A. Mortier, A. S. Bonomo, V. M. Rajpaul, L. A. Buchhave, A. Vanderburg, L. Zeng, M. López-Morales, L. Malavolta, A. Collier Cameron, C. D. Dressing, P. Figueira, V. Nascimbeni, K. Rice, A. Sozzetti, C. A. Watson, L. Affer, F. Bouchy, D. Charbonneau, A. Harutyunyan, R. D. Haywood, J. A. Johnson, D. W. Latham, C. Lovis, A. F. Martinez Fiorenziano, M. Mayor, G. Micela, D. Molinari, F. Motalebi, F. Pepe, G. Piotto, D. F. Phillips, E. Poretti, D. Sasselov, D. Ségransan, S. Udry
Abstract
This paper reports on the validation and mass measurement of K2-263 b, a sub-Neptune orbiting a quiet G9V star. Using K2 data from campaigns C5 and C16, we find this planet to have a period of 50.818947±0.000094 d and a radius of 2.41±0.12 R⊕. We followed this system with HARPS-N to obtain 67 precise radial velocities (RVs). A combined fit of the transit and radial velocity data reveals that K2-263 b has a mass of 14.8±3.1 M⊕. Its bulk density (5.7+1.6−1.4 g cm−3) implies that this planet has a significant envelope of water or other volatiles around a rocky core. K2-263 b likely formed in a similar way as the cores of the four giant planets in our own Solar System, but for some reason, did not accrete much gas. The planetary mass was confirmed by an independent Gaussian process-based fit to both the RVs and the spectroscopic activity indicators. K2-263 b belongs to only a handful of confirmed K2 exoplanets with periods longer than 40 d. It is among the longest periods for a small planet with a precisely determined mass using RVs.
Keywords
techniques: photometric, techniques: radial velocities, techniques: spectroscopic, planets and satellites: individual: K2-263b
Monthly Notices of the Royal Astronomical Society
Volume 481, Issue 2
2018 September
