Confirmation of the hot super-Neptune TOI-672 b with NIRPS and HARPS and Insights into the Neptunian desert around M dwarfs
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2026
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| author | Osborn, Ares Cloutier, Ryan Bourrier, Vincent Skinner, Bennett Gromek, Nicole Srivastava, Avidaan Bouchy, François Cointepas, Marion Cook, Neil J. Nari, Nicola Almenara, Jose Manuel Artigau, 'Etienne Bonfils, Xavier Cadieux, Charles Eggenberger, Patrick L'Heureux, Alexandrine Baron, Frédérique Barros, Susana C. C. Benneke, Björn Bryan, Marta Martins, Bruno L. Canto Cowan, Nicolas B. Cristo, Eduardo Delfosse, Xavier De Medeiros, Jose Renan Doyon, René Dumusque, Xavier Ehrenreich, David Hernández, Jonay I. González Lafrenière, David Leão, Izan de Castro Lovis, Christophe Malo, Lison Melo, Claudio Mignon, Lucile Mordasini, Christoph Pepe, Francesco Rebolo, Rafael Rowe, Jason Santos, Nuno C. Ségransan, Damien Mascareño, Alejandro Suárez Udry, Stéphane Valencia, Diana Wade, Gregg Aguiar, José Luan A. Allart, Romain Moulla, Khaled Al Carmona, Andres Collins, Karen A. Delgado-Mena, Elisa Gomes, Roseane de Lima Dixon, George Evans, Phil Frensch, Yolanda G. C. Fontinele, Dasaev O. Forveille, Thierry Gan, Tianjun Hobson, Melissa J. Messias, Yuri S. Nielsen, Louise D. Parc, Léna Shu, Ying Stefanov, Atanas K. Tan, Thiam-Gun Vignes, Jean-Pascal Wardenier, Joost P. Weisserman, Drew |
| author_facet | Osborn, Ares Cloutier, Ryan Bourrier, Vincent Skinner, Bennett Gromek, Nicole Srivastava, Avidaan Bouchy, François Cointepas, Marion Cook, Neil J. Nari, Nicola Almenara, Jose Manuel Artigau, 'Etienne Bonfils, Xavier Cadieux, Charles Eggenberger, Patrick L'Heureux, Alexandrine Baron, Frédérique Barros, Susana C. C. Benneke, Björn Bryan, Marta Martins, Bruno L. Canto Cowan, Nicolas B. Cristo, Eduardo Delfosse, Xavier De Medeiros, Jose Renan Doyon, René Dumusque, Xavier Ehrenreich, David Hernández, Jonay I. González Lafrenière, David Leão, Izan de Castro Lovis, Christophe Malo, Lison Melo, Claudio Mignon, Lucile Mordasini, Christoph Pepe, Francesco Rebolo, Rafael Rowe, Jason Santos, Nuno C. Ségransan, Damien Mascareño, Alejandro Suárez Udry, Stéphane Valencia, Diana Wade, Gregg Aguiar, José Luan A. Allart, Romain Moulla, Khaled Al Carmona, Andres Collins, Karen A. Delgado-Mena, Elisa Gomes, Roseane de Lima Dixon, George Evans, Phil Frensch, Yolanda G. C. Fontinele, Dasaev O. Forveille, Thierry Gan, Tianjun Hobson, Melissa J. Messias, Yuri S. Nielsen, Louise D. Parc, Léna Shu, Ying Stefanov, Atanas K. Tan, Thiam-Gun Vignes, Jean-Pascal Wardenier, Joost P. Weisserman, Drew |
| contents | The Neptunian desert is a distinct lack of Neptune-sized planets at short orbital periods, purportedly carved by photoevaporation and tidal circularization following high-eccentricity migration. Constraining these processes and how they vary across different host-star spectral types requires the detailed characterization of planets in the desert and around its boundaries. In this study, we confirm the planetary nature of a massive super-Neptune identified by TESS around the M0 dwarf TOI-672. We analyse photometry from TESS and ExTrA and precise radial velocity measurements taken with the recently commissioned Near-InfraRed Planet Searcher (NIRPS) and HARPS spectrographs. We measure the planetary orbital period, radius, and mass of 3.634 days, 5.31 +0.24 -0.26 Rearth, and 50.9 +4.5 -4.4 Mearth, respectively. Our findings place TOI-672 b within the Neptunian ridge, a pile-up of planets from 3--5 days at the Neptunian desert boundary. We then use a novel approach to determine the desert boundaries in period-radius space and instellation-radius space, and, for the first time, compare the Neptunian desert boundaries for planets orbiting FGK versus M dwarf stars. We determine that the boundary ridge shifts slightly inward from 3.3 +- 1.4 days for FGK host stars to 2.2 +- 1.0 days for M dwarf host stars; these values do not statistically significantly differ from each other, and the shift to shorter periods for M dwarf planets is smaller than theoretical photoevaporation models predict. We also find that TOI-672 b is a single-planet system within the sensitivity limits of our RV and TTV datasets. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2603_12345 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | Confirmation of the hot super-Neptune TOI-672 b with NIRPS and HARPS and Insights into the Neptunian desert around M dwarfs Osborn, Ares Cloutier, Ryan Bourrier, Vincent Skinner, Bennett Gromek, Nicole Srivastava, Avidaan Bouchy, François Cointepas, Marion Cook, Neil J. Nari, Nicola Almenara, Jose Manuel Artigau, 'Etienne Bonfils, Xavier Cadieux, Charles Eggenberger, Patrick L'Heureux, Alexandrine Baron, Frédérique Barros, Susana C. C. Benneke, Björn Bryan, Marta Martins, Bruno L. Canto Cowan, Nicolas B. Cristo, Eduardo Delfosse, Xavier De Medeiros, Jose Renan Doyon, René Dumusque, Xavier Ehrenreich, David Hernández, Jonay I. González Lafrenière, David Leão, Izan de Castro Lovis, Christophe Malo, Lison Melo, Claudio Mignon, Lucile Mordasini, Christoph Pepe, Francesco Rebolo, Rafael Rowe, Jason Santos, Nuno C. Ségransan, Damien Mascareño, Alejandro Suárez Udry, Stéphane Valencia, Diana Wade, Gregg Aguiar, José Luan A. Allart, Romain Moulla, Khaled Al Carmona, Andres Collins, Karen A. Delgado-Mena, Elisa Gomes, Roseane de Lima Dixon, George Evans, Phil Frensch, Yolanda G. C. Fontinele, Dasaev O. Forveille, Thierry Gan, Tianjun Hobson, Melissa J. Messias, Yuri S. Nielsen, Louise D. Parc, Léna Shu, Ying Stefanov, Atanas K. Tan, Thiam-Gun Vignes, Jean-Pascal Wardenier, Joost P. Weisserman, Drew Earth and Planetary Astrophysics The Neptunian desert is a distinct lack of Neptune-sized planets at short orbital periods, purportedly carved by photoevaporation and tidal circularization following high-eccentricity migration. Constraining these processes and how they vary across different host-star spectral types requires the detailed characterization of planets in the desert and around its boundaries. In this study, we confirm the planetary nature of a massive super-Neptune identified by TESS around the M0 dwarf TOI-672. We analyse photometry from TESS and ExTrA and precise radial velocity measurements taken with the recently commissioned Near-InfraRed Planet Searcher (NIRPS) and HARPS spectrographs. We measure the planetary orbital period, radius, and mass of 3.634 days, 5.31 +0.24 -0.26 Rearth, and 50.9 +4.5 -4.4 Mearth, respectively. Our findings place TOI-672 b within the Neptunian ridge, a pile-up of planets from 3--5 days at the Neptunian desert boundary. We then use a novel approach to determine the desert boundaries in period-radius space and instellation-radius space, and, for the first time, compare the Neptunian desert boundaries for planets orbiting FGK versus M dwarf stars. We determine that the boundary ridge shifts slightly inward from 3.3 +- 1.4 days for FGK host stars to 2.2 +- 1.0 days for M dwarf host stars; these values do not statistically significantly differ from each other, and the shift to shorter periods for M dwarf planets is smaller than theoretical photoevaporation models predict. We also find that TOI-672 b is a single-planet system within the sensitivity limits of our RV and TTV datasets. |
| title | Confirmation of the hot super-Neptune TOI-672 b with NIRPS and HARPS and Insights into the Neptunian desert around M dwarfs |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2603.12345 |