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dc.contributor.authorHébrard, G.
dc.contributor.authorDíaz, R. F.
dc.contributor.authorCorreia, A. C. M.
dc.contributor.authorCollier Cameron, A.
dc.contributor.authorLaskar, J.
dc.contributor.authorPollacco, D.
dc.contributor.authorAlmenara, J.-M.
dc.contributor.authorAnderson, R.
dc.contributor.authorBarros, S. C. C.
dc.contributor.authorBoisse, I.
dc.contributor.authorBonomo, A. S.
dc.contributor.authorBouchy, F.
dc.contributor.authorBoué, G.
dc.contributor.authorBoumis, P.
dc.contributor.authorBrown, D. J. A.
dc.contributor.authorDalal, S.
dc.contributor.authorDeleuil, M.
dc.contributor.authorDemangeon, O. D. S.
dc.contributor.authorDoyle, A. P.
dc.contributor.authorHaswell, C. A.
dc.contributor.authorHellier, C.
dc.contributor.authorOsborn, H.
dc.contributor.authorKiefer, F.
dc.contributor.authorKolb, U. C.
dc.contributor.authorLam, K.
dc.contributor.authorLecavelier des Étangs, A.
dc.contributor.authorLopez, T.
dc.contributor.authorMartin-Lagarde, M.
dc.contributor.authorMaxted, P.
dc.contributor.authorMcCormac, J.
dc.contributor.authorNielsen, L. D.
dc.contributor.authorPallé, E.
dc.contributor.authorPrieto-Arranz, J.
dc.contributor.authorQueloz, D.
dc.contributor.authorSanterne, A.
dc.contributor.authorSmalley, B.
dc.contributor.authorTurner, O.
dc.contributor.authorUdry, S.
dc.contributor.authorVerilhac, D.
dc.contributor.authorWest, R.
dc.contributor.authorWheatley, P. J.
dc.contributor.authorWilson, P. A.
dc.identifier.citationHébrard , G , Díaz , R F , Correia , A C M , Collier Cameron , A , Laskar , J , Pollacco , D , Almenara , J-M , Anderson , R , Barros , S C C , Boisse , I , Bonomo , A S , Bouchy , F , Boué , G , Boumis , P , Brown , D J A , Dalal , S , Deleuil , M , Demangeon , O D S , Doyle , A P , Haswell , C A , Hellier , C , Osborn , H , Kiefer , F , Kolb , U C , Lam , K , Lecavelier des Étangs , A , Lopez , T , Martin-Lagarde , M , Maxted , P , McCormac , J , Nielsen , L D , Pallé , E , Prieto-Arranz , J , Queloz , D , Santerne , A , Smalley , B , Turner , O , Udry , S , Verilhac , D , West , R , Wheatley , P J & Wilson , P A 2020 , ' Discovery and characterization of the exoplanets WASP-148b and c : a transiting system with two interacting giant planets ' , Astronomy & Astrophysics , vol. 640 , A32 .
dc.identifier.otherBibCode: 2020A&A...640A..32H
dc.identifier.otherORCID: /0000-0002-8863-7828/work/79564691
dc.descriptionFunding: This work was supported by the “Programme National de Planétologie” (PNP) of CNRS/INSU, and the CNRS-PICS program between France and Argentina (PICS07826). A.C.M.C. acknowledges support by CFisUC strategic project (UID/FIS/04564/2019), ENGAGE SKA (POCI-01-0145-FEDER-022217), and PHOBOS (POCI-01-0145-FEDER-029932), funded by COMPETE 2020 and FCT, Portugal. O.D.S.D. acknowledges support from FCT and FEDER/COMPETE2020 in the form of the work contract DL57/2016/CP1364/CT0004 and the projects EPIC (PTDC/FIS-AST/28953/2017& POCI-01-0145-FEDER-028953) and GEANES (PTDC/FIS-AST/32113/2017- POCI-01-0145-FEDER-032113). This work is partly financed by the Spanish Ministry of Economics and Competitiveness through project ESP2016-80435-C2-2-R and PGC2018-098153-B-C31.en
dc.description.abstractWe present the discovery and characterization of WASP-148, a new extrasolar system that includes at least two giant planets. The host star is a slowly rotating inactive late-G dwarf with a V = 12 magnitude. The planet WASP-148b is a hot Jupiter of 0.72 RJup and 0.29MJup that transits its host with an orbital period of 8.80 days. We found the planetary candidate with the SuperWASP photometric survey, then characterized it with the SOPHIE spectrograph. Our radial velocity measurements subsequently revealed a second planet in the system, WASP-148c, with an orbital period of 34.5 days and a minimum mass of 0.40 MJup. No transits of this outer planet were detected. The orbits of both planets are eccentric and fall near the 4:1 mean-motion resonances. This configuration is stable on long timescales, but induces dynamical interactions so that the orbits differ slightly from purely Keplerian orbits. In particular, WASP-148b shows transit-timing variations of typically 15 min, making it the first interacting system with transit-timing variations that is detected on ground-based light curves. We establish that the mutual inclination of the orbital plane of the two planets cannot be higher than 35°, and the true mass of WASP-148c is below 0.60 MJup. We present photometric and spectroscopic observations of this system that cover a time span of ten years. We also provide their Keplerian and Newtonian analyses; these analyses should be significantly improved through future TESS observations.
dc.relation.ispartofAstronomy & Astrophysicsen
dc.subjectPlanetary systemsen
dc.subjectTechniques: radial velocitiesen
dc.subjectTechniques: photometricen
dc.subjectTechniques: spectroscopicen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleDiscovery and characterization of the exoplanets WASP-148b and c : a transiting system with two interacting giant planetsen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews. St Andrews Centre for Exoplanet Scienceen
dc.description.statusPeer revieweden

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