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Main Authors: Turner, Daisy A., Eschen, Yoshi Nike Emilia, Murgas, Felipe, Mortier, Annelies, Wilson, Thomas G, Fernández, Jorge Fernández, Gromek, Nicole, Morello, Giuseppe, Tabernero, Hugo M., Egger, Jo Ann, Vissapragada, Shreyas, Caballero, José A., Dreizler, Stefan, Freckelton, Alix Violet, Hatzes, Artie P., Lakeland, Ben Scott, Nagel, Evangelos, Naponiello, Luca, Vanaverbeke, Siegfried, Venner, Alexander, Osorio, María Rosa Zapatero, Amado, Pedro J., Béjar, Víctor J. S., Bonomo, Aldo Stefano, Buchhave, Lars A., Cameron, Andrew Collier, Carleo, Ilaria, Chaturvedi, Priyanka, Cloutier, Ryan, Damasso, Mario, Daspute, Mangesh, Dholakia, Shishir, Dufoer, Sjoerd, Dumusque, Xavier, Fiorenzano, Aldo Fabricio Martinez, Ghedina, Adriano, Harutyunyan, Avet, Herrero, Enrique, John, Ancy Anna, Lillo-Box, Jorge, Lodieu, Nicolas, López-Morales, Mercedes, Malavolta, Luca, Mancini, Luigi, Mantovan, Giacomo, Montes, David, Morales, Juan Carlos, Nicholson, Belinda, Orell-Miquel, Jaume, Palethorpe, Larissa, Palle, Enric, Quirrenbach, Andreas, Reffert, Sabine, Reiners, Ansgar, Ribas, Ignasi, Rice, Ken, Silva, André M., Sozzetti, Alessandro, Stalport, Manu, Tal-Or, Lev, Trifonov, Trifon, Udry, Stéphane, Zechmeister, Mathias
Format: Preprint
Published: 2025
Subjects:
Earth and Planetary Astrophysics
Online Access:https://arxiv.org/abs/2506.20564
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Table of Contents:
  • Small temperate planets are prime targets for exoplanet studies due to their possible similarities with the rocky planets in the Solar System. M dwarfs are promising hosts since the planetary signals are within our current detection capabilities. Gliese 12 b is a Venus-sized temperate planet orbiting a quiet M dwarf. We present here the first precise mass measurement of this small exoplanet. We performed a detailed analysis using HARPS-N, ESPRESSO, and CARMENES radial velocities, along with new and archival \tess, \cheops, and MuSCAT2/3 photometry data. From fitting the available data, we find that the planet has a radius of $R_\mathrm{p} = 0.93\pm0.06 \,\mathrm{R_\oplus}$ and a mass of $M_\mathrm{p} = 0.95^{+0.29}_{-0.30} \,\mathrm{M_\oplus}$ (a $3.2σ$ measurement of the semi-amplitude $K=0.67\pm0.21\,\mathrm{m\,s^{-1}}$), and is on an orbit with a period of $12.761418^{+0.000060}_{-0.000055}\,\mathrm{d}$. A variety of techniques were utilised to attenuate stellar activity signals. Gliese 12 b has an equilibrium temperature of $T_\mathrm{eq}=317 \pm 8\,\mathrm{K}$, assuming an albedo of zero, and a density consistent with that of Earth and Venus ($ρ_\mathrm{p}=6.4\pm2.4\,\mathrm{g\,cm^{-3}}$). We find that Gliese 12 b has a predominantly rocky interior and simulations indicate that it is unlikely to have retained any of its primordial gaseous envelope. The bulk properties of Gliese 12 b place it in an extremely sparsely populated region of both mass--radius and density--$T_\mathrm{eq}$ parameter space, making it a prime target for follow-up observations, including Lyman-$α$ studies.

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