J/A+A/701/A153ivo://CDS.VizieR/J/A+A/701/A153doi:10.26093/cds/vizier/bc-nx/lbfdCDSSharma A.Stonkute E.Drazdauskas A.Minkeviciute R.Mikolaitis S.,Tautvaisiene G.Jonauskaite U.2026-08-03T06:57:03Z2025-09-15T09:49:43ZCDS support team

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

cds-question@unistra.frmultiple-starsexoplanetschemical-abundancesvisible-astronomyWe present neutron-capture element abundances for a homogeneous sample of 160 FGK-type planet-hosting stars (32 of them are multiplanetary systems). These stars host a total of 175 high-mass planets and 47 Neptunian and Super-Earth planets. Spectra were obtained with the Vilnius University Echelle Spectrograph (VUES) associated with a 1.65m telescope installed at Moletai Astronomical Observatory. The analysed elements include Sr, Y, Zr, Ba, La, Ce, Pr, Nd, and Eu. Abundances were derived using synthetic spectral fitting with the TURBOSPECTRUM code and MARCS model atmospheres under LTE, with NLTE corrections applied for Sr, Y, Ba and Eu. The dataset includes stellar parameters, and individual elemental abundances ([El/H]). We investigate the trends of [El/Fe] with [Fe/H] and planet mass, and examine condensation temperature (T_cond_) trends ({DELTA}[El/H]-T_cond_> slopes) for potential star-planet chemical signatures. The results show that most neutron-capture elements trace Galactic chemical evolution, but [Zr/Fe], [La/Fe], and [Ce/Fe] are enhanced in stars with planets compared to reference stars at a given [Fe/H]. Positive correlations between [El/Fe] and planet mass are observed towards higher-mass planets for most elements excluding strontium, yttrium, and barium, which exhibit insignificant correlations across all subsamples. The {DELTA}[El/H]-T_cond_ slopes suggest a possible enrichment of refractory elements in planet-hosting stars, especially in younger and less metal-rich systems. While strong correlations between {DELTA}[El/H]-T_cond_ slopes and stellar or planetary parameters are not observed, the data suggest some notable trends. Older dwarf stars hosting multiple planets tend to exhibit smaller or even negative {DELTA}[El/H]-T_cond_ slopes, whereas younger dwarfs show larger positive slopes, indicating a possible age-dependent chemical signature. Additionally, we find that multiplanetary systems are more frequently associated with metal-rich stars. This dataset supports ongoing efforts to understand the chemical signatures associated with planet formation.2025A&A...701A.153Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/701/A153CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/691/A160 : Chemical composition of planetary hosts (Sharma+, 2024)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/701/A153https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/701/A153http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/701/A153https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/701/A153https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/701/A153http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/701/A153GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/701/A153/tableb1 (Stellar physical and chemical properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/701/A153/tableb1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/701/A153/tableb1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/701/A153/tableb1?GETtext/xml+votable180.050000true298.56200648.46145420.0055555555555555566/311 341 679 717 748 1201 1597 2152 2254 2312 2472 2497 2577 2579 2971 3118 3350 3663 3906 3932 3979 4082 4735 4881 5009 5067 5309 5522 5553 5556 5572 5718 5815 6006 6217 6219 6298 6760 6791 6831 7136 7162 7402 7760 7786 8109 8319 8478 8671 8785 9061 9350 9403 9459 9483 9662 9753 9843 9893 9934 10004 10061 10079 10217 10278 10490 10550 11087 11326 11352 11394 11473 11589 11598 11699 11732 11734 11756 11910 11931 11987 12030 12056 12082-12083 12117 12146 12148 12186 12352 12465 12482 12592 12612 12644 12646 12899 12983 13643 13808 14278 14329 14419 14434 14466 14516 14525 14548 14568 14682 14896 14918 14957 15030 15174 15177 15273 15973 16035 16096 16135 16213 16342 17731 18164 20020 20145 20338 22518 22878 23030 23201 24019 24312 26120 26440 26521 26575 27616 27750 27975 28044 28085 28103 28130 28274 28392 28400 29589 30170 30176 30541 30707 31428 31478 31606 31689 32509 32561 32575https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/701/A153?format=asciiOpticaldefaultJ/A+A/701/A153/tableb1Stellar physical and chemical propertiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTYCTycho-2 catalogue identificationmeta.id;meta.maincharTeffEffective temperatureKphys.temperature.effectiveinte_TeffUncertainty in effective temperatureKstat.error;phys.temperature.effectiveintloggStellar surface gravitylog(cm.s**-2)phys.gravityfloate_loggUncertainty in stellar surface gravitylog(cm.s**-2)stat.errorfloat[Fe/H]Metallicityphys.abundfloate_[Fe/H]Uncertainty in metallicitystat.error;phys.abund.FefloatVtMicroturbulence velocitykm/sphys.veloc.microTurbfloate_VtUncertainty in microturbulence velocitykm/sstat.errorfloat[Sr/H]? Strontium abundancephys.abundfloatnullablee_[Sr/H]? Uncertainty in Sr abundancestat.error;phys.abundfloatnullable[Y/H]? Yttrium abundancephys.abundfloatnullablee_[Y/H]? Uncertainty in Y abundancestat.error;phys.abundfloatnullable[ZrI/H]? Zirconium (neutral) abundancephys.abundfloatnullablee_[Nd/H]? Uncertainty in Nd abundancestat.error;phys.abundfloatnullable[Eu/H]? Europium abundancephys.abundfloatnullablee_[Eu/H]? Uncertainty in Eu abundancestat.error;phys.abundfloatnullableSimbadSimbad column added by the CDSmeta.ref.urlchar_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.maine_[ZrI/H]? Uncertainty in ZrI abundancestat.error;phys.abundfloatnullable[ZrII/H]? Zirconium (ionised) abundancephys.abundfloatnullablee_[ZrII/H]? Uncertainty in ZrII abundancestat.error;phys.abundfloatnullable[Ba/H]? Barium abundancephys.abundfloatnullablee_[Ba/H]? Uncertainty in Ba abundancestat.error;phys.abundfloatnullable[La/H]? Lanthanum abundancephys.abundfloatnullablee_[La/H]? Uncertainty in La abundancestat.error;phys.abundfloatnullable[Ce/H]? Cerium abundancephys.abundfloatnullablee_[Ce/H]? Uncertainty in Ce abundancestat.error;phys.abundfloatnullable[Pr/H]? Praseodymium abundancephys.abundfloatnullablee_[Pr/H]? Uncertainty in Pr abundancestat.error;phys.abundfloatnullable[Nd/H]? Neodymium abundancephys.abundfloatnullable