B. Toledo-Padrón, C. Lovis, A. Suárez Mascareño, S. C. C. Barros, J. I. González Hernández, A. Sozzetti, F. Bouchy, M. R. Zapatero-Osorio, R. Rebolo López, S. Cristiani, F. Pepe, N. C. Santos, S. G. Sousa, H. M. Tabernero, J. Lillo Box, D. Bossini, V. Zh. Adibekyan, R. Allart, M. Damasso, V. D'Odorico, P. Figueira, B. Lavie, G. Lo Curto, A. Mehner, G. Micela, A. Modigliani, N. J. Nunes, E. Pallé, M. Abreu, M. Affolter, Y. Alibert, M. Aliverti, C. Allende Prieto, D. Castro Alves, M. Amate, G. Avila, V. Baldini, T. Bandy, S. Benatti, W. Benz, A. Bianco, C. Broeg, A. Cabral, G. Calderone, R. Cirami, J. Coelho, P. Conconi, I. Coretti, C. Cumani, G. Cupani, S. Deiries, H. Dekker, B. Delabre, O. Demangeon, P. Di Marcantonio, D. Ehrenreich, A. Fragoso, L. Genolet, M. Genoni, R. T. Génova-Santos, I. Hughes, O. Iwert, J. Knudstrup, M. Landoni, J.-L. Lizon, C. Maire, A. Manescau, C. J. A. P. Martins, D. Megevand, P. Molaro, M. J. P. F. G. Monteiro, M. A. Monteiro, M. Moschetti, E. Mueller, L. Oggioni, A. Oliveira, M. Oshagh, G. Pariani, L. Pasquini, E. Poretti, J. L. Rasilla, E. Redaelli, M. Riva, S. Santana Tschudi, P. Santin, P. Santos, A. G. Segovia Milla, D. Sosnowska, P. Spanò, F. Tenegi, S. Udry, A. Zanutta, F. M. Zerbi
Abstract
Context. An accurate characterization of the known exoplanet population is key to understanding the origin and evolution of planetary systems. Determining true planetary masses through the radial velocity (RV) method is expected to experience a great improvement thanks to the availability of ultra-stable echelle spectrographs.
Aims. We took advantage of the extreme precision of the new-generation echelle spectrograph ESPRESSO to characterize the transiting planetary system orbiting the G2V star K2-38 located at 194 pc from the Sun with V ~ 11.4. This system is particularly interesting because it could contain the densest planet detected to date.
Methods. We carried out a photometric analysis of the available K2 photometric light curve of this star to measure the radius of its two known planets, K2-38b and K2-38c, with Pb = 4.01593 ± 0.00050 d and Pc = 10.56103 ± 0.00090 d, respectively. Using 43 ESPRESSO high-precision RV measurements taken over the course of 8 months along with the 14 previously published HIRES RV measurements, we modeled the orbits of the two planets through a Markov chain Monte Carlo analysis, significantly improving their mass measurements.
Results. Using ESPRESSO spectra, we derived the stellar parameters, Teff = 5731 ± 66, log g = 4.38 ± 0.11 dex, and [Fe/H] = 0.26 ± 0.05 dex, and thus the mass and radius of K2-38, M⋆ = 1.03−0.02+0.04 M⊕ and R⋆ = 1.06−0.06+0.09 R⊕. We determine new values for the planetary properties of both planets. We characterize K2-38b as a super-Earth with RP = 1.54 ± 0.14 R⊕ and Mp = 7.3−1.0+1.1 M⊕, and K2-38c as a sub-Neptune with RP = 2.29 ± 0.26 R⊕ and Mp = 8.3−1.3+1.3 M⊕. Combining the radius and mass measurements, we derived a mean density of ρp = 11.0−2.8+4.1 g cm−3 for K2-38b and ρp = 3.8−1.1+1.8 g cm−3 for K2-38c, confirming K2-38b as one of the densest planets known to date.
Conclusions. The best description for the composition of K2-38b comes from an iron-rich Mercury-like model, while K2-38c is better described by a rocky-model with H2 envelope. The maximum collision stripping boundary shows how giant impacts could be the cause for the high density of K2-38b. The irradiation received by each planet places them on opposite sides of the radius valley. We find evidence of a long-period signal in the RV time-series whose origin could be linked to a 0.25–3 MJ planet or stellar activity.
Keywords
techniques: radial velocities; techniques: photometric; instrumentation: spectrographs; stars: individual: K2-38; planets and satellites: detection; planets and satellites: composition; Astrophysics - Earth and Planetary Astrophysics; Astrophysics - Solar
Notes
Based (in part) on Guaranteed Time Observations collected at the European Southern Observatory under ESO programmes1102.C-0744, 112.C-0958, and 1104.C-0350 by the ESPRESSO Consortium.
The ESPRESSO RVs used in this paper are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/641/A92
Astronomy & Astrophysics
Volume 641, Article Number A92, Number of pages 14
2020 September
