Abundance analysis of APOGEE spectra for 58 metal-poor stars from the bulge spheroid

The central part of the Galaxy hosts a multitude of stellar populations, including the spheroidal bulge stars, stars moved to the bulge through secular evolution of the bar, inner halo, inner thick disc, inner thin disc, as well as debris from past accretion events. We identified a sample of 58 cand...

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Detalles Bibliográficos
Autores: Razera, Roberta, Barbuy, Beatriz, Moura, Tatiana C., Ernandes, Heitor, Pérez-Villegas, Angeles, Souza, S. O., Chiappini, Cristina, Queiroz, Anna Bárbara de Andrade, Anders, Friedrich, Fernández-Trincado, J. G., Friaça, A.C.S., Cunha, Katia, Smith, Verne V., Santiago, Basílio Xavier, Schiavon, Ricardo P., Valentini, Martina, Minniti, Dante, Schultheis, Mathias, Geisler, Doug, Sobeck, Jennifer, Placco, Vinicius M., Zoccali, Manuela
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2022
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/296372
Acceso en línea:http://hdl.handle.net/10261/296372
Access Level:acceso abierto
Palabra clave:Stars: abundances
Stars: atmospheres
Galaxy: bulge
Descripción
Sumario:The central part of the Galaxy hosts a multitude of stellar populations, including the spheroidal bulge stars, stars moved to the bulge through secular evolution of the bar, inner halo, inner thick disc, inner thin disc, as well as debris from past accretion events. We identified a sample of 58 candidate stars belonging to the stellar population of the spheroidal bulge, and analyse their abundances. The present calculations of Mg, Ca, and Si lines are in agreement with the ASPCAP abundances, whereas abundances of C, N, O, and Ce are re-examined. We find normal α-element enhancements in oxygen, similar to magnesium, Si, and Ca abundances, which are typical of other bulge stars surveyed in the optical in Baade’s Window. The enhancement of [O/Fe] in these stars suggests that they do not belong to accreted debris. No spread in N abundances is found, and none of the sample stars is N-rich, indicating that these stars are not second generation stars originated in globular clusters. Ce instead is enhanced in the sample stars, which points to an s-process origin such as due to enrichment from early generations of massive fast rotating stars, the so-called spinstars.

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