Paper: Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Transmission Spectroscopy
Authors: Masayuki Kuzuhara, Akihiko Fukui, John H. Livingston, José A. Caballero, Jerome P. de Leon, Teruyuki Hirano, Yui Kasagi, Felipe Murgas, Norio Narita, Masashi Omiya, Jaume Orell-Miquel, Enric Palle, Quentin Changeat, Emma Esparza-Borges, Hiroki Harakawa, Coel Hellier, Yasunori Hori, Kai Ikuta, Hiroyuki Tako Ishikawa, Takanori Kodama, Takayuki Kotani, Tomoyuki Kudo, Juan C. Morales, Mayuko Mori, Evangelos Nagel, Hannu Parviainen, Volker Perdelwitz, Ansgar Reiners, Ignasi Ribas, Jorge Sanz-Forcada, Bun'ei Sato, Andreas Schweitzer, Hugo M. Tabernero, Takuya Takarada, Taichi Uyama, Noriharu Watanabe, Mathias Zechmeister, Néstor Abreu García, Wako Aoki, Charles Beichman, Víctor J. S. Béjar, Timothy D. Brandt, Yéssica Calatayud-Borras, Ilaria Carleo, David Charbonneau, Karen A. Collins, Thayne Currie, John P. Doty, Stefan Dreizler, Gareb Fernández-Rodríguez, Izuru Fukuda, Daniel Galán, Samuel Geraldía-González, Josafat González-Rodríguez, Yuya Hayashi, Christina Hedges, Thomas Henning, Klaus Hodapp, Masahiro Ikoma, Keisuke Isogai, Shane Jacobson, Markus Janson, Jon M. Jenkins, Taiki Kagetani, Eiji Kambe, Yugo Kawai, Kiyoe Kawauchi, Eiichiro Kokubo, Mihoko Konishi, Judith Korth, Vigneshwaran Krishnamurthy, Takashi Kurokawa, Nobuhiko Kusakabe, Jungmi Kwon, Andrés Laza-Ramos, Florence Libotte, Rafael Luque, Alberto Madrigal-Aguado, Yuji Matsumoto, Dimitri Mawet, Michael W. McElwain, Pedro Pablo Meni Gallardo, Giuseppe Morello, Sara Muñoz Torres, Jun Nishikawa, Stevanus K. Nugroho, Masahiro Ogihara, Alberto Peláez-Torres, David Rapetti, Manuel Sánchez-Benavente, Martin Schlecker, Sara Seager, Eugene Serabyn, Takuma Serizawa, Monika Stangret, Aoi Takahashi, Huan-Yu Teng, Motohide Tamura, Yuka Terada, Akitoshi Ueda, Tomonori Usuda, Roland Vanderspek, Sébastien Vievard, David Watanabe, Joshua N. Winn, Maria Rosa Zapatero Osorio
Figure caption: (Left) Mass–radius relation for planets with masses below 6 M ⊕ around M dwarfs with T eff ≤ 3900 K. Gray circles are all the known exoplanets in this mass range taken from the NASA Exoplanet Archive (2023a). We plot the 1σ, 2σ, and 3σ contours of the mass and the radius of Gliese 12 b. The colored curves show interior models of planets that are composed of pure water, pure silicate, Earth-like rock, and pure iron. We adopted T eq = 312.9 K and the AQUA (Haldemann et al. 2020), Birch–Murnaghan, and Vinet EoS (Seager et al. 2007; Zeng & Sasselov 2013) as equations of state of H2O, MgSiO3, and ϵ − Fe. The dashed and dashed–dotted curves show the mass–radius relation of a rocky core with a hydrogen-rich atmosphere of 0.01 wt% and 0.1 wt%, respectively. (Right) TSM values calculated for Gliese 12 b (square) and other small (R ≤ 1.5 R ⊕) exoplanets against their planetary radii. Colored symbols indicate the planets whose insolation flux (S) is <2.3 S ⊕, with colors scaled by S (as shown by the color bar). The symbols with black edges represent the planets with masses constrained by methods other than an empirical mass–radius relation. The planets within this range are labeled: T700, L890, and T2095 stand for TOI-700 (Gilbert et al. 2023), LP 890-9 (Delrez et al. 2022), and TOI-2095 (Murgas et al. 2023), respectively. The planets with S > 2.3 S ⊕ are indicated by gray symbols. On both the left and right panels, the planets around TRAPPIST-1 are plotted with triangles.