학술논문
TOI-1468: A system of two transiting planets, a super-Earth and a mini-Neptune, on opposite sides of the radius valley
Document Type
Working Paper
Author
Chaturvedi, P.; Bluhm, P.; Nagel, E.; Hatzes, A. P.; Morello, G.; Brady, M.; Korth, J.; Molaverdikhani, K.; Kossakowski, D.; Caballero, J. A.; Guenther, E. W.; Pallé, E.; Espinoza, N.; Seifahrt, A.; Lodieu, N.; Cifuentes, C.; Furlan, E.; Amado, P. J.; Barclay, T.; Bean, J.; Béjar, V. J. S.; Bergond, G.; Boyle, A. W.; Ciardi, D.; Collins, K. A.; Collins, K. I.; Esparza-Borges, E.; Fukui, A.; Gnilka, C. L.; Goeke, R.; Guerra, P.; Henning, Th.; Herrero, E.; Howell, S. B.; Jeffers, S. V.; Jenkins, J. M.; Jensen, E. L. N.; Kasper, D.; Kodama, T.; Latham, D. W.; López-González, M. J.; Luque, R.; Montes, D.; Morales, J. C.; Mori, M.; Murgas, F.; Narita, N.; Nowak, G.; Parviainen, H.; Passegger, V. M.; Quirrenbach, A.; Reffert, S.; Reiners, A.; Ribas, I.; Ricker, G. R.; Rodríguez, E.; Rodríguez-López, C.; Schlecker, M.; Schwarz, R. P.; Schweitzer, A.; Seager, S.; Stefánsson, G.; Stockdale, C.; Tal-Or, L.; Twicken, J. D.; Vanaverbeke, S.; Wang, G.; Watanabe, D.; Winn, J. N.; Zechmeister, M.
Source
A&A 666, A155 (2022)
Subject
Language
Abstract
We report the discovery and characterization of two small transiting planets orbiting the bright M3.0V star TOI-1468 (LSPM J0106+1913), whose transit signals were detected in the photometric time series in three sectors of the TESS mission. We confirm the e planetary nature of both of them using precise radial velocity measurements from the CARMENES and MAROON-X spectrographs, and supplement them with ground-based transit photometry. A joint analysis of all these data reveals that the shorter-period planet, TOI-1468 b ($P_{\rm b}$ = 1.88 d), has a planetary mass of $M_{\rm b} = 3.21\pm0.24$ $M_{\oplus}$ and a radius of $R_{\rm b} =1.280^{+0.038}_{-0.039} R_{\oplus}$, resulting in a density of $\rho_{\rm b} = 8.39^{+ 1.05}_{- 0.92}$ g cm$^{-3}$, which is consistent with a mostly rocky composition. For the outer planet, TOI-1468 c ($P_{\rm c} = 15.53$ d), we derive a mass of $M_{\rm c} = 6.64^{+ 0.67}_{- 0.68}$ $M_{\oplus}$, a radius of $R_{\rm c} = 2.06\pm0.04\,R_{\oplus}$, and a bulk density of $\rho_{c} = 2.00^{+ 0.21}_{- 0.19}$ g cm$^{-3}$, which corresponds to a rocky core composition with a H/He gas envelope. These planets are located on opposite sides of the radius valley, making our system an interesting discovery as there are only a handful of other systems with the same properties. This discovery can further help determine a more precise location of the radius valley for small planets around M dwarfs and, therefore, shed more light on planet formation and evolution scenarios.
Comment: 26 pages, 15 figures
Comment: 26 pages, 15 figures