TESS and HARPS-N unveil two planets transiting TOI-1453

Context. The TESS mission is searching for transiting planets over the entire sky, including two continuous viewing zones. Data from the continuous viewing zones span a long time baseline and offer ideal conditions for precise planet radius estimations, enabling the community to prepare for the PLATO mission. Aims. We report on the validation and characterisation of two transiting planets around TOI-1453, a K-dwarf star in the TESS northern continuous viewing zone. Methods. In addition to the TESS data, we used ground-based photometric, spectroscopic, and high-resolution imaging follow-up observations to validate the two planets. We obtained 100 HARPS-N high-resolution spectra over two seasons and used them together with the TESS light curve to constrain the mass, radius, and orbit of each planet. Results. TOI-1453 b is a super-Earth with an orbital period of P b =4.314 days, a radius of R b =1.17±0.06 R ⊕ , and a mass lower than 2.32 M ⊕ (99%). TOI-1453 c is a sub-Neptune with a period of P c =6.589 days, radius of R c =2.22±0.09 R ⊕ , and mass of M c =2.95 −0.84 +0.83 M ⊕ . The two planets orbit TOI-1453 with a period ratio close to 3/2, although they are not in a mean motion resonance (MMR) state. We did not detect any transit timing variations in our attempt to further constrain the planet masses. TOI-1453 c has a very low bulk density and is one of the least massive sub-Neptunes discovered to date. It is compatible with having either a water-rich composition or a rocky core surrounded by a thick H/He atmosphere. However, we set constraints on the water mass fraction in the envelope according to either a water-rich or water-poor formation scenario. The star TOI-1453 belongs to the Galactic thin disc based on Gaia kinematics and has a sub-solar metallicity. This system is orbited by a fainter stellar companion at a projected distance of ∼150 AU, classifying TOI-1453 b and c of S-type planets. These various planetary and stellar characteristics make TOI-1453 a valuable system for understanding the origin of super-Earths and sub-Neptunes.

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Journal
Astronomy and Astrophysics
Published
2025-03-07
DOI
https://doi.org/10.1051/0004-6361/202452969
Citations
1
Primary Topic
Astro and Planetary Science
Type
article
Field-Weighted Citation Impact
1.15

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article

TESS and HARPS-N unveil two planets transiting TOI-1453

J. Lillo-Box, S. Udry, K.A. Collins, D.R. Ciardi et al.
1 citations
Astronomy and Astrophysics
Astro and Planetary Science
1.15
article

TESS and HARPS-N unveil two planets transiting TOI-1453

J. Lillo-Box, S. Udry, K.A. Collins, D.R. Ciardi, J. N. Winn, M. Pinamonti, F. Murgas, Cristilyn N. Watkins, S.N. Quinn, J.A. Egger, A. Vanderburg, Alessandro Sozzetti, S. Seager, C. Ziegler, M. Damasso, R.P. Schwarz, S. B. Howell, W. Boschin, Pablo Lewin, Lars A. Buchhave, A. Leleu, M. Cretignier, G. Andreuzzi, X. Dumusque, David Baker, D. W. Latham, A. Fukui, J.M. Jenkins, N. Narita, E. Poretti, E.B. Ting, M. López-Morales, R. D. Haywood, M. Pedani, A. Martinez Fiorenzano, M. Stalport, A. Mortier, L. Malavolta, Ana Maria Silva, L. Di Fabrizio
article en
1 citations

Abstract

Context. The TESS mission is searching for transiting planets over the entire sky, including two continuous viewing zones. Data from the continuous viewing zones span a long time baseline and offer ideal conditions for precise planet radius estimations, enabling the community to prepare for the PLATO mission. Aims. We report on the validation and characterisation of two transiting planets around TOI-1453, a K-dwarf star in the TESS northern continuous viewing zone. Methods. In addition to the TESS data, we used ground-based photometric, spectroscopic, and high-resolution imaging follow-up observations to validate the two planets. We obtained 100 HARPS-N high-resolution spectra over two seasons and used them together with the TESS light curve to constrain the mass, radius, and orbit of each planet. Results. TOI-1453 b is a super-Earth with an orbital period of P b =4.314 days, a radius of R b =1.17±0.06 R ⊕ , and a mass lower than 2.32 M ⊕ (99%). TOI-1453 c is a sub-Neptune with a period of P c =6.589 days, radius of R c =2.22±0.09 R ⊕ , and mass of M c =2.95 −0.84 +0.83 M ⊕ . The two planets orbit TOI-1453 with a period ratio close to 3/2, although they are not in a mean motion resonance (MMR) state. We did not detect any transit timing variations in our attempt to further constrain the planet masses. TOI-1453 c has a very low bulk density and is one of the least massive sub-Neptunes discovered to date. It is compatible with having either a water-rich composition or a rocky core surrounded by a thick H/He atmosphere. However, we set constraints on the water mass fraction in the envelope according to either a water-rich or water-poor formation scenario. The star TOI-1453 belongs to the Galactic thin disc based on Gaia kinematics and has a sub-solar metallicity. This system is orbited by a fainter stellar companion at a projected distance of ∼150 AU, classifying TOI-1453 b and c of S-type planets. These various planetary and stellar characteristics make TOI-1453 a valuable system for understanding the origin of super-Earths and sub-Neptunes.

Astronomy and AstrophysicsVol. 696
University of Geneva (CH), University of Bern (CH), Austin College (US), California Institute of Technology (US), Ames Research Center (US), University of Padua (IT), University of Liège (BE), Universidad de La Laguna (ES), Universidade do Porto (PT), Princeton University (US), Stephen F. Austin State University (US), University of Exeter (GB), NASA Exoplanet Science Institute (US), Astronomical Observatory of Rome (IT), University of Oxford (GB), Institute of Astrophysics and Space Sciences (PT), Osservatorio Astrofisico di Torino (IT), Center for Astrophysics Harvard & Smithsonian (US), Centro de Astrobiología (ES), Instituto de Astrofísica de Canarias (ES), Tokyo Metropolitan Komaba High School (JP), Osservatorio Astronomico di Padova (IT), Telescopio Nazionale Galileo (ES), American Institute of Aeronautics and Astronautics (US), Massachusetts Institute of Technology (US), The University of Tokyo (JP), University of Birmingham (GB), National Institute for Astrophysics (IT), Technical University of Denmark (DK)
National Science Foundation, Smithsonian Institution, National Aeronautics and Space Administration, California Institute of Technology, Harvard University, Space Telescope Science Institute, UK Research and Innovation, European Space Agency, Scottish Universities Physics Alliance, University of St Andrews, European Commission, Queen's University Belfast, Schweizerischer Nationalfonds zur Förderung der Wissenschaftlichen Forschung, Belgian Federal Science Policy Office, Queen's University, Ministry of Science, ICT and Future Planning, Istituto Nazionale di Astrofisica, National Astronomical Observatory of Japan, Université de Genève, Ames Research Center, Smithsonian Astrophysical Observatory, Science Mission Directorate, Science and Technology Facilities Council, Japan Society for the Promotion of Science, Precursory Research for Embryonic Science and Technology
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Astro and Planetary Science
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