Precise mass and radius determination for two new and one known Neptune-sized planets around G Dwarf hosts

Abstract As part of the KESPRINT collaboration, we present the discovery and characterization of three exoplanets in the sub-Neptune to super-Neptune regime, spanning key regions of the exo-Neptunian landscape. TOI-1472 c and TOI-1648 b are newly discovered sub-Neptunes, while TOI-1472 b is a previously known super-Neptune for which we provide an improved mass measurement. These planets have orbital periods of 6–15 days and radii of 2.5–4.1 R⊕, probing regions where planet formation and atmospheric evolution remain poorly understood. We combine TESS transit photometry with ground-based radial velocities to determine precise masses, radii, and orbital properties. TOI-1472 b has a mass of $18.0^{+0.84}_{-0.85}$ M⊕ and a radius of 4.06 ± 0.10 R⊕, TOI-1472 c has a mass of $21.1^{+0.96}_{-0.99}$ M⊕ and a radius of 3.33 ± 0.08 R⊕, and TOI-1648 b has a mass of $7.4^{+1.1}_{-1.3}$ M⊕ and a radius of $2.54^{+0.14}_{-0.12}$ R⊕. The planets exhibit a range of eccentricities (0.041–0.178), indicating diverse evolutionary histories. TOI-1648 b, with a high Transmission Spectroscopy Metric (TSM ∼59), is a promising target for atmospheric characterization. Together, these three planets provide precise constraints on the structure, composition, and dynamical evolution of small to intermediate-sized exoplanets, enriching our understanding of the exo-Neptunian landscape.

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Journal
Monthly Notices of the Royal Astronomical Society
Published
2025-11-07
DOI
https://doi.org/10.1093/mnras/staf1958
Primary Topic
Astro and Planetary Science
Type
article
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article

Precise mass and radius determination for two new and one known Neptune-sized planets around G Dwarf hosts

J. Lillo-Box, H. J. Deeg, Pau Bosch-Cabot, R. Luque et al.
Monthly Notices of the Royal Astronomical Society
Astro and Planetary Science
article

Precise mass and radius determination for two new and one known Neptune-sized planets around G Dwarf hosts

J. Lillo-Box, H. J. Deeg, Pau Bosch-Cabot, R. Luque, Emil Knudstrup, T. Masseron, Florence Libotte, Kiyoe Kawauchi, Bob Massey, F. Murgas, Akihiko Fukui, Ε. Πάλλη, D. Gandolfi, Michael B. Lund, Andrew W. Boyle, Matteo Brogi, Karen A. Collins, Steve B. Howell, G. Lacedelli, J. Korth, J. S. Jenkins, I. Carleo, A. Castro-González, Boris S. Safonov, Seth Redfield, Richard P. Schwarz, A. P. Hatzes, C. M. Persson, John H. Livingston, David A. Baker, S. Messina, J. Orell-Miquel, Catherine A. Clark, P. Eggenberger, Avi Shporer, R. M. González Delgado, Eduardo Lorenzo Martín Guerrero de Escalante, Elise Furlan, Dawid Jankowski, José I Vines, C. Hellier, P. Guerra, Emily Wong, David R. Ciardi, Krzysztof Goździewski, Norio Narita, V. Bourrier, M. Stangret, Núria Casasayas Barris, Keivan G. Stassun, G. Nowak, Allyson Bieryla, Edward J Michaels, D. R. Alves, Giuseppe Morello, Cristilyn N. Watkins, S. González, Stavros Chairetas, Hannu Parvianien
article en

Abstract

Abstract As part of the KESPRINT collaboration, we present the discovery and characterization of three exoplanets in the sub-Neptune to super-Neptune regime, spanning key regions of the exo-Neptunian landscape. TOI-1472 c and TOI-1648 b are newly discovered sub-Neptunes, while TOI-1472 b is a previously known super-Neptune for which we provide an improved mass measurement. These planets have orbital periods of 6–15 days and radii of 2.5–4.1 R⊕, probing regions where planet formation and atmospheric evolution remain poorly understood. We combine TESS transit photometry with ground-based radial velocities to determine precise masses, radii, and orbital properties. TOI-1472 b has a mass of $18.0^{+0.84}_{-0.85}$ M⊕ and a radius of 4.06 ± 0.10 R⊕, TOI-1472 c has a mass of $21.1^{+0.96}_{-0.99}$ M⊕ and a radius of 3.33 ± 0.08 R⊕, and TOI-1648 b has a mass of $7.4^{+1.1}_{-1.3}$ M⊕ and a radius of $2.54^{+0.14}_{-0.12}$ R⊕. The planets exhibit a range of eccentricities (0.041–0.178), indicating diverse evolutionary histories. TOI-1648 b, with a high Transmission Spectroscopy Metric (TSM ∼59), is a promising target for atmospheric characterization. Together, these three planets provide precise constraints on the structure, composition, and dynamical evolution of small to intermediate-sized exoplanets, enriching our understanding of the exo-Neptunian landscape.

Monthly Notices of the Royal Astronomical Society
Wesleyan University (US), Universidad de Santiago de Chile (CL), University of North Carolina at Chapel Hill (US), California Institute of Technology (US), Ames Research Center (US), Ritsumeikan University (JP), Universidad de La Laguna (ES), Royal Belgian Institute for Space Aeronomy (BE), The Graduate University for Advanced Studies, SOKENDAI (JP), Vanderbilt University (US), Aarhus University (DK), Montana State University (US), Universitat de Girona (ES), NASA Exoplanet Science Institute (US), Universidad Católica del Norte (CL), Nicolaus Copernicus University (PL), TMT Observatory (US), Millennium Institute of Astrophysics (CL), Osservatorio Astrofisico di Torino (IT), Astrobiology Center (JP), Institute of Astronomy (RU), Osservatorio Astrofisico di Catania (IT), Center for Astrophysics Harvard & Smithsonian (US), Hospital de Sabadell (ES), Osservatorio Astronomico di Palermo (IT), Centro de Astrobiología (ES), Instituto de Astrofísica de Canarias (ES), Bellatrix Astronomical Observatory (IT), Tokyo Metropolitan Komaba High School (JP), Astronomy and Space (AU), Thüringer Landessternwarte Tautenburg (DE), Astronomical Observatory (RS), Instituto de Astrofísica de Andalucía (ES), National Astronomical Observatory of Japan (JP), Lehmann Eye Center (US), University of Turin (IT), Keele University (GB), Massachusetts Institute of Technology (US), Chalmers University of Technology (SE), University of Chile (CL), The University of Tokyo (JP), The University of Texas at Austin (US), Universidad Diego Portales (CL)
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