J/A+A/668/A88ivo://CDS.VizieR/J/A+A/668/A88doi:10.26093/cds/vizier.36680088CDSNandakumar G.Ryde N.Montelius M.Thorsbro B.Joensson H.Mace G.2024-11-28T20:01:36Z2022-12-09T08:04:39ZCDS support team

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

cds-question@unistra.frmilky-way-galaxyk-starsgiant-starschemical-abundancesinfrared-astronomyspectroscopyeffective-temperaturePhosphorus (P) is considered to be one of the key elements for life, making it an important element to look for in the abundance analysis of spectra of stellar systems. Yet, only a select number of spectroscopic studies exist to estimate the phosphorus abundances and investigate its trend across a range of metallicities. This is due to the lack of good phosphorus lines in the optical wavelength region and the requirement of careful manual analysis of the blended phosphorus lines in near-infrared H-band spectra obtained with individual observations and surveys such as the Apache Point Observatory Galactic Evolution Experiment (APOGEE). Based on a consistent and systematic analysis of high-resolution, near-infrared Immersion GRating INfrared Spectrograph (IGRINS) spectra of 38 K giant stars in the Solar neighborhood, we present and investigate the phosphorus abundance trend in the metallicity range of -1.2dex<[Fe/H]<0.4dex. Furthermore, we compare this trend with the available chemical evolution models to shed some light on the origin and evolution of phosphorus. We have observed full H- and K-band spectra at a spectral resolving power of R=45000 with IGRINS mounted on the Gemini South telescope, the Discovery Channel Telescope, and the Harlan J Smith Telescope at McDonald Observatory. Abundances were determined from spectral lines by modeling the synthetic spectrum that best matches the observed spectrum by chi-square minimization. For this task, we used the Spectroscopy Made Easy (SME) tool in combination with one-dimensional (1D) Model Atmospheres in a Radiative and Convective Scheme (MARCS) stellar atmosphere models. The investigated sample of stars have reliable stellar parameters estimated using optical FIber-fed Echelle Spectrograph (FIES) spectra obtained in a previous study of a set of stars called GIants in the Local Disk (GILD). In order to determine the phosphorus abundances from the 16482.92 Angstrom phosphorus line, we needed to take special care blending the CO(7-4) line. With the stellar parameters known, we thus determined the C, N, and O abundances from atomic carbon and a range of nonblended molecular lines (CO, CN, and OH) which are plentiful in the H-band region of K giant stars, assuring an appropriate modeling of the blending CO(7-4) line. We present the [P/Fe] versus [Fe/H] trend for K giant stars in the metallicity range of -1.2dex<[Fe/H]<0.4dex and enhanced phosphorus abundances for two metal-poor s-rich stars. We find that our trend matches well with the compiled literature sample of prominently dwarf stars and the limited number of giant stars. Our trend is found to be higher by 0.05-0.1dex compared to the theoretical chemical evolution trend resulting from the core collapse supernova (type II) of massive stars with the phosphorus yields arbitrarily increased by a factor of 2.75. Thus the enhancement factor might need to be 0.05-0.1dex higher to match our trend. We also find an empirically determined primary behavior for phosphorus. Furthermore, the phosphorus abundance is found to be elevated by 0.6-0.9dex in the two s-enriched stars compared to the theoretical chemical evolution trend.2022A&A...668A..88Nhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/668/A88CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/668/A88https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/668/A88http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/668/A88https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/668/A88https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/668/A88http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/668/A88GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/668/A88/table2 (Stellar parameters and phosphorus abundances for sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/668/A88/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/668/A88/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/668/A88/table2?GETtext/xml+votable180.050000true213.915300319.18240920.0055555555555555566/4345 4444 4574 5982 6219 8767 9258 9665 10584 11929 13282 14585 14589 14591 14735 14753 14757 14825 14827 14923 14936 14948 14954 15040 15060 15148 15154 15176 16035 18953 24715 26552 30215 30419 30606https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/668/A88?format=asciiInfrareddefaultJ/A+A/668/A88/table2Stellar parameters and phosphorus abundances for sampleSimbadNameSimbad column added by the CDSmeta.idcharnullablevmacroMacroturbulence velocitykm/sphys.veloc.microTurbfloat[P/Fe]Relative phosphorus abundancephys.abundfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarName (HD, HIP, KIC, 2M)meta.id;meta.maincharn_Star[a] Note on Star (1)meta.notecharPopDesignated stellar population (2)meta.codecharTeffEffective temperatureKphys.temperature.effectiveintloggSurface gravitylog(cm.s**-2)phys.gravityfloat[Fe/H]Relative iron abundancephys.abund.FefloatvmicroMicroturbulence velocitykm/sphys.veloc.microTurbfloate_[P/Fe]Uncertainty in the relative phosphorus abundancestat.error;phys.abundfloatS/NSignal-to-noise ratiostat.snrint_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