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http://hdl.handle.net/20.500.12386/29481
Titolo: | HADES RV Programme with HARPS-N at TNG. VI. GJ 3942 b behind dominant activity signals | Autori: | Perger, M. Ribas, I. Damasso, Mario Morales, J. C. AFFER, Laura Suárez Mascareño, A. MICELA, Giuseppina MALDONADO PRADO, Jesus González Hernández, J. I. Rebolo, R. SCANDARIATO, GAETANO LETO, Giuseppe Zanmar Sanchez, R. BENATTI, SERENA BIGNAMINI, ANDREA BORSA, Francesco Carbognani, Albino CLAUDI, Riccardo DESIDERA, Silvano Esposito, M. Lafarga, M. Martinez Fiorenzano, A. F. Herrero, E. MOLINARI, Emilio Carlo NASCIMBENI, VALERIO PAGANO, Isabella Pedani, M. PORETTI, Ennio RAINER, Monica Rosich, A. SOZZETTI, Alessandro Toledo-Padrón, B. |
Data pubblicazione: | 2017 | Rivista: | ASTRONOMY & ASTROPHYSICS | Numero: | 608 | Da pagina:: | A63 | Abstract: | Context. Short- to mid-term magnetic phenomena on the stellar surface of M-type stars can resemble the effects of planets in radial velocity data, and may also hide them. <BR /> Aims: We analyze 145 spectroscopic HARPS-N observations of GJ 3942 taken over the past five years and additional photometry in order to disentangle stellar activity effects from genuine Doppler signals as a result of the orbital motion of the star around the common barycenter with its planet. <BR /> Methods: To achieve this, we use the common methods of pre-whitening, and treat the correlated red noise by a first-order moving average term and by Gaussian-process regression following an MCMC analysis. <BR /> Results: We identify the rotational period of the star at 16.3 days and discover a new super-Earth, GJ 3942 b, with an orbital period of 6.9 days and a minimum mass of 7.1 M<SUB>⊕</SUB>. An additional signal in the periodogram of the residuals is present, but at this point we cannot claim with sufficient significance that it is related to a second planet. If confirmed, this planet candidate would have a minimum mass of 6.3 M<SUB>⊕</SUB> and a period of 10.4 days, which might indicate a 3:2 mean-motion resonance with the inner planet. <P />Based on observations made with the Italian Telescopio Nazionale Galileo (TNG), operated on the island of La Palma by the INAF - Fundación Galileo Galilei at the Roque de los Muchachos Observatory of the Instituto de Astrofísica de Canarias (IAC); photometric observations from the APACHE array located at the Astronomical Observatory of the Aosta Valley; photometric observations made with the robotic APT2 (within the EXORAP program) located at Serra La Nave on Mt. Etna.Table 9 is only available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A> (<A href="http://130.79.128.5">http://130.79.128.5</A>) or via <A href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/608/A63">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/608/A63 | URI: | http://hdl.handle.net/20.500.12386/29481 | URL: | http://arxiv.org/abs/1709.06851v1 https://www.aanda.org/articles/aa/full_html/2017/12/aa31307-17/aa31307-17.html |
ISSN: | 0004-6361 | DOI: | 10.1051/0004-6361/201731307 | Bibcode ADS: | 2017A&A...608A..63P | Fulltext: | open |
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