Bibcode
Perger, M.; Scandariato, G.; Ribas, I.; Morales, J. C.; Affer, L.; Azzaro, M.; Amado, P. J.; Anglada-Escudé, G.; Baroch, D.; Barrado, D.; Bauer, F. F.; Béjar, V. J. S.; Caballero, J. A.; Cortés-Contreras, M.; Damasso, M.; Dreizler, S.; González-Cuesta, L.; González Hernández, J. I.; Guenther, E. W.; Henning, T.; Herrero, E.; Jeffers, S. V.; Kaminski, A.; Kürster, M.; Lafarga, M.; Leto, G.; López-González, M. J.; Maldonado, J.; Micela, G.; Montes, D.; Pinamonti, M.; Quirrenbach, A.; Rebolo, R.; Reiners, A.; Rodríguez, E.; Rodríguez-López, C.; Schmitt, J. H. M. M.; Sozzetti, A.; Suárez Mascareño, A.; Toledo-Padrón, B.; Zanmar Sánchez, R.; Zapatero Osorio, M. R.; Zechmeister, M.
Bibliographical reference
Astronomy and Astrophysics, Volume 624, id.A123, 19 pp.
Advertised on:
4
2019
Journal
Citations
21
Refereed citations
20
Description
Context. Small planets around low-mass stars often show orbital periods
in a range that corresponds to the temperate zones of their host stars
which are therefore of prime interest for planet searches. Surface
phenomena such as spots and faculae create periodic signals in radial
velocities and in observational activity tracers in the same range, so
they can mimic or hide true planetary signals. Aims: We aim to
detect Doppler signals corresponding to planetary companions, determine
their most probable orbital configurations, and understand the stellar
activity and its impact on different datasets. Methods: We
analyzed 22 yr of data of the M1.5 V-type star Gl 49 (BD+61 195)
including HARPS-N and CARMENES spectrographs, complemented by APT2 and
SNO photometry. Activity indices are calculated from the observed
spectra, and all datasets are analyzed with periodograms and noise
models. We investigated how the variation of stellar activity imprints
on our datasets. We further tested the origin of the signals and
investigate phase shifts between the different sets. To search for the
best-fit model we maximize the likelihood function in a Markov chain
Monte Carlo approach. Results: As a result of this study, we are
able to detect the super-Earth Gl 49b with a minimum mass of 5.6
M⊕. It orbits its host star with a period of 13.85 d at
a semi-major axis of 0.090 au and we calculate an equilibrium
temperature of 350 K and a transit probability of 2.0%. The contribution
from the spot-dominated host star to the different datasets is complex,
and includes signals from the stellar rotation at 18.86 d, evolutionary
timescales of activity phenomena at 40-80 d, and a long-term variation
of at least four years.
Based on observations made with the Italian TNG, operated on the island
of La Palma, Spain; the CARMENES instrument installed at the 3.5 m
telescope of the Calar Alto Observatory, Spain; the robotic APT2 located
at Serra La Nave on Mt. Etna, Italy; and the T90 telescope at Sierra
Nevada Observatory, Spain.Full Table A.1 is 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/624/A123
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