J/A+A/673/A123ivo://CDS.VizieR/J/A+A/673/A123doi:10.26093/cds/vizier.36730123CDSBrauner M.Masseron T.Garcia-Hernandez D.A.Pignatari M.Womack K.A.,Lugaro M.Hayes C.R.2025-07-04T20:02:01Z2023-05-17T09:06:59ZCDS support team

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

cds-question@unistra.frpeculiar-variable-starschemically-peculiar-starsinfrared-astronomyspectroscopyThe origin of phosphorus, one of the essential elements for life on Earth, is currently unknown. Prevalent models of Galactic chemical evolution (GCE) systematically underestimate the amount of P compared to observations, especially at low metallicities. The recently discovered P-rich ([P/Fe]>~1.2dex) and metal-poor ([Fe/H]~-1.0dex) giants further challenge the GCE models, calling current theories on stellar nucleosynthesis into question. Since the observed low-mass giants are not expected to produce their high P contents themselves, our primary goal is to find clues on their progenitor or polluter. By increasing the number of known P-rich stars, we aim to narrow down a statistically reliable chemical abundance pattern that defines these peculiar stars. In this way, we place more robust constraints on the nucleosynthetic mechanism responsible for the unusually high P abundances. In the long term, identifying the progenitor of the P-rich stars may contribute to the search for the source of P in our Galaxy. We performed a detailed chemical abundance analysis based on the high resolution near-infrared (H-band) spectra from the latest data release (DR17) of the APOGEE-2 survey. Employing the BACCHUS code, we measured the abundances of 13 elements in the inspected sample, which is mainly composed of a recent collection of Si-enhanced giants. We also analyzed the orbital motions and compared the abundance results to possible nucleosynthetic formation scenarios, as well as to detailed GCE models. These models were produced with the OMEGA+ chemical evolution code, using four different massive star yield sets to investigate different scenarios for massive star evolution. We enlarged the sample of confirmed P-rich stars from 16 to a group of 78 giants, representing the largest sample of P-rich stars to date, including the first detection of a P-rich star in a Galactic globular cluster. Significant enhancements in O, Al, Si and Ce, as well as systematic correlations among the studied elements, unveil the unique chemical fingerprint of the P-rich stars. In contrast, the high [Mg/Fe] and [(C+N)/Fe] found in some of the P-rich stars with respect to P-normal stars is, due to the present uncertainties, not confirmed over the full sample. Strikingly, the strong over-abundance in the alpha-element Si is accompanied by normal Ca and S abundances, at odds with present stellar nucleosynthesis models of massive stars. Our analysis of the orbital motion showed that the P-rich stars do not belong to a locally specific population in the Galaxy. In addition, we confirm that the majority of the sample stars are not part of binary systems.2023A&A...673A.123Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/673/A123CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-tohttps://www.sdss4.org/dr16/irspec/aspcap : ASPCAP DR16 Home pagehttps://www.sdss4.org/dr17/irspec/aspcap : ASPCAP DR17 Home pagehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/673/A123https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/673/A123http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/673/A123https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/673/A123https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/673/A123http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/673/A123GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/673/A123/table2 (Stellar parameters and elemental abundances of the full P-rich stars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/673/A123/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/673/A123/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/673/A123/table2?GETtext/xml+votable180.050000true1.1741667-0.09869440.0055555555555555566/4881 5618 8891 9037 9172 9258 9264 9579 9664 9883 9892 10102 10294 10300 10676 10911 11012 11275 11286 13808 14470 15132 18090 18437 18569 18668 19412 25694 26112 27870 28685 28715 28726 28734 28778 28782 28785 28831 28842 28849 28910 29184-29185 29194 29231 29283 29349 29351 29404 29464 29468 29754 30997 31018 31115 31604 31624 32511 33000 33057 33239 37406 37419 37517 38927 38973 42243 42355 42417 42449 42705 42873 42887 42955 43003 44717 45025 46268 47658 47756 47793 47796 47801 47871 48028 49077https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/673/A123?format=asciiInfrareddefaultJ/A+A/673/A123/table2Stellar parameters and elemental abundances of the full P-rich starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintAPOGEEAPOGEE identifier (APOGEE_ID)meta.id;meta.maincharSourceSource of the parameters (DR16 or DR17)meta.id;meta.datasetchar[M/H]Uncalibrated [M/H] from ASPCAP analysis of combined spectrumphys.abund.FefloatS/NSignal-to-Noise ratio from ASPCAP analysis of combined spectrumstat.snrfloatSimbadSimbad column added by the CDSmeta.ref.urlcharTeffEffective Temperature from ASPCAP analysis of combined spectrum (MH)Kphys.temperature.effectivefloatloggSurface Gravity from ASPCAP analysis of combined spectrum (MH)phys.gravityfloat[C/Fe]? [C/Fe] from BACCHUS analysis of combined spectrumphys.abundfloatnullablen_[C/Fe][*+: ] Note on [C/Fe] (1)meta.notechars_[C/Fe]? Standard deviation of [C/Fe]stat.stdev;phys.abundfloatnullablel_[C/Fe][0/1] Indicator of upper limits in [C/Fe] (2)meta.code.error;phys.abundint[N/Fe]? [N/Fe] from BACCHUS analysis of combined spectrumphys.abundfloatnullables_[N/Fe]? Standard deviation of [N/Fe]stat.stdev;phys.abundfloatnullablel_[N/Fe][0/1] Indicator of upper limits in [N/Fe] (2)meta.code.error;phys.abundint[O/Fe]? [O/Fe] from BACCHUS analysis of combined spectrumphys.abundfloatnullables_[O/Fe]? Standard deviation of [O/Fe]stat.stdev;phys.abundfloatnullablel_[O/Fe][0/1] Indicator of upper limits in [O/Fe] (2)meta.code.error;phys.abundint[Na/Fe]? [Na/Fe] from BACCHUS analysis of combined spectrumphys.abundfloatnullables_[Na/Fe]? Standard deviation of [Na/Fe]stat.stdev;phys.abundfloatnullablel_[Na/Fe][0/1] Indicator of upper limits in [Na/Fe] (2)meta.code.error;phys.abundint[Mg/Fe]? [Mg/Fe] from BACCHUS analysis of combined spectrumphys.abundfloatnullables_[Mg/Fe]? Standard deviation of [Mg/Fe]stat.stdev;phys.abundfloatnullable[Al/Fe]? [Al/Fe] from BACCHUS analysis of combined spectrumphys.abundfloatnullables_[Al/Fe]? Standard deviation of [Al/Fe]stat.stdev;phys.abundfloatnullable[Si/Fe]? [Si/Fe] from BACCHUS analysis of combined spectrumphys.abundfloatnullables_[Si/Fe]? Standard deviation of [Si/Fe]stat.stdev;phys.abundfloatnullable[P/Fe]? [P/Fe] from BACCHUS analysis of combined spectrumphys.abundfloatnullables_[P/Fe]? Standard deviation of [P/Fe]stat.stdev;phys.abundfloatnullablel_[P/Fe][0/1] Indicator of upper limits in [P/Fe] (2)meta.code.error;phys.abundint[S/Fe]? [S/Fe] from BACCHUS analysis of combined spectrumphys.abundfloatnullablen_[S/Fe][*+: ] Note on [S/Fe] (1)meta.notechars_[S/Fe]? Standard deviation of [S/Fe]stat.stdev;phys.abundfloatnullablel_[S/Fe][0/1] Indicator of upper limits in [S/Fe] (2)meta.code.error;phys.abundint[Ca/Fe]? [Ca/Fe] from BACCHUS analysis of combined spectrumphys.abundfloatnullablen_[Ca/Fe][*+: ] Note on [Ca/Fe] (1)meta.notechars_[Ca/Fe]? Standard deviation of [Ca/Fe]stat.stdev;phys.abundfloatnullablel_[Ca/Fe][0/1] Indicator of upper limits in [Ca/Fe] (2)meta.code.error;phys.abundint[Fe/H]? [Fe/H] from BACCHUS analysis of combined spectrumphys.abund.Fefloatnullablen_[Fe/H][: ] Note on [Fe/H] (1)meta.notechars_[Fe/H]Standard deviation of [Fe/H]stat.stdev;phys.abund.Fefloat[Ce/Fe]? [Ce/Fe] from BACCHUS analysis of combined spectrumphys.abundfloatnullablen_[Ce/Fe][*+: ] Note on [Ce/Fe] (1)meta.notechars_[Ce/Fe]? Standard deviation of [Ce/Fe]stat.stdev;phys.abundfloatnullablel_[Ce/Fe][0/1] Indicator of upper limits in [Ce/Fe] (2)meta.code.error;phys.abundint[Nd/Fe]? [Nd/Fe] from BACCHUS analysis of combined spectrumphys.abundfloatnullablen_[Nd/Fe][*+: ] Note on [Nd/Fe] (1)meta.notechars_[Nd/Fe]? Standard deviation of [Nd/Fe]stat.stdev;phys.abundfloatnullablel_[Nd/Fe][0/1] Indicator of upper limits in [Nd/Fe] (2)meta.code.error;phys.abundint_RAPosiitons from APOGEE name (right ascension part)degpos.eq.ra;meta.main_DEPosiitons from APOGEE name (declination part)degpos.eq.dec;meta.mainn_[N/Fe][*+: ] Note on [N/Fe] (1)meta.notecharn_[O/Fe][*+: ] Note on [O/Fe] (1)meta.notecharn_[Na/Fe][*+: ] Note on [Na/Fe] (1)meta.notecharn_[Mg/Fe][*: ] Note on [Mg/Fe] (1)meta.notecharn_[Al/Fe][*: ] Note on [Al/Fe] (1)meta.notecharn_[Si/Fe][: ] Note on [Si/Fe] (1)meta.notecharn_[P/Fe][*+: ] Note on [P/Fe] (1)meta.notechar