Bright Metal-Poor Stars from the Hamburg/ESO Survey. II. A Chemodynamical analysis
dc.contributor.author | Beers, Timothy C. | |
dc.contributor.author | Placco, V. M. | |
dc.contributor.author | Carollo, Daniela | |
dc.contributor.author | Rossi, Silvia | |
dc.contributor.author | Lee, Young Sun | |
dc.contributor.author | Frebel, Anna | |
dc.contributor.author | Norris, John | |
dc.contributor.author | Dietz, Sarah | |
dc.contributor.author | Masseron, Thomas | |
dc.date.accessioned | 2021-05-14T00:36:11Z | |
dc.date.issued | 2017 | |
dc.date.updated | 2020-11-23T10:16:36Z | |
dc.description.abstract | We obtain estimates of stellar atmospheric parameters for a previously published sample of 1777 relatively bright (9 < B < 14) metal-poor candidates from the Hamburg/ESO Survey. The original Frebel et al. analysis of these stars was able to derive estimates of [Fe/H] and [C/Fe] only for a subset of the sample, due to limitations in the methodology then available. A new spectroscopic analysis pipeline has been used to obtain estimates of Teff , log g, [Fe/H], and [C/Fe] for almost the entire data set. This sample is very local-about 90% of the stars are located within 0.5 kpc of the Sun. We consider the chemodynamical properties of these stars in concert with a similarly local sample of stars from a recent analysis of the Bidelman and MacConnell 'weak metal' candidates by Beers et al. We use this combined sample to identify possible members of the halo stream of stars suggested by Helmi et al. and Chiba & Beers, as well as stars that may be associated with stripped debris from the putative parent dwarf of the globular cluster Omega Centauri, suggested to exist by previous authors. We identify a clear increase in the cumulative frequency of carbon-enhanced metal-poor (CEMP) stars with declining metallicity, as well as an increase in the fraction of CEMP stars with distance from the Galactic plane, consistent with previous results. We also identify a relatively large number of CEMP stars with kinematics consistent with the metal-weak thick-disk population, with possible implications for its origin. | en_AU |
dc.description.sponsorship | T.C.B., D.C., V.M.P., and S.D. acknowledge partial support for this work from grants PHY 08-22648, Physics Frontier Center/JINA, and PHY 14-30152, Physics Frontier Center/ JINA Center for the Evolution of the Elements, awarded by the US National Science Foundation. S.R. acknowledges partial support for this work from CAPES, CNPq, FAPESP, and INCT. Y.S.L. acknowledges partial support from the National Research Foundation of Korea (NRF) to the Center for Galaxy Evolution Research and Basic Science Research Program, funded by the Ministry of Science, ICT, and Future Planning (NRF-2015R1C1A1A02036658). A.F. acknowledges funding from NSF-CAREER grant AST 12-55160 and from the Silverman (1968) Family Career Development Professorship. The study at RSAA, ANU, of the Galaxyʼs metal-poor stars is supported by Australian Research Council grants DP0663562 and DP0984924, which J.E.N. is pleased to acknowledge. | en_AU |
dc.format.mimetype | application/pdf | en_AU |
dc.identifier.issn | 0004-637X | en_AU |
dc.identifier.uri | http://hdl.handle.net/1885/233043 | |
dc.language.iso | en_AU | en_AU |
dc.provenance | https://v2.sherpa.ac.uk/id/publication/6401..."The accepted version can be archived in Institutional Repository" from SHERPA/RoMEO as at 19/05/2021 | |
dc.publisher | IOP Publishing | en_AU |
dc.relation | http://purl.org/au-research/grants/arc/DP0984924 | en_AU |
dc.rights | © 2017. The American Astronomical Society | en_AU |
dc.source | The Astrophysical Journal | en_AU |
dc.source.uri | https://iopscience.iop.org/article/10.3847/1538-4357/835/1/81 | en_AU |
dc.subject | Galaxy: kinematics and dynamics | en_AU |
dc.subject | Galaxy: stellar content | en_AU |
dc.subject | stars: abundances | en_AU |
dc.subject | stars: carbon | en_AU |
dc.subject | stars: Population II | en_AU |
dc.subject | stars: kinematics and dynamics | en_AU |
dc.title | Bright Metal-Poor Stars from the Hamburg/ESO Survey. II. A Chemodynamical analysis | en_AU |
dc.type | Journal article | en_AU |
dcterms.accessRights | Open Access | |
local.bibliographicCitation.issue | 1 | en_AU |
local.contributor.affiliation | Beers, Timothy C, University of Notre Dame | en_AU |
local.contributor.affiliation | Placco, V. M., University of Notre Dame | en_AU |
local.contributor.affiliation | Carollo, Daniela, College of Science, ANU | en_AU |
local.contributor.affiliation | Rossi, Silvia, Universidade de Sao Paulo | en_AU |
local.contributor.affiliation | Lee, Young Sun, Chungnam National University | en_AU |
local.contributor.affiliation | Frebel, Anna, Massachusetts Institute of Technology | en_AU |
local.contributor.affiliation | Norris, John, College of Science, ANU | en_AU |
local.contributor.affiliation | Dietz, Sarah, University of Notre Dame | en_AU |
local.contributor.affiliation | Masseron, Thomas, University of Cambridge | en_AU |
local.contributor.authoremail | u7401084@anu.edu.au | en_AU |
local.contributor.authoruid | Carollo, Daniela, u4431829 | en_AU |
local.contributor.authoruid | Norris, John, u7401084 | en_AU |
local.description.notes | Imported from ARIES | en_AU |
local.identifier.absfor | 020104 - Galactic Astronomy | en_AU |
local.identifier.ariespublication | a383154xPUB6406 | en_AU |
local.identifier.citationvolume | 835 | en_AU |
local.identifier.doi | 10.3847/1538-4357/835/1/81 | en_AU |
local.identifier.scopusID | 2-s2.0-85011341230 | |
local.identifier.thomsonID | 000393455400081 | |
local.identifier.uidSubmittedBy | a383154 | en_AU |
local.publisher.url | https://iopscience.iop.org | en_AU |
local.type.status | Accepted Version | en_AU |
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