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Aims. The aim of this work is the study of abundances of the heavy elements Ba, La, Ce, Nd, and Eu in 56 bulge giants (red giant branch and red clump) with metallicities ranging from 1 : 3 dex to 0 : 5 dex. Methods. We obtained high-resolution spectra of our giant stars using the FLAMES-UVES sp...


Van der Swaelmen, MBarbuy, BHill, VZoccali, MMinniti, DOrtolani, SGomez, A[Heavy elements Ba, La, Ce, Nd, and Eu in 56 Galactic bulge red giants]Heavy elements Ba, La, Ce, Nd, and Eu in 56 Galactic bulge red giants

Rojas-Arriagada, A.Recio-Blanco, A.de Laverny, P.Schultheis, M.Guiglion, G.Mikolaitis, Š.Kordopatis, G.Hill, V.Gilmore, G.Randich, S.Alfaro, E. J.Bensby, T.Koposov, S. E.Costado, M. T.Franciosini, E.Hourihane, A.Jofré, P.Lardo, C.Lewis, J.Lind, K.Magrini, L.Monaco, L.Morbidelli, L.Sacco, G. G.Worley, C. C.Zaggia, S.Chiappini, C.[The Gaia-ESO Survey: Separating disk chemical substructures with cluster models⋆ Evidence of a separate evolution in the metal-poor thin disk]The Gaia-ESO Survey: Separating disk chemical substructures with cluster models⋆ Evidence of a separate evolution in the metal-poor thin disk

Fernandez-Trincado, JGRobin, ACMoreno, ESchiavon, RPPerez, AEGVieira, KCunha, KZamora, OSneden, CSouto, DCarrera, RJohnson, JAShetrone, MZasowski, GGarcia-Hernandez, DAMajewski, SRReyle, CBlanco-Cuaresma, SMartinez-Medina, LAPerez-Villegas, AValenzuela, OPichardo, BMeza, AMeszaros, SSobeck, JGeisler, DAnders, FSchultheis, MTang, BRoman-Lopes, AMennickent, REPan, KNitschelm, CAllard, F[DISCOVERY OF A METAL-POOR FIELD GIANT WITH A GLOBULAR CLUSTER SECOND-GENERATION ABUNDANCE PATTERN]DISCOVERY OF A METAL-POOR FIELD GIANT WITH A GLOBULAR CLUSTER SECOND-GENERATION ABUNDANCE PATTERN

Aims. Carbon-enhanced metal-poor (CEMP) stars represent a sizeable fraction of all known metal-poor stars in the Galaxy. Their formation and composition remains a significant topic of investigation within the stellar astrophysics community. Methods. We analysed a sample of low-resolution spectra ...


Caffau, E.Gallagher, A.J.Bonifacio, P.Spite, M.Duffau, S.Spite, F.Monaco, L.Sbordone, L.[Investigation of a sample of carbon-enhanced metal-poor stars observed with FORS and GMOS]Investigation of a sample of carbon-enhanced metal-poor stars observed with FORS and GMOS

D'Orazi, V.Magurno, D.Bono, G.Matsunaga, N.Braga, V.F.Elgueta, S.S.Fukue, K.Hamano, S.Inno, L.Kobayashi, N.Kondo, S.Monelli, M.Nonino, M.Przybilla, N.Sameshima, H.Saviane, I.Taniguchi, D.Thevenin, F.Urbaneja-Perez, M.Watase, A.Arai, A.Bergemann, M.Buonanno, R.Dall'Ora, M.Da Silva, R.Fabrizio, M.Ferraro, I.Fiorentino, G.Francois, P.Gilmozzi, R.Iannicola, G.Ikeda, Y.Jian, M.Kawakita, H.Kudritzki, R.P.Lemasle, B.Marengo, M.Marinoni, S.Martínez-Vázquez, C.E.Minniti, D.Neeley, J.Otsubo, S.Prieto, J.L.Proxauf, B.Romaniello, M.Sanna, N.Sneden, C.Takenaka, K.Tsujimoto, T.Valenti, E.Yasui, C.Yoshikawa, T.Zoccali, M.[On the Chemical Abundances of Miras in Clusters: V1 in the Metal-rich Globular NGC 5927]On the Chemical Abundances of Miras in Clusters: V1 in the Metal-rich Globular NGC 5927

Context. Oxygen and zinc in the Galactic bulge are key elements for the understanding of the bulge chemical evolution. Oxygen-to-iron abundance ratios provide a most robust indicator of the star formation rate and chemical evolution of the bulge. Zinc is enhanced in metal-poor stars, behaving as ...


Da Silveira, C.R.Barbuy, B.Friaça, A.C.S.Hill, V.Zoccali, M.Rafelski, M.Gonzalez, O.A.Minniti, D.Renzini, A.Ortolani, S.[Oxygen and zinc abundances in 417 Galactic bulge red giants]Oxygen and zinc abundances in 417 Galactic bulge red giants

We observed six He-clump stars of the intermediate-Age stellar cluster Gaia1 with the MIKE/Magellan spectrograph. A possible extra-galactic origin of this cluster, recently discovered thanks to the first data release of the ESA Gaia mission, has been suggested, based on its orbital parameters. Ab...


Mucciarelli, A.Monaco, L.Bonifacio, P.Saviane, I.[Chemical composition of the stellar cluster Gaia1: No surprise behind Sirius]Chemical composition of the stellar cluster Gaia1: No surprise behind Sirius

We find two chemically distinct populations separated relatively cleanly in the [Fe/H]-[Mg/Fe] plane, but also distinguished in other chemical planes, among metal-poor stars (primarily with metallicities [Fe H] < -0.9) observed by the Apache Point Observatory Galactic Evolution Experiment (APOGEE...


Hayes, C.R.Majewski, S.R.Shetrone, M.Fernández-Alvar, E.Prieto, C.A.Schuster, W.J.Carigi, L.Cunha, K.Smith, V.V.Sobeck, J.Almeida, A.Beers, T.C.Carrera, R.Fernández-Trincado, J.G.García-Hernández, D.A.Geisler, D.Lane, R.R.Lucatello, S.Matthews, A.M.Minniti, D.Nitschelm, C.Tang, B.Tissera, P.B.Zamora, O.[Disentangling the Galactic Halo with APOGEE. I. Chemical and Kinematical Investigation of Distinct Metal-poor Populations]Disentangling the Galactic Halo with APOGEE. I. Chemical and Kinematical Investigation of Distinct Metal-poor Populations

We report the first estimate of the He abundance of the population of RR Lyrae stars in the Galactic bulge. This is done by comparing the recent observational data with the latest models. We use the large samples of ab-type RR Lyrae stars found by OGLE IV in the inner bulge and by the VVV survey ...


Marconi, M.Minniti, D.[Gauging the Helium Abundance of the Galactic Bulge RR Lyrae Stars]Gauging the Helium Abundance of the Galactic Bulge RR Lyrae Stars

The formation processes that led to the current Galactic stellar halo are still under debate. Previous studies have provided evidence for different stellar populations in terms of elemental abundances and kinematics, pointing to different chemical and star formation histories (SFHs). In the prese...


Fernández-Alvar, E.Carigi, L.Schuster, W.J.Hayes, C.R.Ávila-Vergara, N.Majewski, S.R.Allende Prieto, C.Beers, T.C.Sánchez, S.F.Zamora, O.García-Hernández, D.A.Tang, B.Fernández-Trincado, J.G.Tissera, P.Geisler, D.Villanova, S.[Disentangling the Galactic Halo with APOGEE. II. Chemical and Star Formation Histories for the Two Distinct Populations]Disentangling the Galactic Halo with APOGEE. II. Chemical and Star Formation Histories for the Two Distinct Populations

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