D. Hidalgo, E. Pallé, R. Alonso, D. Gandolfi, M. Fridlund, G. Nowak, R. Luque, T. Hirano, A. B. Justesen, W. D. Cochran, O. Barragán, L. Spina, F. Rodler, S. Albrecht, D. R. Anderson, P. J. Amado, E. M. Bryant, J. Caballero, J. Cabrera, Sz. Csizmadia, F. Dai, J. de Leon, H. J. Deeg, P. Eigmüller, M. Endl, A. Erikson, M. Esposito, P. Figueira, I. Georgieva, S. Grziwa, E. W. Guenther, A. Hatzes, M. Hjorth, H. J. Hoeijmakers, P. Kabath, J. Korth, M. Kuzuhara, M. Lafarga, M. Lampon, I.C. Leão, J. H. Livingston, S. Mathur, P. Montañés Rodríguez, J. C. Morales, F. Murgas, E. Nagel, N. Narita, L. D. Nielsen, M. Pätzold, C. M. Persson, J. Prieto-Arranz, A. Quirrenbach, H. Rauer, S. Redfield, A. Reiners, I. Ribas, A. M. S. Smith, J. ¦ubjak, V. Van Eylen, P. A. Wilson
We report the discovery of a new planetary system with three transiting planets, one super-Earth and two sub-Neptunes, that orbit EPIC 249893012, a G8 IV-V evolved star (M⋆ = 1.05 ± 0.05 M⊙, R⋆ = 1.71 ± 0.04 R⊙, Teff = 5430 ± 85 K). The star is just leaving the main sequence. We combined K2 photometry with IRCS adaptive-optics imaging and HARPS, HARPS-N, and CARMENES high-precision radial velocity measurements to confirm the planetary system, determine the stellar parameters, and measure radii, masses, and densities of the three planets. With an orbital period of 3.5949−0.0007+0.0007 days, a mass of 8.75−1.08+1.09 M⊕, and a radius of 1.95−0.08+0.09 R⊕, the inner planet b is compatible with nickel-iron core and a silicate mantle (ρb = 6.39−1.04+1.19 g cm−3). Planets c and d with orbital periods of 15.624−0.001+0.001 and 35.747−0.005+0.005 days, respectively, have masses and radii of 14.67−1.89+1,84 M⊕ and 3.67−0.14+0.17 R⊕ and 10.18−2.42+2.46 M⊕ and 3.94−0.12+0.13 R⊕, respectively, yielding a mean density of 1.62−0.29+0.30 and 0.91−0.23+0.25 g cm−3, respectively. The radius of planet b lies in the transition region between rocky and gaseous planets, but its density is consistent with a rocky composition. Its semimajor axis and the corresponding photoevaporation levels to which the planet has been exposed might explain its measured density today. In contrast, the densities and semimajor axes of planets c and d suggest a very thick atmosphere. The singularity of this system, which orbits a slightly evolved star that is just leaving the main sequence, makes it a good candidate for a deeper study from a dynamical point of view.
planetary systems; planets and satellites: detection; techniques: photometric; techniques: radial velocities; planets and satellites: fundamental parameters; Astrophysics - Earth and Planetary Astrophysics; Astrophysics - Solar and Stellar Astrophysics
Based on observations made with the ESO-3.6m telescope at La Silla Observatory (Chile) under programs 0101.C-0829, 1102.C-0923, and 60.A-9700.
Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundación Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, under programs CAT18A_130, CAT18B_93, and A37TAC_37.
Astronomy and Astrophysics
Volume 636, Article Number A89, Number of pages 13