Article (Scientific journals)
GJ 357: A low-mass planetary system uncovered by precision radial velocities and dynamical simulations
Jenkins, James S.; Pozuelos Romero, Francisco José; Tuomi, Mikko et al.
2019In Monthly Notices of the Royal Astronomical Society, 490 (4), p. 5585 - 5595
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Keywords :
Planetary systems; Planets and satellites: detection; Planets and satellites: dynamical evolution and stability; Stars: activity; Stars: low-mass; Astronomy and Astrophysics; Space and Planetary Science; astro-ph.EP; astro-ph.SR
Abstract :
[en] 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, 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, 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+0.117−0.120 M, 1.167+0.037−0.036 R, and 7.757+0.889−0.789 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.
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
Jenkins, James S. ;  Departamento de Astronomía, Universidad de Chile, Santiago, Chile ; Centro de Astrofísica y Tecnologías Afines (CATA), Santiago, Chile
Pozuelos Romero, Francisco José  ;  Université de Liège - ULiège > Unités de recherche interfacultaires > Space sciences, Technologies and Astrophysics Research (STAR) ; Université de Liège - ULiège > Département d'astrophysique, géophysique et océanographie (AGO) > Origines Cosmologiques et Astrophysiques (OrCa)
Tuomi, Mikko;  Departamento de Astronomía, Universidad de Chile, Santiago, Chile ; Center for Astrophysics, University of Hertfordshire, College Lane Campus, Hatfield, Hertfordshire, United Kingdom
Berdiñas, Zaira M.;  Departamento de Astronomía, Universidad de Chile, Santiago, Chile
Díaz, Matias R.;  Departamento de Astronomía, Universidad de Chile, Santiago, Chile
Vines, Jose I.;  Departamento de Astronomía, Universidad de Chile, Santiago, Chile
Suárez, Juan C. ;  Departamento de Física Teórica y del Cosmos, Universidad de Granada, Campus de Fuentenueva s/n, Granada, Spain ; Instituto de Astrofísica de Andalucía (CSIC), Granada, Spain
Peña Rojas, Pablo A.;  Departamento de Astronomía, Universidad de Chile, Santiago, Chile
Language :
English
Title :
GJ 357: A low-mass planetary system uncovered by precision radial velocities and dynamical simulations
Publication date :
December 2019
Journal title :
Monthly Notices of the Royal Astronomical Society
ISSN :
0035-8711
eISSN :
1365-2966
Publisher :
Oxford University Press
Volume :
490
Issue :
4
Pages :
5585 - 5595
Peer reviewed :
Peer Reviewed verified by ORBi
Name of the research project :
Proyecto Basal
Funders :
FONDECYT - Chile Fondo Nacional de Desarrollo Científico y Tecnológico [CL]
CATA-Basal
CONICYT - Comisión Nacional de Investigación Científica y Tecnológica [CL]
Spanish Public Funds for Research
Funding text :
We thank the referee Stephen Kane for his detailed review of the manuscript that helped tighten-up various sections of our work. JSJ 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 fromSpanish Public Funds for Research under projects ESP2017-87676-C5-2-R. JCS acknowledgesfunding from RYC-2012-09913 under the "Ram?n y Cajal" program of the Spanish Ministry of Science and Education.We thank the referee Stephen Kane for his detailed review of the manuscript that helped tighten-up various sections of our work. JSJ and MT acknowledge funding by Fondecyt through grant 1161218 and partial support from CATA-Basal (PB06, Con-icyt). ZMB acknowledges CONICYT-FONDECYT/Chile Post-doctorado 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 fromSpanish Public Funds for Research under projects ESP2017-87676-C5-2-R. JCS acknowledgesfunding from RYC-2012-09913 under the "Ramón y Cajal" program of the Spanish Ministry of Science and Education.
Commentary :
Manuscript accepted to MNRAS 15/10/2019
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