TOI-7166 b: a habitable zone mini-Neptune planet around a nearby low-mass star

ABSTRACT We present the discovery and validation of TOI-7166 b, a $2.01 \pm 0.05\,\mathrm{ R}_{\oplus }$ planet orbiting a nearby low-mass star. We validated the planet by combining Transiting Exoplanet Survey Satellite and multicolour high-precision photometric observations from ground-based telescopes, together with spectroscopic data, high-contrast imaging, archival images, and statistical arguments. The host star is an M4-type dwarf at a distance of $\sim$35 pc from the Sun. It has a mass and a radius of $M_\star = 0.190 \pm 0.004\, \mathrm{ M}_\odot$ and $R_\star =0.222 \pm 0.005\, \mathrm{ R}_\odot$, respectively. TOI-7166 b has an orbital period of 12.9 d, which places it close to the inner edge of the Habitable Zone of its host star, receiving an insolation flux of $S_\mathrm{ p}=1.07\pm 0.08\, \mathrm{ S}_{\oplus }$ and an equilibrium temperature of $T_{\rm eq}~= 249\pm 5$ K (assuming a null Bond albedo). The brightness of the host star makes TOI-7166 a suitable target for radial velocity follow-up to measure the planetary mass and bulk density. Moreover, the physical parameters of the system including the infrared brightness ($K_{\rm mag} = 10.6$) of the star and the planet-to-star radius ratio ($0.0823 \pm 0.0012$) make TOI-7166 b an exquisite target for transmission spectroscopic observations with the James Webb Space Telescope, to constrain the exoplanet atmospheric compositions.

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Journal
Monthly Notices of the Royal Astronomical Society
Published
2025-10-20
DOI
https://doi.org/10.1093/mnras/staf1807
Primary Topic
Astro and Planetary Science
Type
article
Field-Weighted Citation Impact
0.00

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article

TOI-7166 b: a habitable zone mini-Neptune planet around a nearby low-mass star

Benjamin V. Rackham, Julien de Wit, Selçuk Yalçınkaya, Benjamin M. Tofflemire et al.
Monthly Notices of the Royal Astronomical Society
Astro and Planetary Science
article

TOI-7166 b: a habitable zone mini-Neptune planet around a nearby low-mass star

Benjamin V. Rackham, Julien de Wit, Selçuk Yalçınkaya, Benjamin M. Tofflemire, Ramotholo Sefako, M. Gillon, F. J. Pozuelos, John Jenkins, A. Sota, Emmanuël Jehin, D. Queloz, Georgina Dransfield, Adam J. Burgasser, P. J. Amado, Sebastián Zúñiga-Fernández, Abderahmane Soubkiou, Yasmin Davis, Karen A. Collins, Chris Stockdale, M. Serra‐Ricart, Steve B. Howell, A. H. M. J. Triaud, Artem Burdanov, Y. Gómez Maqueo Chew, Mathilde Timmermans, Colin Littlefield, K. Horne, Prajwal Niraula, Khalid Barkaoui, R. Varas, P. P. Pedersen, M. J. Hooton, Clàudia Janó Muñoz, Emma Softich, Elsa Ducrot, Brice-Olivier Demory, Özgür Baştürk, E. L. Martín, Keivan G. Stassun, Sarah J. Deveny, Avi Shporer, Francis Zong Lang, M. G. Scott, Özlem Şimşir
article en

Abstract

ABSTRACT We present the discovery and validation of TOI-7166 b, a $2.01 \pm 0.05\,\mathrm{ R}_{\oplus }$ planet orbiting a nearby low-mass star. We validated the planet by combining Transiting Exoplanet Survey Satellite and multicolour high-precision photometric observations from ground-based telescopes, together with spectroscopic data, high-contrast imaging, archival images, and statistical arguments. The host star is an M4-type dwarf at a distance of $\sim$35 pc from the Sun. It has a mass and a radius of $M_\star = 0.190 \pm 0.004\, \mathrm{ M}_\odot$ and $R_\star =0.222 \pm 0.005\, \mathrm{ R}_\odot$, respectively. TOI-7166 b has an orbital period of 12.9 d, which places it close to the inner edge of the Habitable Zone of its host star, receiving an insolation flux of $S_\mathrm{ p}=1.07\pm 0.08\, \mathrm{ S}_{\oplus }$ and an equilibrium temperature of $T_{\rm eq}~= 249\pm 5$ K (assuming a null Bond albedo). The brightness of the host star makes TOI-7166 a suitable target for radial velocity follow-up to measure the planetary mass and bulk density. Moreover, the physical parameters of the system including the infrared brightness ($K_{\rm mag} = 10.6$) of the star and the planet-to-star radius ratio ($0.0823 \pm 0.0012$) make TOI-7166 b an exquisite target for transmission spectroscopic observations with the James Webb Space Telescope, to constrain the exoplanet atmospheric compositions.

Monthly Notices of the Royal Astronomical SocietyVol. 544(2)
Andrews University (US), University of Bern (CH), Ames Research Center (US), Centre National de la Recherche Scientifique (FR), Planetary Science Institute (US), Research Institute for Advanced Computer Science (US), Ankara University (TR), University of Liège (BE), Universidad de La Laguna (ES), University of St Andrews (GB), Maria Curie-Skłodowska University (PL), Vanderbilt University (US), Commissariat à l'Énergie Atomique et aux Énergies Alternatives (FR), Université Paris-Saclay (FR), Oakwood Academy (GB), Northeast Catholic College (US), NASA Research Park (US), ETH Zurich (CH), University of California San Diego (US), University of Oxford (GB), Astrophysique, Instrumentation et Modélisation (FR), Cavendish Hospital (GB), Bay Area Environmental Research Institute (US), South African Radio Astronomy Observatory (ZA), Observatorio de la Inmigración de Tenerife (ES), Center for Astrophysics Harvard & Smithsonian (US), CEA Paris-Saclay (FR), Instituto de Astrofísica de Canarias (ES), Astronomy and Space (AU), Spanish National Observatory (ES), Astronomical Observatory (RS), Instituto de Astrofísica de Andalucía (ES), Ellinbank Observatory (AU), Massachusetts Institute of Technology (US), University of Birmingham (GB), Search for Extraterrestrial Intelligence (US), Universidad Nacional Autónoma de México (MX)
National Science Foundation, National Aeronautics and Space Administration, Magdalen College, University of Oxford, European Commission, Schweizerischer Nationalfonds zur Förderung der Wissenschaftlichen Forschung, Fonds De La Recherche Scientifique - FNRS, Nuclear Safety and Security Commission, Ministerio de Ciencia e Innovación, Fondation Merac, Instituto de Astrofísica de Andalucía, Science Mission Directorate, Science and Technology Facilities Council, Agencia Estatal de Investigación
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