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(Referência obtida automaticamente do Web of Science, por meio da informação sobre o financiamento pela FAPESP e o número do processo correspondente, incluída na publicação pelos autores.)


Texto completo
Placco, Vinicius M. [1] ; Kennedy, Catherine R. [2, 3] ; Rossi, Silvia [1] ; Beers, Timothy C. [2, 3] ; Lee, Young Sun [2, 3] ; Christlieb, Norbert [4] ; Sivarani, Thirupathi [5] ; Reimers, Dieter [6] ; Wisotzki, Lutz [7]
Número total de Autores: 9
Afiliação do(s) autor(es):
[1] Univ Sao Paulo, Dept Astron, Inst Astron Geofis & Ciencias Atmosfer, BR-05508900 Sao Paulo - Brazil
[2] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 - USA
[3] Michigan State Univ, JINA, E Lansing, MI 48824 - USA
[4] Univ Heidelberg, Zentrum Astron, D-69117 Heidelberg - Germany
[5] Indian Inst Astrophys, Bangalore 560034, Karnataka - India
[6] Univ Hamburg, D-21029 Hamburg - Germany
[7] Astrophys Inst Potsdam, D-14482 Potsdam - Germany
Número total de Afiliações: 7
Tipo de documento: Artigo Científico
Fonte: ASTRONOMICAL JOURNAL; v. 139, n. 3, p. 1051-1065, MAR 2010.
Citações Web of Science: 17

We have developed a new procedure to search for carbon-enhanced metal-poor (CEMP) stars from the Hamburg/ESO (HES) prism-survey plates. This method employs an extended line index for the CH G band, which we demonstrate to have superior performance when compared to the narrower G-band index formerly employed to estimate G-band strengths for these spectra. Although CEMP stars have been found previously among candidate metal-poor stars selected from the HES, the selection on metallicity undersamples the population of intermediate-metallicity CEMP stars (-2.5 <= {[}Fe/H] <= -1.0); such stars are of importance for constraining the onset of the s-process in metal-deficient asymptotic giant branch stars (thought to be associated with the origin of carbon for roughly 80% of CEMP stars). The new candidates also include substantial numbers of warmer carbon-enhanced stars, which were missed in previous HES searches for carbon stars due to selection criteria that emphasized cooler stars. A first subsample, biased toward brighter stars (B < 15.5), has been extracted from the scanned HES plates. After visual inspection (to eliminate spectra compromised by plate defects, overlapping spectra, etc., and to carry out rough spectral classifications), a list of 669 previously unidentified candidate CEMP stars was compiled. Follow-up spectroscopy for a pilot sample of 132 candidates was obtained with the Goodman spectrograph on the SOAR 4.1 m telescope. Our results show that most of the observed stars lie in the targeted metallicity range, and possess prominent carbon absorption features at 4300 angstrom. The success rate for the identification of new CEMP stars is 43% (13 out of 30) for {[}Fe/H] < -2.0. For stars with {[}Fe/H] < -2.5, the ratio increases to 80% (four out of five objects), including one star with {[}Fe/H] < -3.0. (AU)

Processo FAPESP: 07/04356-3 - Busca por estrelas muito pobres em metais baseada no enriquecimento em carbono
Beneficiário:Vinicius Moris Placco
Linha de fomento: Bolsas no Brasil - Doutorado