 2024, 'Evidence for transit-timing variations of the 11 Myr exoplanet TOI-1227 b', Astronomy and Astrophysics, vol. 683, A96. https://doi.org/10.1051/0004-6361/202348492

TY - JOUR

T1 - Evidence for transit-timing variations of the 11 Myr exoplanet TOI-1227 b

AU - Almenara, J.M.

AU - Bonfils, X.

AU - Guillot, T.

AU - Timmermans, M.

AU - Díaz, R.F.

AU - Venturini, J.

AU - Petit, A.C.

AU - Forveille, T.

AU - Suarez, O.

AU - Mekarnia, D.

AU - Triaud, A.H.M.J.

AU - Abe, L.

AU - Bendjoya, P.

AU - Bouchy, F.

AU - Bouvier, J.

AU - Delrez, L.

AU - Dransfield, G.

AU - Ducrot, E.

AU - Gillon, M.

AU - Hooton, M.J.

AU - Jehin, E.

AU - Mann, A.W.

AU - Mardling, R.

AU - Murgas, F.

AU - Leleu, A.

AU - Lendl, M.

AU - Queloz, D.

AU - Seager, S.

AU - Winn, J.

AU - Zuñiga Fernández, S.

N1 - Acknowledgments: We are grateful to the ESO/La Silla staff for their continuous support of ExTrA and to the wintering staff at Concordia Station in Antarctica who look after ASTEP during the long austral winter night. We acknowledge funding from the European Research Council under the ERC Grant Agreement n. 337591-ExTrA. This paper includes data collected with the TESS mission, obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the TESS mission is provided by the NASA Explorer Program. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5_26555. We acknowledge the use of public TESS data from the 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 work makes use of observations from the Las Cumbres Observatory global telescope network. Simulations in this paper made use of the REBOUND code which can be downloaded freely at http://github.com/hannorein/rebound. We thank the Swiss National Science Foundation (SNSF) and the Geneva University for their continuous support to our planet search programs. 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. 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 no. T.0109.20), from the University of Liège, 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 research is in part funded by the European Union’s Horizon 2020 research and innovation programme (grant’s agreement no. 803193/BEBOP), from the MERAC foundation, and from the Science and Technology Facilities Council (STFC; grant no. ST/S00193X/1, and ST/W000385/1). This is also based on data collected by the TRAPPIST-South telescope at the ESO La Silla Observatory. TRAPPIST is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, FNRS) under the grant FRFC 2.5.594.09.F, with the participation of the Swiss National Science Fundation (SNF). E.J. is a Senior Research Scientist at FNRS. This paper uses data obtained with the ASTEP telescope, at Concordia Station in Antarctica. ASTEP benefited from the support of the French and Italian polar agencies IPEV and PNRA in the framework of the Concordia station program, from OCA, INSU, Idex UCAJEDI (ANR- 15-IDEX-01) and ESA through the Science Faculty of the European Space Research and Technology Centre (ESTEC). The Birmingham contribution to ASTEP is supported by the European Union’s Horizon 2020 research and innovation programme (grant’s agreement no. 803193/BEBOP), and from the Science and Technology Facilities Council (STFC; grant no. ST/S00193X/1, and ST/W002582/1). This research has made use of the Spanish Virtual Observatory (https://svo. cab.inta-csic.es) project funded by MCIN/AEI/10.13039/501100011033/ through grant PID2020-112949GB-I00. This work was supported by the "Programme National de Physique Stellaire" (PNPS) and “Programme National de Planétology” of CNRS/INSU co-funded by CEA and CNES. M.L. acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. J.V. acknowledges support from the Swiss National Science Foundation (SNSF) under grant PZ00P2_208945.

PY - 2024/3/12

Y1 - 2024/3/12

N2 - TOI-1227 b is an 11 Myr old validated transiting planet in the middle of its contraction phase, with a current radius of 0.85 RJ. It orbits a low-mass pre-main sequence star (0.170 M⊙, 0.56 R⊙) every 27.4 days. The magnetic activity of its young host star induces radial velocity jitter and prevents good measurements of the planetary mass. We gathered additional transit observations of TOI-1227 b with space- and ground-based telescopes, and we detected highly significant transit-timing variations (TTVs). Their amplitude is about 40 minutes and their dominant timescale is longer than 3.7 years. Their most probable origin is dynamical interactions with additional planets in the system. We modeled the TTVs with inner and outer perturbers near first and second order resonances; several orbital configurations provide an acceptable fit. More data are needed to determine the actual orbital configuration and eventually measure the planetary masses. These TTVs and an updated transit chromaticity analysis reinforce the evidence that TOI-1227 b is a planet.

AB - TOI-1227 b is an 11 Myr old validated transiting planet in the middle of its contraction phase, with a current radius of 0.85 RJ. It orbits a low-mass pre-main sequence star (0.170 M⊙, 0.56 R⊙) every 27.4 days. The magnetic activity of its young host star induces radial velocity jitter and prevents good measurements of the planetary mass. We gathered additional transit observations of TOI-1227 b with space- and ground-based telescopes, and we detected highly significant transit-timing variations (TTVs). Their amplitude is about 40 minutes and their dominant timescale is longer than 3.7 years. Their most probable origin is dynamical interactions with additional planets in the system. We modeled the TTVs with inner and outer perturbers near first and second order resonances; several orbital configurations provide an acceptable fit. More data are needed to determine the actual orbital configuration and eventually measure the planetary masses. These TTVs and an updated transit chromaticity analysis reinforce the evidence that TOI-1227 b is a planet.

KW - techniques: photometric

KW - stars: individual: TOI-1227

KW - stars: low-mass

KW - planetary systems

KW - stars: pre-main sequence

U2 - 10.1051/0004-6361/202348492

DO - 10.1051/0004-6361/202348492

M3 - Article

SN - 0004-6361

VL - 683

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A96

ER -

Evidence for transit-timing variations of the 11 Myr exoplanet TOI-1227 b

Abstract

Bibliographical note

Keywords

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