J/A+A/699/A185ivo://CDS.VizieR/J/A+A/699/A185doi:10.26093/cds/vizier/bc-nv/lbifCDSSchmerling H.Goffo E.Grziwa S.Persson C.M.Gandolfi D.Paetzold M.,Hatzes A.Hellier C.Livingston J.Acuna L.Aguichine A.Costanza E.,Deeg H.J.Masseron T.Palle E.Cochran W.Nowak G.Jankowski D.,Gozdziewski K.Luque R.Mathur S.Palakkatharappil D.B.Garcia R.A.2026-08-03T06:55:32Z2025-07-11T07:15:29ZCDS support team

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

cds-question@unistra.frmultiple-starsexoplanetsk-starsradial-velocityvisible-astronomyUsing high-precision photometry, NASA's TESS space mission has discovered many intriguing transiting planet candidates. These discoveries require ground-based follow-up observations, including high-precision Doppler spectroscopy, to rule out false positive scenarios and measure the mass of the transiting planets. In this study, we present an intensive Doppler follow-up campaign of the TESS object of interest TOI-2427, carried out with the High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph to determine the mass of the previously validated transiting planet (TOI-2427 b) and search for additional orbiting companions. By analyzing TESS transit photometry alongside our HARPS radial velocity measurements, we spectroscopically confirmed the transiting planet TOI-2427 b, which orbits its host star every ~1.3d. We also discovered the presence of a second non-transiting planetary companion with an orbital period of ~5.15d, which is very close to four times the orbital period of the inner transiting planet. We found that TOI-2427 b is a short-period, high-density super-Earth with a mass of Mb=5.69_-0.50_^+0.51^M_{Earth}_ and a radius of Rb=1.64_-0.11_^+0.12^R_{Earth}_, implying a mean density of {rho}b=7.1_-0.4_^+0.8^g/cm^3^. Its interior seems to be composed of a predominantly iron core and a silicate mantle and crust. Despite its high density, it is unlikely that TOI-2427 b can sustain any atmosphere composed of lighter gases; however, it could still retain heavier gases. The outer non-transiting planet TOI-2427 c has a minimum mass of Mc sin ic = 6.46-0.78+0.79 M_{Earth}_. Assuming that TOI-2427 b and c are coplanar, a statistical analysis suggests that planets with a mass of ~6.5M_{Earth}_ tend to have radii around 2.7_-0.8_^+1.1^R_{Earth}_. This would place TOI-2457 c near the sub-Neptune regime, while also leaving open the possibility of it being a super-Earth.2025A&A...699A.185Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/699/A185CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/699/A185https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/699/A185http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/699/A185https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/699/A185https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/699/A185http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/699/A185GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/699/A185/tablea1HARPS RV measurementsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBJDBarycentric Julian date (TDB)dtime.epochdoubleRV-DRSHARPS DRS radial velocitykm/sphys.veloc;pos.heliocentricdoublee_RV-DRSHARPS DRS radial velocity uncertaintykm/sstat.errordoubleRV-TERRATERRA relative radial velocitykm/sphys.veloc;pos.heliocentricdoublee_RV-TERRATERRA relative radial velocity uncertaintykm/sstat.errordoubleRV-SERVALSERVAL relative radial velocitykm/sphys.veloc;pos.heliocentricdoublee_RV-SERVALSERVAL relative radial velocity uncertaintykm/sstat.errordoubleBISBisector inverse slopekm/sphys.velocdoubleFWHMFull width at half-maximumkm/sspect.line.widthdoubleJ/A+A/699/A185/tablea2HARPS activity indicatorsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBJDBarycentric Julian date (TDB)dtime.epochdoubleContrastDepth of cross-correlation function as percentage%phot.flux;arith.ratiodoubledLWDifferential line widthm**2.s**-2spect.line.widthdoublee_dLWdLW uncertaintym**2.s**-2stat.errordoubleCRXChromatic Index of the Radial Velocitym/sspect.indexdoublee_CRXCRX uncertaintym/sstat.errordoubleSIndexChromosperic activity indexspect.indexdoublee_SIndexS-Index uncertaintystat.errordoubleHalphaEmission in the H-alpha line0.1nmspect.index;em.line.HalphadoubleNaD1Emission in the NaD1 line0.1nmspect.indexdoubleNaD2Emission in the NaD2 line0.1nmspect.indexdoubleSNRSignal to noise ratio at 550nmstat.snrfloat