J/A+A/687/L1ivo://CDS.VizieR/J/A+A/687/L1doi:10.26093/cds/vizier.36879001CDSLeleu A.Delisle J.-B.Burn R.Izidoro A.Udry S.Dumusque X.,Lovis C.Millholland S.Parc L.Bouchy F.Bourrier V.Alibert Y.,Faria J.Mordasini C.Segransan D.2024-11-21T20:02:21Z2024-07-08T05:23:52ZCDS support team

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

cds-question@unistra.frmultiple-starsexoplanetsradial-velocitystellar-ageseffective-temperatureA systematic, population-level discrepancy exists between the densities of exoplanets whose masses have been measured with transit timing variations (TTVs) versus those measured with radial velocities (RVs). Since the TTV planets are predominantly nearly resonant, it is still unclear whether the discrepancy is attributed to detection biases or to astrophysical differences between the nearly resonant and non resonant planet populations. We defined a controlled, unbiased sample of 36 sub-Neptunes characterised by Kepler, TESS, HARPS, and ESPRESSO. We found that their density depends mostly on the resonant state of the system, with a low probability (of 0.002_-0.001_^+0.010^) that the mass of (nearly) resonant planets is drawn from the same underlying population as the bulk of sub-Neptunes. Increasing the sample to 133 sub-Neptunes reveals finer details: the densities of resonant planets are similar and lower than non-resonant planets, and both the mean and spread in density increase for planets that are away from resonance. This trend is also present in RV-characterised planets alone. In addition, TTVs and RVs have consistent density distributions for a given distance to resonance. We also show that systems closer to resonances tend to be more co-planar than their spread-out counterparts. These observational trends are also found in synthetic populations, where planets that survived in their original resonant configuration retain a lower density; whereas less compact systems have undergone post-disc giant collisions that increased the planet's density, while expanding their orbits. Our findings reinforce the claim that resonant systems are archetypes of planetary systems at their birth.2024A&A...687L...1Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/687/L1CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/AJ/154/5 : 145 Kepler planets transit timing variations (Hadden+, 2017)J/A+A/669/A117 : Mass-radius relationship of 34 Kepler planets (Leleu+, 2023)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/687/L1https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/687/L1http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/687/L1https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/687/L1https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/687/L1http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/687/L1GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/687/L1/sample (Full used in section 3 of the paper)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/687/L1/sample?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/687/L1/sample?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/687/L1/sample?GETtext/xml+votable180.050000true175.576558123.02685330.0055555555555555566/1036 3849 4673 7487 9038 11577 11724 11923 13644 14586 14591 14733-14734 14751 14753 14757 14768 14792 14824-14826 14896 14918 14924 14930 14932 14937 14939 14966 14973 14975 15060 15109 15115 15131 15134 15149 15170 15748 15973 16258 16347 16472 17089 17149 18147 18350 18361 18569 18574 18800 18881 19791 20667 21206 21270 22351 24587 25673 25699 25723 25725 26253 26278 26768 26977 26991 27358 27393 27787 28055 28279 28400 29349 32319 32433 32757 32811 33169 33210 33386 33972 36015 37947 38067 38946 40833 41941 43631 44272 44317 44474 45165 45172 47194 47488https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/687/L1?format=asciidefaultJ/A+A/687/L1/sampleFull used in section 3 of the paperSimbadNameSimbad column added by the CDSmeta.idcharnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNamePlanet namemeta.id;meta.maincharPerOrbital perioddtime.perioddoublee_PerOrbital period mean errordstat.errordoubleMasspPlanetary mass(5.97236x10+24kg)phys.massdoublee_MasspPlanetary mass mean error(5.97236x10+24kg)stat.errordoubleRadpPlanetary radius(6.3781x10+6m)phys.angSize;srcdoublee_RadpPlanetary radius mean error(6.3781x10+6m)stat.errordoubleDistresDistance to the resonance following eq. (1) of the paperpos.angDistancedoubleBibCodeBibCode of reference papermeta.bib.bibcodecharAutAuthor's name of reference papermeta.bib.authorcharTeqEquilibrium temperatureKphys.temperaturedoublee_TeqEquilibrium temperature mean errorKstat.errordoubleTeffStellar effective temperatureKphys.temperature.effectivefloate_TeffStellar effective temperature mean errorKstat.error;phys.temperature.effectivefloat[Fe/H]Stellar metallicityphys.abund.Zfloate_[Fe/H]Stellar metallicity mean errorstat.error;phys.abund.FedoubleAgeStellar ageGyrtime.agefloate_AgeStellar age mean errorGyrstat.error;time.agedoubleRadStellar radiussolRadphys.size.radiusfloat_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.main