J/A+A/640/A32ivo://CDS.VizieR/J/A+A/640/A32doi:10.26093/cds/vizier.36400032CDSHebrard G.Diaz R.F.Correia A.C.M.Collier Cameron A.Laskar J.,Pollacco D.Almenara J.-M.Anderson D.R.Barros S.C.C.Boisse I.,Bonomo A.S.Bouchy F.Boue G.Boumis P.Brown D.J.A.Dalal S.,Deleuil M.Demangeon O.Doyle A.P.Haswell C.A.Hellier C.Osborn H.,Kiefer F.Kolb U.C.Lam K.Lecavelier des Etangs A.Lopez T.,Martin-Lagarde M.Maxted P.McCormac J.Nielsen L.D.Palle E.,Prieto-Arranz J.Queloz D.Santerne A.Smalley B.Turner O.Udry S.,Verilhac D.West R.Wheatley P.J.Wilson P.A.2021-09-07T11:59:47Z2020-08-10T07:35:56ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frmultiple-starsradial-velocityWe 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 0.72R_Jup_ 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 0.40M_Jup_. 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 minutes, 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 0.60M_Jup_. 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.2020A&A...640A..32Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/640/A32CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/640/A32https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/640/A32http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/640/A32https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/640/A32https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/640/A32http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/640/A32GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/640/A32/table2SOPHIE measurements of WASP-148recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBJDBarycentric Julian Day (UTC) of the measurement (BJD-2450000)dtime.epochdoubleRVRadial velocitykm/sphys.veloc;pos.heliocentricfloate_RV1-sigma uncertainty of the radial velocitykm/sstat.errorfloatBISBisector spankm/sphys.velocfloatTimeExpExposure timestime.duration;obs.exposureintS/NSignal-to-noise ratio per pixel at 550nmstat.snrfloat