J/A+A/709/A265ivo://CDS.VizieR/J/A+A/709/A265CDSBonfanti A.Gandolfi D.Leonardi P.Osborn H.P.Serrano L.M.,Hebrard G.Billot N.Bekkelien A.Olofsson G.Broeg C.Nardiello D.,Sousa S.G.Wilson T.G.Correia A.C.M.Pezzotti C.Brandeker A.,Fossati L.Gillon M.Stalport M.Akinsanmi B.Alibert Y.Alonso R.,Asquier J.Barczy T.Barrado D.Barros S.C.C.Baumjohann W.Benz W.,Borsato L.Castro-Gonzalez A.Collier Cameron A.Csizmadia Sz.,Cubillos P.E.Davies M.B.Deleuil M.Delfosse X.Deline A.,Demangeon O.D.S.Demory B.-O.Derekas A.Destriez F.Edwards B.,Ehrenreich D.Erikson A.Fortier A.Fridlund M.Gazeas K.Gudel M.,Gunther M.N.Hara N.Heidari N.Heitzmann A.Helling C.Isaak K.G.,Keller T.Kiss L.L.Kitzmann D.Korth J.Lacedelli G.Lam K.W.F.,Laskar J.Lecavelier des Etangs A.Leleu A.Lendl M.Magrin D.,Maxted P.F.L.Mecina M.Merin B.Mordasini C.Nascimbeni V.,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.,Sulis S.Szabo Gy.M.Udry S.Ulmer-Moll S.Van Grootel V.,Venturini J.Verrecchia F.Villaver E.Walton N.A.Wolf S.,Wolter D.Zingales T.2026-05-22T09:10:21Z2026-05-22T10:08:28ZCDS support team

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

cds-question@unistra.frmultiple-starsexoplanetsphotometryradial-velocityspectroscopyvisible-astronomyinfrared-astronomyline-intensitiesFollowing the 2022 alert of a TESS object of interest transiting TOI-5624 (a G7, Vstar ~100pc away), a CHEOPS campaign in 2023 detected four planetary signals at P_b_~3.4, P_c_~7.9, P_d_~13.7, and P_e_~21.5 days, later confirmed by additional TESS and CHEOPS photometry in 2024-2025. By using TESS and CHEOPS photometry along with HARPS-N and SOPHIE high-resolution spectra, we determined the planet properties and performed a dynamical analysis of the system. After analysing the photometric data, we extracted and modelled the radial velocity (RV) time series using two independent methodologies both within a Markov chain Monte Carlo framework. We further integrated the N-body equations of motion, while simultaneously fitting the transit times and the detrended RVs, to dynamically characterise the system. We present the discovery of four transiting sub-Neptunes with radii of R_b_=2.314+/-0.035R_{Earth}_, R_c_=2.474+/-0.042R_{Earth}_, R_d_=3.584_-0.050_^+0.051^ R_{Earth}_, and R_e_=3.247_-0.043_^+0.042^ R_{Earth}_ and masses of M_b_=9.4+/-1.4M_{Earth}_, M_c_=4.8+/-1.9M_{Earth}, M_d_=4.9+/-2.2M_{Earth}_, and M_e_=8.9_-3.0_^+2.9^M_{Earth}_. Our photometric analysis reveals that the outermost transiting planet TOI-5624e shows significant transit time variations (TTVs). Indeed, we find a robust Keplerian signal in the RV time series close to the 2:1 period commensurability with TOI-5624e, which explains the TTV pattern exhibited by TOI-5624e according to our dynamical analysis. We label this non-transiting planet as TOI-5624f and find its minimum mass to be M_f_*sini_f_=13.0+/-3.7M_{Earth}_. Among the known systems hosting more than four planets, the remarkable precision with which the radii have been measured (<1.7%) and the firm assessment (>3{sigma}) of the mass for at least three planets has been previously reached only for TRAPPIST-1. Additional photometric observations will enable a better sample of the TTV modulation and a more robust dynamical determination of the masses.2026A&A...709A.265Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/709/A265CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/709/A265https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/709/A265http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/709/A265https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/709/A265https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/709/A265http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/709/A265GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticalInfrareddefaultJ/A+A/709/A265/tablea1RV time series extracted from HARPS-NrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBJDObservation time as BJD TDB (BJD-2450000)dtime.epochdoubleRVRVs extracted from HARPS-N CCFs as SN fitm/sphys.veloc;pos.heliocentricfloate_RVErrors on the RVsm/sstat.errorfloatFWHM-SNFWHM of the fitted skew-Normal functionkm/sspect.line.widthfloatHaH-alpha inferred from spectra0.1nmem.line.HalphafloatgammaSkewness of the fitted skew-Normal functionstat.fit.paramfloatNaD2NaD2 inferred from spectra0.1nmspect.indexfloatRVdDetrended normalized RVsm/sphys.veloc;pos.heliocentricfloate_RVdErrors on the detrended RVs with jitter effect includedm/sstat.errorfloatJ/A+A/709/A265/tablea2RV time series extracted from SOPHIErecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBJDObservation time as BJD TDB (BJD-2450000)dtime.epochdoubleRVRVs extracted from SOPHIE CCFs as Gaussian fitm/sphys.veloc;pos.heliocentricfloate_RVError on the RVm/sstat.errorfloatFWHMFWHM of the fitted Gaussiankm/sspect.line.widthfloatAContrast of the fitted Gaussian%stat.fit.paramfloatBisBisector inferred from the fitted Gaussianstat.fit.paramfloatlogRHKlogRHK inferred from spectraphot.flux;arith.ratiofloatRVdDetrended normalized RVm/sphys.veloc;pos.heliocentricfloate_RVdError on the detrended RV jitter includedm/sstat.errorfloatJ/A+A/709/A265/listCHEOPS detrended LCs file listrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintFileNameLC file name in lc directorymeta.id;meta.filecharLCLight curvesmeta.ref.urlcharBJDminMinimum observation time as BJD TDB (JD-2450000)dtime.epoch;stat.mindoubleBJDmaxMaximum observation time as BJD TDB (JD-2450000)dtime.epoch;stat.maxdouble