The HADES RV Programme with HARPS-N at TNG XI. GJ 685 b: a warm super-Earth around an active M dwarf
| Autor: | Pinamonti, M., Sozzetti, A., Giacobbe, P., Damasso, M., Scandariato, G., Perger, M., Hernández, J. I. González, Lanza, A. F., Maldonado, J., Micela, G., Mascareño, A. Suárez, Toledo-Padrón, B., Affer, L., Benatti, S., Bignamini, A., Bonomo, A. S., Claudi, R., Cosentino, R., Desidera, S., Maggio, A., Fiorenzano, A. Martinez, Pagano, I., Piotto, G., Rainer, M., Rebolo, R., Ribas, I. |
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| Rok vydání: | 2019 |
| Předmět: | |
| Zdroj: | A&A 625, A126 (2019) |
| Druh dokumentu: | Working Paper |
| DOI: | 10.1051/0004-6361/201834969 |
| Popis: | Small rocky planets seem to be very abundant around low-mass M-type stars. Their actual planetary population is however not yet precisely understood. Currently several surveys aim to expand the statistics with intensive detection campaigns, both photometric and spectroscopic. We analyse 106 spectroscopic HARPS-N observations of the active M0-type star GJ 685 taken over the past five years. We combine these data with photometric measurements from different observatories to accurately model the stellar rotation and disentangle its signals from genuine Doppler planetary signals in the RV data. We run an MCMC analysis on the RV and activity indexes time series to model the planetary and stellar signals present in the data, applying Gaussian Process regression technique to deal with the stellar activity signals. We identify three periodic signals in the RV time series, with periods of 9, 24, and 18 d. Combining the analyses of the photometry of the star with the activity indexes derived from the HARPS-N spectra, we identify the 18 d and 9 d signals as activity-related, corresponding to the stellar rotation period and its first harmonic respectively. The 24 d signals shows no relations with any activity proxy, so we identify it as a genuine planetary signal. We find the best-fit model describing the Doppler signal of the newly-found planet, GJ 685\,b, corresponding to an orbital period $P_b = 24.160^{+0.061}_{-0.047}$ d and a minimum mass $M_P \sin i = 9.0^{+1.7}_{-1.8}$ M$_\oplus$. We also study a sample of 70 RV-detected M-dwarf planets, and present new statistical evidence of a difference in mass distribution between the populations of single- and multi-planet systems, which can shed new light on the formation mechanisms of low-mass planets around late-type stars. Comment: 18 pages, 13 figures, accepted for publication in A&A |
| Databáze: | arXiv |
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