J/other/PHYS/101ivo://CDS.VizieR/J/other/PHYS/101.Q5005CDSSenturk S.A.Sahin T.Kayhan C.2026-06-23T09:03:53Z2026-06-23T10:00:22ZCDS support team

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

cds-question@unistra.frg-starsthe-sunstellar-agesstellar-massesdwarf-starsinfrared-astronomyspectroscopychemical-abundancesWe present the first high-resolution near-infrared spectroscopic analysis of the solar analog HD 115617 (61 Virginis), complemented by optical spectroscopy, asteroseismology, and spectral energy distribution modeling. Using ESPRESSO and IGRINS spectra with a newly calibrated NIR line list, we derived atmospheric parameters that revealed notable differences between spectral regions: the optical analysis yielded Teff=5500+/-140K, logg=4.40+/-0.16 , and solar metallicity, whereas the NIR yielded Teff=5750+/-140K. We tested this 250K discrepancy using the independent line depth ratio (LDR) method for both spectra. When applied to the optical lines, LDR confirmed the cooler scale (5553+/-73K); for the NIR lines, it provided an intermediate temperature (5636+/-15K). Asteroseismic scaling with TESS data yielded a radius of 0.98+/-0.09R_{Sun}_, consistent with SED fitting and confirming the star's main-sequence solar-like status. However, the age estimates diverged between methods, with optical and NIR analyses yielding ages of 10.97 and 8.04 Gyr, respectively. Critically, a condensation temperature analysis revealed no significant trend, confirming the star's bulk solar-like composition and showing no chemical signature of planetary formation processes. Kinematic diagnostics place HD 115617 in the thin Galactic disk, with a birth radius of approx 5.7-8.0kpc. Although the spectral differences may be linked to the star's multi-planet system or debris disk, our analysis highlights the critical challenge of distinguishing such effects from methodological systematics in multi-wavelength studies. Consequently, we propose a systematic, homogeneous optical-NIR survey of solar-type stars to resolve this ambiguity, which could ultimately inform novel indirect methods for characterizing stellar environments.2026PhyS..101q5005Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/other/PHYS/101.Q5005CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/other/PHYS/101.Q5005https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/other/PHYS/101.Q5005http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/other/PHYS/101.Q5005https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/other/PHYS/101.Q5005https://vizier.iucaa.in/viz-bin/votable?-source=J/other/PHYS/101.Q5005http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/other/PHYS/101.Q5005GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapInfrareddefaultJ/other/PHYS/101.Q5005/table1Stellar atmospheric parametersrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarTarget star identifiermeta.id;meta.maincharSpectrInstrument used for spectral observationmeta.id;instrcharWaveRangeWavelength range of the spectrum (in Angstroems)em.wlcharTeffEffective temperatureKphys.temperature.effectiveinte_TeffUncertainty in TeffKstat.error;phys.temperature.effectiveintloggSurface gravitylog(cm.s**-2)phys.gravityfloate_loggUncertainty in logglog(cm.s**-2)stat.errorfloat[Fe/H]Metallicityphys.abund.Zfloate_[Fe/H]Uncertainty in [Fe/H]stat.error;phys.abund.FefloatksiMicroturblence velocitykm/sphys.veloc.microTurbfloate_ksiUncertainty in ksikm/sstat.errorfloatJ/other/PHYS/101.Q5005/table2Chemical abundances for Sun and HD 115617recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSpeciesElemental ionization state and spectral datainstr.bandwidth;phys.atmol.ionizationcharn_Species[*] Note (1)meta.notecharlogeps(X)Logarithmic abundances of HD115617phys.abundfloate_logeps(X)Uncertainty in log_epsilon(X)stat.errorfloat[X/Fe]Elemental abundance of HD115617 relative to Sunphys.abundfloate_[X/Fe]Uncertainty in [X/Fe]stat.error;phys.abundfloato_[X/Fe]Number of the lines measured in HD115617meta.numberintlogepsSunCalculated solar reference abundancesphys.abundfloate_logepsSunUncertainty in the solar reference abundancestat.errorfloato_logepsSunNumber of the lines measured in the Sunmeta.numberintAsp21Reported solar abundances in the Asplund et al. (2021A&A...653A.141A)phys.abundfloate_Asp21Uncertainty abundances for Asplund et al. (2021A&A...653A.141A)stat.errorfloatdeltaDifference between solar abundance in the this study and those in Asplund et al. (2021A&A...653A.141A)obs.param;arith.difffloatJ/other/PHYS/101.Q5005/table5HD 115617 photometric bands and observed magnitudesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintCatalogPhotometric survey/catalog namemeta.idcharBandPhotometric filter/bandinstr.bandpasscharmagObserved magnitude in Bandmagphot.magfloate_magUncertainty in magnitudemagstat.error;phot.magfloatJ/other/PHYS/101.Q5005/table6Results of the SED fittingrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTeffSEDEffective temperature derived from SEDKphys.temperature.effectiveinte_TeffSEDUncertainty in Teff_SEDKstat.errorintloggSEDSurface gravity derived from SEDlog(cm.s**-2)phys.gravityfloate_loggSEDUncertainty in logg_SEDlog(cm.s**-2)stat.errorfloat[Fe/H]SEDMetallicity derived from SEDphys.abund.Fefloate_[Fe/H]SEDUncertainty in FeH_SEDstat.error;phys.abund.FefloatDistSEDDistance derived from SEDpcpos.distancefloate_DistSEDUncertainty in Dist_SEDpcstat.errorfloatRadSEDStellar radius derived from SEDsolRadphys.size.radiusfloate_RadSEDUncertainty in Radius_SEDsolRadstat.errorfloatJ/other/PHYS/101.Q5005/table7Stellar parameters derived from MESA evolutionary modelsRadStellar radius derived from MESA modelingsolRadphys.size.radiusfloate_RadUncertainty in RadiussolRadstat.errorfloatAge? Stellar age derived from MESA modelingMyrtime.agefloatnullablee_Age? Uncertainty in AgeMyrstat.error;time.agefloatnullableTeffMESAEffective temperature from the best-fitting MESA modelKphys.temperature.effectiveinte_TeffMESAUncertainty in TeffMESAKstat.errorintloggMESASurface gravity from the best-fitting MESA modellog(cm.s**-2)phys.gravityfloate_loggMESAUncertainty in loggMESAlog(cm.s**-2)stat.errorfloat[Fe/H]MESA? Metallicity [Fe/H] from the best-fitting MESA modelphys.abund.Zfloatnullablee_[Fe/H]MESA? Uncertainty in [Fe/H]SEDstat.error;phys.abund.FefloatnullableMethodFitting methodmeta.notecharTeffiObservational Teff adopted in the fitKphys.temperature.effectiveinte_TeffiUncertainty in TeffiKstat.errorintloggiObservational log(g) adopted in the fitlog(cm.s**-2)phys.gravityfloate_loggiUncertainty in loggilog(cm.s**-2)stat.errorfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMassStellar mass derived from MESA modelingsolMassphys.massfloate_MassUncertainty in MasssolMassstat.error;phys.massfloat[Fe/H]iObservational metallicity [Fe/H] adopted in the fitphys.abund.Z;meta.modelledfloate_[Fe/H]iUncertainty in [Fe/H]istat.error;phys.abund.FefloatStarStellar identifiermeta.id;meta.mainchar