Lalitha, S.; Baroch, D.; Morales, J. C.; Passegger, V. M.; Bauer, F. F.; Cardona Guillén, C.; Dreizler, S.; Oshagh, M.; Reiners, A.; Ribas, I.; Caballero, J. A.; Quirrenbach, A.; Amado, P. J.; Béjar, V. J. S.; Colomé, J.; Cortés-Contreras, M.; Galadí-Enríquez, D.; González-Cuesta, L.; Guenther, E. W.; Hagen, H.-J.; Henning, T.; Herrero, E.; Husser, T.-O.; Jeffers, S. V.; Kaminski, A.; Kürster, M.; Lafarga, M.; Lodieu, N.; López-González, M. J.; Montes, D.; Perger, M.; Rosich, A.; Rodríguez, E.; Rodríguez-López, C.; Schmitt, J. H. M. M.; Tal-Or, L.; Zechmeister, M.
Bibliographical reference
Astronomy and Astrophysics, Volume 627, id.A116, 21 pp.
Description
Although M dwarfs are known for high levels of stellar activity, they
are ideal targets for the search of low-mass exoplanets with the radial
velocity (RV) method. We report the discovery of a planetary-mass
companion around LSPM J2116+0234 (M3.0 V) and confirm the existence of a
planet orbiting GJ 686 (BD+18 3421; M1.0 V). The discovery of the planet
around LSPM J2116+0234 is based on CARMENES RV observations in the
visual and near-infrared channels. We confirm the planet orbiting around
GJ 686 by analyzing the RV data spanning over two decades of
observationsfrom CARMENES VIS, HARPS-N, HARPS, and HIRES. We find
planetary signals at 14.44 and 15.53 d in the RV data for LSPM
J2116+0234 and GJ 686, respectively. Additionally, the RV, photometric
time series, and various spectroscopic indicators show hints of
variations of 42 d for LSPM J2116+0234 and 37 d for GJ 686, which we
attribute to the stellar rotation periods. The orbital parameters of the
planets are modeled with Keplerian fits together with correlated noise
from the stellar activity. A mini-Neptune with a minimum mass of 11.8
M⊕ orbits LSPM J2116+0234 producing a RV semi-amplitude
of 6.19 m s-1, while a super-Earth of mass 6.6
M⊕ orbits GJ 686 and produces a RV semi-amplitude of
3.0 m s-1. Both LSPM J2116+0234 and GJ 686 have planetary
companions populating the regime of exoplanets with masses lower than 15
M⊕ and orbital periods <20 d.
Table A.1 and A.2 are only available at the CDS via anonymous ftp to
http://cdsarc.u-strasbg.fr
(
ftp://130.79.128.5) or via
http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/627/A116
Related projects
Very Low Mass Stars, Brown Dwarfs and Planets
Our goal is to study the processes that lead to the formation of low mass stars, brown dwarfs and planets and to characterize the physical properties of these objects in various evolutionary stages. Low mass stars and brown dwarfs are likely the most numerous type of objects in our Galaxy but due to their low intrinsic luminosity they are not so
Very Low Mass Stars, Brown Dwarfs and Planets
Our goal is to study the processes that lead to the formation of low mass stars, brown dwarfs and planets and to characterize the physical properties of these objects in various evolutionary stages. Low mass stars and brown dwarfs are likely the most numerous type of objects in our Galaxy but due to their low intrinsic luminosity they are not so
Exoplanets and Astrobiology
The search for life in the universe has been driven by recent discoveries of planets around other stars (known as exoplanets), becoming one of the most active fields in modern astrophysics. The growing number of new exoplanets discovered in recent years and the recent advance on the study of their atmospheres are not only providing new valuable
Exoplanets and Astrobiology
The search for life in the universe has been driven by recent discoveries of planets around other stars (known as exoplanets), becoming one of the most active fields in modern astrophysics. The growing number of new exoplanets discovered in recent years and the recent advance on the study of their atmospheres are not only providing new valuable
