Chemical abundances of giant stars in the Crater stellar system

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dc.contributor.authorBonifacio, P.
dc.contributor.authorCaffau, E.
dc.contributor.authorZaggia, S.
dc.contributor.authorFrancois, P.
dc.contributor.authorSbordone, L.
dc.contributor.authorAndrievsky, S. M.
dc.contributor.authorKorotin, S. A.
dc.date.accessioned2024-01-10T13:46:44Z
dc.date.available2024-01-10T13:46:44Z
dc.date.issued2015
dc.description.abstractAims. We obtained spectra for two giants of Crater (Crater J113613-105227 and Crater J113615-105244) using X-Shooter at the VLT, with the purpose of determining their radial velocities and metallicities.
dc.description.abstractMethods. Radial velocities were determined by cross-correlating the spectra with that of a standard star. The spectra were analysed with the MyGIsFOS code using a grid of synthetic spectra computed from one-dimensional, local thermodynamic equilibrium (LTE) model atmospheres. Effective temperature and surface gravity were derived from photometry measured from images obtained by the Dark Energy Survey.
dc.description.abstractResults. The radial velocities are 144.3 +/- 4.0 km s(-1) for Crater J113613-105227 and and 134.1 +/- 4.0 km s(-1) for Crater J113615-105244. The metallicities are [Fe/H] = -1.73 and [Fe/H] = -1.67, respectively. In addition to the iron abundance, we were able to determine abundances for nine elements: Na, Mg, Ca, Ti, V, Cr, Mn, Ni, and Ba. For Na and Ba we took into account deviations from LTE because the corrections are significant. The abundance ratios are similar in the two stars and resemble those of Galactic stars of the same metallicity. In the deep photometric images we detected several stars that lie to the blue of the turn-off.
dc.description.abstractConclusions. The radial velocities imply that both stars are members of the Crater stellar system. The difference in velocity between the two taken at face value implies a velocity dispersion >3.7 km s(-1) at a 95% confidence level. Our spectroscopic metallicities agree excellently well with those determined by previous investigations using photometry. Our deep photometry and the spectroscopic metallicity imply an age of 7 Gyr for the main population of the system. The stars to the blue of the turn-off can be interpreted as a younger population that is of the same metallicity and an age of 2.2Gyr. Finally, spatial and kinematical parameters support the idea that this system is associated with the galaxies Leo IV and Leo V. All the observations favour the interpretation of Crater as a dwarf galaxy.
dc.description.funderFONDATION MERAC
dc.description.funderProgramme National de Cosmologie et Galaxies (PNCG)
dc.description.funderProgramme National de Physique Stellaire (PNPS) of the Institut National de Sciences de l'Univers of CNRS
dc.description.funderChile's Ministry of Economy, Development, and Tourism's Millennium Science Initiative
dc.description.funderNational Science Foundation
dc.description.funderPRIN INAF
dc.fechaingreso.objetodigital2024-05-02
dc.format.extent7 páginas
dc.fuente.origenWOS
dc.identifier.doi10.1051/0004-6361/201526366
dc.identifier.eissn1432-0746
dc.identifier.issn0004-6361
dc.identifier.urihttps://doi.org/10.1051/0004-6361/201526366
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/79195
dc.identifier.wosidWOS:000358877100008
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.subjectstars: Population II
dc.subjectglobular clusters: general
dc.subjectgalaxies: abundances
dc.subjectLocal Group
dc.subjectGLOBULAR-CLUSTER SYSTEM
dc.subjectDWARF GALAXIES
dc.subjectX-SHOOTER
dc.subjectHOMOGENEOUS SAMPLE
dc.subjectISOCHRONES
dc.subjectEVOLUTION
dc.subjectCODE
dc.subject.ods11 Sustainable Cities and Communities
dc.subject.odspa11 Ciudades y comunidades sostenibles
dc.titleChemical abundances of giant stars in the Crater stellar system
dc.typeartículo
dc.volumen579
sipa.codpersvinculados243032
sipa.indexWOS
sipa.indexScopus
sipa.trazabilidadCarga SIPA;09-01-2024
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