J/A+A/580/A24ivo://CDS.VizieR/J/A+A/580/A24doi:10.26093/cds/vizier.35800024CDSda Silva R.Milone A.C.Rocha-Pinto H.J.2017-06-27T06:37:52Z2015-07-23T08:47:38ZCDS support team

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

cds-question@unistra.frchemical-abundancesspectroscopyWe have analyzed high-resolution and high signal-to-noise ratio optical spectra of nearby FGK stars with and without detected giant planets in order to homogeneously measure their photospheric parameters, mass, age, and the abundances of volatile (C, N, and O) and refractory (Na, Mg, Si, Ca, Ti, V, Mn, Fe, Ni, Cu, and Ba) elements. Our sample contains 309 stars from the solar neighborhood (up to the distance of 100pc), out of which 140 are dwarfs, 29 are subgiants, and 140 are giants. The photospheric parameters are derived from the equivalent widths (EWs) of FeI and FeII lines. Masses and ages come from the interpolation in evolutionary tracks and isochrones on the HR diagram. The abundance determination is based on the equivalent widths of selected atomic lines of the refractory elements and on the spectral synthesis of C_2_, CN, CI, OI, and NaI features. We apply a set of statistical methods to analyze the abundances derived for the three subsamples. Our results show that: i) giant stars systematically exhibit underabundance in [C/Fe] and overabundance in [N/Fe] and [Na/Fe] in comparison with dwarfs, a result that is normally attributed to evolution-induced mixing processes in the envelope of evolved stars; ii) for solar analogs only, the abundance trends with the condensation temperature of the elements are correlated with age and anticorrelated with the surface gravity, which is in agreement with recent studies; iii) as in the case of [Fe/H], dwarf stars with giant planets are systematically enriched in [X/H] for all the analyzed elements, except for O and Ba (the former due to limitations of statistics), confirming previous findings in the literature that not only iron has an important relation with the planetary formation; and iv) giant planet hosts are also significantly overabundant for the same metallicity when the elements from Mg to Cu are combined together.2015A&A...580A..24Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/580/A24CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/526/A71 : C abundances in G and K nearby stars (da Silva+, 2011)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/580/A24https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/580/A24http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/580/A24https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/580/A24https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/580/A24http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/580/A24GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/580/A24/stars (Stars analyzed: photospheric parameters, abundances, and evolution parameters)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/580/A24/stars?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/580/A24/stars?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/580/A24/stars?GETtext/xml+votable180.050000true44.444468929.66145940.0055555555555555566/60 100 210 215 309 311 322 341 377 428 587 684 737 742 748 871 915 917 944 1032 1042 1249 1341 1452 1819 1827 1960 2110 2167 2169 2324 2433 2472 2476 2541 2828 2923 3020 3026 3102 3258 3313 3335 3390 3511 3619 3639 3691 3697 3755 3979 4051 4079 4129 4146 4227 4444 4969 4985 5009 5053 5059 5413 5522 5530 5676 5726 5815 5950 5983 6166 6203 6217 6219 6334 6385 6493 6827 6933 7006 7039 7052 7113 7131 7177 7320 7466 7760 7763 7771 8080 8357 8716 8845 9061 9083 9127 9213 9219 9337 9403 9610 9753 9801 9835 10101 10184 10354 10375 10632 10899 11150 11165 11326 11394 11412 11473 11659 11735 12208 12337 12464 12592 12634 12644 12654 12792 12856 12890 12944 13025 13114 13158 13282 13333 13487 13643 13731 13749 13778 13791 14005 14013 14109 14220 14278 14290 14329 14416 14434 14502 14534 14604 14630 14650 14693 14767 15174 15363 15373 15597 15715 15727 16013 16023 16031 16035 16056 16069 16213 16883 16895 17061 17159 17171 17219 17266 17573 17587 17606 17656 17731 17764 17847 17852 17860 18123 18688 18802 18821 18915 18972 19237 19718 19799 19868 19912 20145 20308 20402 20973 21089 21273 21423 21484 21612 21696 21768 21829 21940 22036 22157 22199 22330 22340 22354-22355 22654 22878 22900 22932 23030 23096 23190 23201 23230 23479 23533 23537-23539 23547-23548 23575 23583 23661 23695 23774 23843 24117 24151 24262 24558 24924 25444 25567 25571 25608 25906 25939 26562 26575 27014 27040 27088 27179 27255 27386 27752 27975 28104 28276 28400 28436 28487 29712 29765 30015 30123 30339 30437 30529 30576 30665 30878 31172 31204 31393 31399 31416 31433 31444 31478 31796 31821 32045 32067 32096 32328 32348 32509 32575 32633 32645 36664 36693 36697 38733 40355 40618 40644 40827 40932 48943 48980 49114https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/580/A24?format=asciiOpticaldefaultJ/A+A/580/A24/table8Slopes of the linear regressions on [X/Fe] vs. TcNameHD, BD, or HIP stellar numbermeta.number;phys.atmol.numbercharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintslope0Slope of the regressions before CCE (1)stat.fit.paramdoublee_slope0Error in the slopesstat.errordoubler0[-1/1] Correlation coefficientstat.correlationfloatstd0[0.01/0.15] Standard deviation of regressionsstat.stdevfloatslope1Slope of the regression after CCE, age-based (1)stat.fit.paramdoublee_slope1Error in the slopesstat.errordoubler1[-1/1] Correlation coefficientstat.correlationfloatstd1[0.02/0.15] Standard deviation of regressionsstat.stdevfloatslope2Slope of the regression after CCE, [Fe/H]-based (1)stat.fit.paramdoublee_slope2Error in the slopesstat.errordoubler2[-1/1] Correlation coefficientstat.correlationfloatstd2[0.01/0.13] Standard deviation of regressionsstat.stdevfloatJ/A+A/580/A24/table3Atomic parameters for lines with important hyperfine structurerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintLineAtomic line identificationmeta.id;spect.linecharlambda0[4571/6286] Spectral line central wavelength0.1nmem.wl.centralfloatlambda[4571/6286] Hyperfine component wavelength0.1nmem.wldoubleloggfLogarithmic statistical weight of the lower level multiplied by the oscillator strengthstat.weight;phys.atmol.oscStrength;phys.atmol.levelfloatJ/A+A/580/A24/table5Atomic and molecular line parametersrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda0[4200/6315] Spectral line central wavelength0.1nmem.wl.centraldoubleLineAtomic and molecular line identificationmeta.id;spect.linefloatchi[0/40] Excitation potential {chi}eVphys.atmol.excitationfloatloggfLogarithmic statistical weight of the lower level multiplied by the oscillator strengthstat.weight;phys.atmol.oscStrength;phys.atmol.leveldoubleD0? Dissociation energy for molecular featureseVphys.energy;phys.mol.dissociationfloatnullableJ/A+A/580/A24/table6Atomic parameters for strong atomic linesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda0S[4200/6163] pectral line central wavelength0.1nmem.wl.centraldoubleLineAtomic and molecular line identificationmeta.id;spect.linefloatchi[0/4.5] Excitation potential {chi}eVphys.atmol.excitationfloatloggfLogarithmic statistical weight of the lower level multiplied by the oscillator strengthstat.weight;phys.atmol.oscStrength;phys.atmol.leveldoubleJ/A+A/580/A24/starsStars analyzed: photospheric parameters, abundances, and evolution parametersRefReferences related to the special cases (2)meta.refchar_RAPosition from Simbad (right ascension part)degpos.eq.ra;meta.mainrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameHD, BD, or HIP stellar numbermeta.number;phys.atmol.number;meta.maincharprimaryRSimbad column added by the CDSmeta.ref.urlcharSpTypeSpectral typesrc.spTypecharVbroad[0/15] Broadening velocitykm/sspect.line.broadfloatTeff[4169/6503] Star's effective temperatureKphys.temperature.effectiveinte_Teff[21/163] Error in star's effective temperatureKstat.error;phys.temperature.effectiveintlogg[1/5] Star's surface gravityphot.sbfloate_logg[0.1/0.6] Error in the star's surface gravitystat.errorfloatxi[0.03/5.6] Star's microturbulent velocity {xi}km/sphys.velocfloate_xi[[0.03/3] Error in microturbulent velocitykm/sstat.errorfloat[Fe/H]Abundance ratio [Fe/H]log(Sun)phys.abund.Fe;arith.ratiofloate_[Fe/H]Error in [Fe/H]log(Sun)stat.error;phys.abund.Fefloat[C/Fe]? Abundance ratio [C/Fe]log(Sun)phys.abund;arith.ratiofloatnullablee_[C/Fe]? Error in [C/Fe]log(Sun)stat.error;phys.abundfloatnullable[N/Fe]? Abundance ratio [N/Fe]log(Sun)phys.abund;arith.ratiofloatnullablee_[N/Fe]? Error in [N/Fe]log(Sun)stat.error;phys.abundfloatnullable[O/Fe]? Abundance ratio [O/Fe]log(Sun)phys.abund;arith.ratiofloatnullablee_[O/Fe]? Error in [O/Fe]log(Sun)stat.error;phys.abundfloatnullable[Na/Fe]? Abundance ratio [Na/Fe]log(Sun)phys.abund;arith.ratiofloatnullablee_[Na/Fe]? Error in [Na/Fe]log(Sun)stat.error;phys.abundfloatnullable[Mg/Fe]? Abundance ratio [Mg/Fe]log(Sun)phys.abund;arith.ratiofloatnullablee_[Mg/Fe]? Error in [Mg/Fe]log(Sun)stat.error;phys.abundfloatnullable[Si/Fe]? Abundance ratio [Si/Fe]log(Sun)phys.abund;arith.ratiofloatnullablee_[Si/Fe]? Error in [Si/Fe]log(Sun)stat.error;phys.abundfloatnullable[Ca/Fe]? Abundance ratio [Ca/Fe]log(Sun)phys.abund;arith.ratiofloatnullablee_[Ca/Fe]? Error in [Ca/Fe]log(Sun)stat.error;phys.abundfloatnullable[Ti/Fe]? Abundance ratio [Ti/Fe]log(Sun)phys.abund;arith.ratiofloatnullablee_[Ti/Fe]? Error in [Ti/Fe]log(Sun)stat.error;phys.abundfloatnullable[V/Fe]? Abundance ratio [V/Fe]log(Sun)phys.abund;arith.ratiofloatnullablee_[V/Fe]? Error in [V/Fe]log(Sun)stat.error;phys.abundfloatnullable[Mn/Fe]? Abundance ratio [Mn/Fe]log(Sun)phys.abund;arith.ratiofloatnullablee_[Mn/Fe]? Error in [Mn/Fe]log(Sun)stat.error;phys.abundfloatnullable[Ni/Fe]? Abundance ratio [Ni/Fe]log(Sun)phys.abund;arith.ratiofloatnullablee_[Ni/Fe]? Error in [Ni/Fe]log(Sun)stat.error;phys.abundfloatnullable[Cu/Fe]? Abundance ratio [Cu/Fe]log(Sun)phys.abund;arith.ratiofloatnullablee_[Cu/Fe]? Error in [Cu/Fe] J234-238 F5.2 [Sun] [Ba/Fe] ? Abundance ratio [Ba/Fe]log(Sun)stat.error;phys.abundfloatnullablee_[Ba/Fe]? Error in [Ba/Fe]log(Sun)stat.error;phys.abundfloatnullableClassSpectral luinosity classification: dwarf, giant or subgiantlog(Sun)src.class.luminositycharSimbadSimbad column added by the CDSmeta.ref.urlcharB-V[0.47/1.3] B-V color indexmagphot.color;em.opt.B;em.opt.VfloatVMag[-0.71/7.7] Absolute magnitude at the V bandmagphys.magAbs;em.opt.VfloatDist[3/100] Heliocentric distancepcpos.distancefloatBC[-0.9/0.02] Bolometric correctionphot.mag.bcfloatlogL[-1/2.3] Logarithmic luminositylog(solLum)phys.luminosityfloate_logL[0.005/0.09] Error in the logarithmic luminositylog(solLum)stat.errorfloatMass[0.6/3.6]? Mass of the starsolMassphys.massfloatnullablee_Mass[0.01/9.99]? Error in the stellar masssolMassstat.error;phys.massfloatnullableAge[0.1/32]? Age of the starGyrtime.agefloatnullablee_Age[0/12]? Lower error in the stellar ageGyrstat.error;time.agefloatnullableE_Age[0/12]? Upper error in the stellar ageGyrstat.error;stat.maxfloatnullablePopulPopulation membership (thin, thick or a transition population thin/thick)meta.code.member;src.samplecharRemRemarks on some special cases (1)meta.notechar_DEPosition from Simbad (declination part)degpos.eq.dec;meta.mainJ/A+A/580/A24/table2Atomic line parameters and solar EWsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda0[4518/6753] Spectral line central wavelength0.1nmem.wl.centraldoubleLineAtomic line identificationmeta.id;spect.linecharchi[0/5.7] Lower-level excitation potential {chi}eVphys.atmol.excitationfloatloggf? Logarithmic statistical weight of the lower level multiplied by the oscillator strengthstat.weight;phys.atmol.oscStrength;phys.atmol.levelfloatnullableEW[5/122] Solar equivalent width (m{AA})0.1pmspect.line.eqWidthfloat