Galactic evolution of sulphur as traced by globular clusters

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dc.contributor.authorKacharov, N.
dc.contributor.authorKoch, A.
dc.contributor.authorCaffau, E.
dc.contributor.authorSbordone, L.
dc.date.accessioned2024-01-10T13:13:14Z
dc.date.available2024-01-10T13:13:14Z
dc.date.issued2015
dc.description.abstractContext. Sulphur is an important volatile a element, but its role in the Galactic chemical evolution is still uncertain, and more observations constraining the sulphur abundance in stellar photospheres are required.
dc.description.abstractAims. We derive the sulphur abundances in red giant branch (RGB) stars in three Galactic halo globular clusters (GC) that cover a wide metallicity range (-2.3 < [Fe/H] < -1.2): M4 (NGC6121), M22 (NGC6656), and M30 (NGC7099). The halo field stars show a large scatter in the [S/Fe] ratio in this metallicity span, which is inconsistent with canonical chemical evolution models. To date, very few measurements of [S/Fe] exist for stars in GCs, which are good tracers of the chemical enrichment of their environment. However, some light and a elements show star-to-star variations within individual GCs, and it is as yet unclear whether the a element sulphur also varies between GC stars.
dc.description.abstractMethods. We used the infrared spectrograph CRIRES to obtain high-resolution (R similar to 50 000), high signal-to-noise (S/N similar to 200 per px) spectra in the region of the S I multiplet 3 at 1045 nm for 15 GC stars selected from the literature (six stars in M4, six stars in M22, and three stars in M30). Multiplet 3 is better suited for S abundance derivation than the more commonly used lines of multiplet 1 at 920 nm, since its lines are not blended by telluric absorption or other stellar features at low metallicity.
dc.description.abstractResults. We used spectral synthesis to derive the [S/Fe] ratio of the stars assuming local thermodynamic equilibrium (LTE). We find mean [S/Fe](LTE) = 0.58 +/- 0.01 +/- 0.20 dex (statistical and systematic error) for M4, [S/Fe](LTE) = 0.57 +/- 0.01 +/- 0.19 dex for M22, and [S/Fe](LTE) = 0.55 +/- 0.02 +/- 0.16 dex for M30. The negative NLTE corrections are estimated to be in the order of the systematic uncertainties. We do not detect star-to-star variations of the S abundance in any of the observed GCs, with the possible exception of two individual stars, one in M22 and one in M30, which appear to be highly enriched in S.
dc.description.abstractConclusions. With the tentative exception of two stars with measured high S abundances, we conclude that sulphur behaves like a typical a element in the studied Galactic GCs, showing enhanced abundances with respect to the solar value at metallicities below [Fe/H] -1.0 dex without a considerable spread.
dc.description.funderDeutsche Forschungsgemeinschaft
dc.description.funderFONDATION MERAC
dc.fechaingreso.objetodigital2024-05-02
dc.format.extent9 páginas
dc.fuente.origenWOS
dc.identifier.doi10.1051/0004-6361/201425058
dc.identifier.eissn1432-0746
dc.identifier.issn0004-6361
dc.identifier.urihttps://doi.org/10.1051/0004-6361/201425058
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/78282
dc.identifier.wosidWOS:000353579600018
dc.information.autorucAstrofísica;Sbordone L;S/I;243032
dc.language.isoen
dc.nota.accesocontenido parcial
dc.publisherEDP SCIENCES S A
dc.revistaASTRONOMY & ASTROPHYSICS
dc.rightsacceso restringido
dc.subjectstars: abundances
dc.subjectGalaxy: halo
dc.subjectglobular clusters: individual: M 4
dc.subjectglobular clusters: individual: M 22
dc.subjectglobular clusters: individual: M 30
dc.subjectglobular clusters: general
dc.subjectMETAL-POOR STARS
dc.subjectABUNDANCE RATIOS
dc.subjectCHEMICAL EVOLUTION
dc.subjectABSORPTION-LINE
dc.subjectZINC ABUNDANCES
dc.subjectHALO STARS
dc.subjectGALAXIES
dc.subjectSI
dc.subjectNUCLEOSYNTHESIS
dc.subjectSPECTROSCOPY
dc.subject.ods11 Sustainable Cities and Communities
dc.subject.odspa11 Ciudades y comunidades sostenibles
dc.titleGalactic evolution of sulphur as traced by globular clusters
dc.typeartículo
dc.volumen577
sipa.codpersvinculados243032
sipa.indexWOS
sipa.indexScopus
sipa.trazabilidadCarga SIPA;09-01-2024
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