J/A+A/686/L18ivo://CDS.VizieR/J/A+A/686/L18doi:10.26093/cds/vizier.36869018CDSSulis S.Borsato L.Grouffal S.Osborn H.P.Santerne A.Brandeker A.,Guenther M.N.Heitzmann A.Lendl M.Fridlund M.Gandolfi D.Alibert Y.,Alonso R.Barczy T.Barrado Navascues D.Barros S.C.C.Baumjohann W.,Beck T.Benz W.Bergomi M.Billot N.Bonfanti A.Broeg C.,Collier Cameron A.Corral van Damme C.Correia A.C.M.Csizmadia Sz.,Cubillos P.E.Davies M.B.Deleuil M.Deline A.Delrez L.,Demangeon O.D.S.Demory B.-O.Derekas A.Edwards B.Ehrenreich D.,Erikson A.Fortier A.Fossati L.Gazeas K.Gillon M.Guedel M.,Helling C.Hoyer S.Isaak K.G.Kiss L.L.Korth J.Lam K.W.F.,Laskar J.Lecavelier des Etangs A.Magrin D.Maxted P.F.L.Mordasini C.,Nascimbeni V.Olofsson G.Ottensamer R.Pagano I.Palle E.Peter G.,Piazza D.Piotto G.Pollacco D.Queloz D.Ragazzoni R.Rando N.,Rauer H.Ribas I.Santos N.C.Scandariato G.Segransan D.Simon A.E.,Smith A.M.S.Sousa S.G.Stalport M.Steinberger M.Szabo Gy.M.,Tuson A.Udry S.Ulmer-Moll S.Van Grootel V.Venturini J.Villaver E.,Walton N.A.Wilson T.G.Wolter D.Zingales T.2024-11-21T20:01:48Z2024-06-21T08:58:50ZCDS support team

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

cds-question@unistra.frmultiple-starsexoplanetsradial-velocityHIP 41378d is a long period planet that was observed to transit only twice, three years apart, with K2. According to stability considerations and a partial detection of the Rossiter-McLaughlin effect, the literature assessed Pd=278.36d as the most likely orbital period. We targeted HIP 41378d with CHEOPS at the predicted transit timing based on Pd=278.36d, but the observations show no transit. We find that large transit timing variations (TTV), larger than 22.4-hours (duration related to the CHEOPS observation window) could explain this non-detection. We also investigate the possibility of an incorrect orbital solution, which would have major implications for our knowledge of this system. If Pd!=278.36d, we find that the periods minimizing the eccentricity are 101.22d and 371.14d. The shortest orbital period will be tested by TESS, which will observe HIP 41378 in Sector 88 starting in January, 2025. Our study shows the importance of a mission like CHEOPS, which is today the only mission able to make long observations (i.e. from space) to track the ephemeris of long-period planets, possibly affected by large TTVs.2024A&A...686L..18Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/686/L18CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/686/L18https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/686/L18http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/686/L18https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/686/L18https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/686/L18http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/686/L18GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/686/L18/datasetCHEOPS observationsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTimeBaricentric Julian date (BJD)time.epochdoubleRFluxRelative flux before detrendingphot.flux;arith.ratiodoubleRFluxdet? Relative after before detrendingphot.flux;arith.ratiodoublenullablee_RFluxFlux errorstat.errordouble