GJ 357: a low-mass planetary system uncovered by precision radial velocities and dynamical simulations

We report the detection of a new planetary system orbiting the nearby M2.5V star GJ 357, using precision radial velocities from three separate echelle spectrographs, High Accuracy Radial velocity Planet Searcher (HARPS), High Resolution Echelle Spectrograph (HiRES), and Ultraviolet and Visible Echelle Spectrograph (UVES). Three small planets have been confirmed in the system, with periods of 9.125 +/- 0.001, 3.9306 +/- 0.0003, and 55.70 +/- 0.05 d, and minimum masses of 3.33 +/- 0.48, 2.09 +/- 0.32, and 6.72 +/- 0.94 M-circle plus, respectively. The second planet in our system, GJ 357 c, was recently shown to transit by the Transiting Exoplanet Survey Satellite (TESS), but we could find no transit signatures for the other two planets. Dynamical analysis reveals the system is likely to be close to coplanar, is stable on Myr time-scales, and places strong upper limits on the masses of the two non-transiting planets GJ 357 b and GJ 357 d of 4.25 and 11.20 M-circle plus, respectively. Therefore, we confirm the system contains at least two super-Earths, and either a third super-Earth or mini-Neptune planet. GJ 357 b and GJ 357 c are found to be close to a 7:3 mean motion resonance, however no libration of the orbital parameters was found in our simulations. Analysis of the photometric light curve of the star from the TESS, when combined with our radial velocities, reveals GJ 357 c has an absolute mass, radius, and density of 2.248(-0.120)(+0.117) M-circle plus, 1.167(-0.036)(+0.037) R-circle plus, and 7.757(-0.789)(+0.889) g cm(-3), respectively. Comparison to super-Earth structure models reveals the planet is likely an iron-dominated world. The GJ 357 system adds to the small sample of low-mass planetary systems with well constrained masses, and further observational and dynamical follow-up is warranted to better understand the overall population of small multiplanet systems in the solar neighbourhood.Copyright © 2020 The Royal Astronomical SocietySJ and MT acknowledge funding by Fondecyt through grant 1161218 and partial support from CATA-Basal (PB06, Conicyt). ZMB acknowledges CONICYT-FONDECYT/Chile Postdoctorado 3180405. JIV acknowledges support of CONICYT-PFCHA/Doctorado Nacional-21191829, Chile. MRD acknowledges support of CONICYT-PFCHA/Doctorado Nacional-21140646, Chile, and Proyecto Basal AFB-170002. FJP and JCS acknowledge funding support from Spanish Public Funds for Research under projects ESP2017-87676-C5-2-R. JCS acknowledges funding from RYC-2012-09913 under the "Ramon y Cajal" program of the Spanish Ministry of Science and Education.Peer reviewe