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dc.contributor.authorDamasso, M.
dc.contributor.authorBonomo, A. S.
dc.contributor.authorAstudillo-Defru, N.
dc.contributor.authorBonfils, X.
dc.contributor.authorMalavolta, L.
dc.contributor.authorSozzetti, A.
dc.contributor.authorLopez, E.
dc.contributor.authorZeng, L.
dc.contributor.authorHaywood, R. D.
dc.contributor.authorIrwin, J. M.
dc.contributor.authorMortier, A.
dc.contributor.authorVanderburg, A.
dc.contributor.authorMaldonado, J.
dc.contributor.authorLanza, A. F.
dc.contributor.authorAffer, L.
dc.contributor.authorAlmenara, J.-M.
dc.contributor.authorBenatti, S.
dc.contributor.authorBiazzo, K.
dc.contributor.authorBignamini, A.
dc.contributor.authorBorsa, F.
dc.contributor.authorBouchy, F.
dc.contributor.authorBuchhave, L. A.
dc.contributor.authorCameron, A. C.
dc.contributor.authorCarleo, I.
dc.contributor.authorCharbonneau, D.
dc.contributor.authorClaudi, R.
dc.contributor.authorCosentino, R.
dc.contributor.authorCovino, E.
dc.contributor.authorDelfosse, X.
dc.contributor.authorDesidera, S.
dc.contributor.authorDi Fabrizio, L.
dc.contributor.authorDressing, C.
dc.contributor.authorEsposito, M.
dc.contributor.authorFares, R.
dc.contributor.authorFigueira, P.
dc.contributor.authorFiorenzano, A. F. M.
dc.contributor.authorForveille, T.
dc.contributor.authorGiacobbe, P.
dc.contributor.authorGonzález-Álvarez, E.
dc.contributor.authorGratton, R.
dc.contributor.authorHarutyunyan, A.
dc.contributor.authorJohnson, J. Asher
dc.contributor.authorLatham, D. W.
dc.contributor.authorLeto, G.
dc.contributor.authorLopez-Morales, M.
dc.contributor.authorLovis, C.
dc.contributor.authorMaggio, A.
dc.contributor.authorMancini, L.
dc.contributor.authorMasiero, S.
dc.contributor.authorMayor, M.
dc.contributor.authorMicela, G.
dc.contributor.authorMolinari, E.
dc.contributor.authorMotalebi, F.
dc.contributor.authorMurgas, F.
dc.contributor.authorNascimbeni, V.
dc.contributor.authorPagano, I.
dc.contributor.authorPepe, F.
dc.contributor.authorPhillips, D. F.
dc.contributor.authorPiotto, G.
dc.contributor.authorPoretti, E.
dc.contributor.authorRainer, M.
dc.contributor.authorRice, K.
dc.contributor.authorSantos, N. C.
dc.contributor.authorSasselov, D.
dc.contributor.authorScandariato, G.
dc.contributor.authorSégransan, D.
dc.contributor.authorSmareglia, R.
dc.contributor.authorUdry, S.
dc.contributor.authorWatson, C.
dc.contributor.authorWünsche, A.
dc.date.accessioned2018-03-14T15:30:09Z
dc.date.available2018-03-14T15:30:09Z
dc.date.issued2018-07
dc.identifier.citationDamasso , M , Bonomo , A S , Astudillo-Defru , N , Bonfils , X , Malavolta , L , Sozzetti , A , Lopez , E , Zeng , L , Haywood , R D , Irwin , J M , Mortier , A , Vanderburg , A , Maldonado , J , Lanza , A F , Affer , L , Almenara , J-M , Benatti , S , Biazzo , K , Bignamini , A , Borsa , F , Bouchy , F , Buchhave , L A , Cameron , A C , Carleo , I , Charbonneau , D , Claudi , R , Cosentino , R , Covino , E , Delfosse , X , Desidera , S , Di Fabrizio , L , Dressing , C , Esposito , M , Fares , R , Figueira , P , Fiorenzano , A F M , Forveille , T , Giacobbe , P , González-Álvarez , E , Gratton , R , Harutyunyan , A , Johnson , J A , Latham , D W , Leto , G , Lopez-Morales , M , Lovis , C , Maggio , A , Mancini , L , Masiero , S , Mayor , M , Micela , G , Molinari , E , Motalebi , F , Murgas , F , Nascimbeni , V , Pagano , I , Pepe , F , Phillips , D F , Piotto , G , Poretti , E , Rainer , M , Rice , K , Santos , N C , Sasselov , D , Scandariato , G , Ségransan , D , Smareglia , R , Udry , S , Watson , C & Wünsche , A 2018 , ' Eyes on K2-3 : a system of three likely sub-Neptunes characterized with HARPS-N and HARPS ★ ' , Astronomy & Astrophysics , vol. 615 , A69 . https://doi.org/10.1051/0004-6361/201732459en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 252545285
dc.identifier.otherPURE UUID: 65dfdc59-c3c7-4231-8c46-665ed4404c05
dc.identifier.otherBibCode: 2018arXiv180208320D
dc.identifier.otherScopus: 85056663058
dc.identifier.otherORCID: /0000-0002-8863-7828/work/58531469
dc.identifier.otherWOS: 000439002800001
dc.identifier.urihttps://hdl.handle.net/10023/12942
dc.description.abstractContext. M-dwarf stars are promising targets for identifying and characterizing potentially habitable planets. K2-3 is a nearby (45 pc), early-type M dwarf hosting three small transiting planets, the outermost of which orbits close to the inner edge of the stellar (optimistic) habitable zone. The K2-3 system is well suited for follow-up characterization studies aimed at determining accurate masses and bulk densities of the three planets. Aims. Using a total of 329 radial velocity measurements collected over 2.5 years with the HARPS-N and HARPS spectrographs and a proper treatment of the stellar activity signal, we aim to improve measurements of the masses and bulk densities of the K2-3 planets. We use our results to investigate the physical structure of the planets. Methods. We analysed radial velocity time series extracted with two independent pipelines using Gaussian process regression. We adopted a quasi-periodic kernel to model the stellar magnetic activity jointly with the planetary signals. We used Monte Carlo simulations to investigate the robustness of our mass measurements of K2-3 c and K2-3 d, and to explore how additional high-cadence radial velocity observations might improve these values. Results. Even though the stellar activity component is the strongest signal present in the radial velocity time series, we are able to derive masses for both planet b (Mb = 6.6 ± 1.1 M⊕) and planet c (Mc = 3.1−1.2+1.3 M⊕). The Doppler signal from K2-3 d remains undetected, likely because of its low amplitude compared to the radial velocity signal induced by the stellar activity. The closeness of the orbital period of K2-3 d to the stellar rotation period could also make the detection of the planetary signal complicated. Based on our ability to recover injected signals in simulated data, we tentatively estimate the mass of K2-3 d to be Md = 2.7−0.8+1.2 M⊕ M⊕. These mass measurements imply that the bulk densities and therefore the interior structures of the three planets may be similar. In particular, the planets may either have small H/He envelopes (<1%) or massive water layers, with a water content ≥50% of their total mass, on top of rocky cores. Placing further constraints on the bulk densities of K2-3 c and d is difficult; in particular, we would not have been able to detect the Doppler signal of K2-3 d even by adopting a semester of intense, high-cadence radial velocity observations with HARPS-N and HARPS.
dc.format.extent14
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© 2018, ESO. This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1051/0004-6361/201732459en
dc.subjectStars: individual: K2-3 (2MASS 11292037-0127173, EPIC 201367065)en
dc.subjectPlanets and satellites: fundamental parametersen
dc.subjectPlanets and satellites: compositionen
dc.subjectTechniques: radial velocitiesen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleEyes on K2-3 : a system of three likely sub-Neptunes characterized with HARPS-N and HARPS★en
dc.typeJournal articleen
dc.contributor.sponsorEuropean Commissionen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews. St Andrews Centre for Exoplanet Scienceen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201732459
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2018arXiv180208320Den
dc.identifier.grantnumberen


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