J/A+A/691/A233ivo://CDS.VizieR/J/A+A/691/A233doi:10.26093/cds/vizier.36910233CDSCastro-Gonzalez A.Lillo-Box J.Armstrong D.J.Acuna L.Aguichine A.,Bourrier V.Gandhi S.Sousa S.G.Delgado-Mena E.Moya A.Adibekyan V.,Correia A.C.M.Barrado D.Damasso M.Winn J.N.Santos N.C.Bakaoui K.,Barros S.C.C.Benkhaldoun Z.Bouchy F.Briceno C.Caldwell D.A.,Collins K.A.Essack Z.Ghachoui M.Gillon M.Hounsell R.Jehin E.,Jenkins J.M.Keniger M.A.F.Law N.Mann A.W.Nielsen L.D.,Pozuelos F.J.Schanche N.Seager S.Tan T.-G.Timmermans M.,Villasenor J.Watkins C.N.Ziegler C.2025-02-18T20:02:04Z2024-11-15T10:01:50ZCDS support team

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

cds-question@unistra.frmultiple-starsexoplanetsphotometryvisible-astronomyradial-velocityThe Neptunian desert and savanna have been recently found to be separated by a ridge, an overdensity of planets in the ~3-5 days period range. These features are thought to be shaped by dynamical and atmospheric processes. However, their relative roles are not yet well understood. We intend to confirm and characterise the super-Neptune TESS candidate TOI-5005.01, which orbits a moderately bright (V=11.8) solar-type star (G2 V) with an orbital period of 6.3 days. With such properties, TOI-5005.01 is located in the Neptunian savanna near the ridge. We used Bayesian inference to analyze 38 HARPS radial velocity measurements, three sectors of TESS photometry, and two PEST and TRAPPIST-South transits. We tested a set of models involving eccentric and circular orbits, long-term drifts, and Gaussian processes to account for correlated stellar and instrumental noise. We computed the Bayesian evidences to find the model that best represents our data set and infer the orbital and physical properties of the system. We confirm TOI-5005~b to be a transiting super-Neptune with a radius of Rp_=6.25+/-0.24R_{Earth} (R_p_=0.558+/-0.021R_Jup_) and a mass of M_p_=32.7+/-5.9M_{Earth} (M_p=0.103+/-0.018M_Jup_), which corresponds to a mean density of rho_p_=0.74+/-0.16g/cm^3^. Our internal structure modelling indicates that the core mass fraction (CMF=0.74^+0.05^_-0.45_) and envelope metal mass fraction (Z_env_=0.08^+0.41^_-0.06_) of TOI-5005 b are degenerate, but the overall metal mass fraction is well constrained to a value slightly lower than that of Neptune and Uranus (Z_planet_=0.76^+0.04^_-0.11_). The Z_planet_/Z_star_ ratio is consistent with the well-known mass-metallicity relation, which suggests that TOI-5005~b was formed via core accretion. We also estimated the present-day atmospheric mass-loss rate of TOI-5005 b but found contrasting predictions depending on the choice of photoevaporation model (0.013+/-0.008M_{Earth}_/Gyr versus 0.17+/-0.12M_{Earth}_/Gyr). At a population level, we find statistical evidence (p-value =0.0092^+0.0184^_-0.0066_) that planets in the savanna such as TOI-5005 b tend to show lower densities than planets in the ridge, with a dividing line around 1g/cm^-3^, which supports the hypothesis of different evolutionary pathways populating both regimes. TOI-5005 b is located in a key region of the period-radius space to study the transition between the Neptunian ridge and the savanna. It orbits the brightest star of all such planets known today, which makes it a target of interest for atmospheric and orbital architecture observations that will bring a clearer picture of its overall evolution.2024A&A...691A.233Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/691/A233CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/691/A233https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/691/A233http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/691/A233https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/691/A233https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/691/A233http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/691/A233GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/691/A233/tablec1TESS Simple Aperture Photometry (SAP) of TOI-5005 (Sectors 12, 39, and 65)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBJDBaricentric Julian datedtime.epochdoubleindexedSAPTESS Simple Aperture Photometry (SAP) normalized fluxphot.flux;arith.ratiodoublee_SAPTESS Simple Aperture Photometry (SAP) normalized flux errorstat.errordoubleSectorTESS Sectorobs.fieldcharJ/A+A/691/A233/tablec2TESS QLP (Sector 12) and PDCSAP (Sectors 39 and 65) photometry of TOI-5005recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBJDBaricentric Julian datedtime.epochdoubleindexedQLP/PDCSAP? TESS QLP (Sector 12) and PDCSAP (Sectors 39 and 65) normalized fluxphot.flux;arith.ratiodoublenullablee_QLP/PDCSAPTESS QLP (Sector 12) and PDCSAP (Sectors 39 and 65) normalized flux errorstat.errordoubleSectorTESS Sectorobs.fieldcharJ/A+A/691/A233/tablec3PEST photometry of TOI-5005 corresponding to a transit of TOI-5005 bYcoordY coordinate of the target in the CCDpos.cartesian.ydoubleDistCenterDistance to the center of the CCDpos;arith.diffdoubleFWHMFull width at half maximum (FWHM) of the Point Spread Function (PSF)spect.line.widthfloatAirMassAirmassobs.airMassfloatSkyBackground fluxinstr.backgrounddoubleENSavgAverage ENSstat.fit.paramfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBJDBaricentric Julian date (TDB)dtime.epochdoubleFluxPEST normalized fluxphot.flux;arith.ratiofloate_FluxPEST normalized flux errorstat.error;phot.fluxfloatVarFluxNormalised PEST flux so that its mean is 1phot.flux;arith.ratiofloatCompFluxNormalized PEST flux of a comparison field star so that its mean is 1phot.flux;arith.ratiofloatXcoordX coordinate of the target in the CCDpos.cartesian.xdoubleJ/A+A/691/A233/tablec4TRAPPIST-South photometry of TOI-5005 corresponding to a transit of TOI-5005 brecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintdFluxTRAPPIST-South differential fluxphot.flux;arith.ratiodoublee_dFluxTRAPPIST-South differential flux errorstat.errordoubledXmoveDisplacement of the target in the CCD across the X axispos.angDistancedoubledYmoveDisplacement of the target in the CCD across the Y axispos.angDistancedoubleFWHMFull width at half maximum (FWHM) of the Point Spread Function (PSF)spect.line.widthdoubleFWHMXFull width at half maximum (FWHM) of the Point Spread Function (PSF) across the X axisspect.line.widthdoubleFWHMYFull width at half maximum (FWHM) of the Point Spread Function (PSF) across the Y axisspect.line.widthdoubleSkyLevelBackground fluxinstr.backgrounddoubleAirMassAirmassobs.airMassdoubleExpTimeExposure timestime.duration;obs.exposurefloatBJDBaricentric Julian date (TDB)dtime.epochdoubleJ/A+A/691/A233/tablec5HARPS radial velocities of TOI-5005 obtained under the programs 108.21YY.001 and 108.21YY.002 (PI: Armstrong)e_ContrastError of the contrast of the cross-correlation function (CCF)%stat.errorfloate_HaH{alpha} line depth errorstat.errordoubleContrastContrast of the cross-correlation function (CCF)%phot.flux;arith.ratiodoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintJDReduced Julian date (JD-2400000)dtime.epochdoubleRVRadial velocitym/sphys.veloc;pos.heliocentricdoublee_RVRadial velocity errorm/sstat.errordoubleFWHMFull width at half maximum (FWHM) of the cross-correlation function (CCF)m/sstat.correlationdoublee_FWHMError of the full width at half maximum (FWHM) of the cross-correlation function (CCF)m/sstat.error;phys.angSizedoubleSMWS-indexphot.flux;arith.ratiodoublee_SMWS-index errorstat.errordoubleCaCalcium line depthspect.indexdoublee_CaCalcium line depth errorstat.errordoubleHaH{alpha} line depthphys.absorption.opticalDepth;spect.linedouble