Silicon and strontium abundances of very metal-poor stars determined from near-infrared spectra

Silicon and strontium are key elements to explore the nucleosynthesis and chemical evolution of the Galaxy by measurements of very metal-poor stars. There are, however, only a few useful spectral lines of these elements in the optical range that are measurable for such low-metallicity stars. Here we...

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Main Authors: Aoki, W. (Author), Beers, T.C (Author), Harakawa, H. (Author), Hirano, T. (Author), Hodapp, K. (Author), Honda, S. (Author), Ishikawa, H.T (Author), Ishizuka, M. (Author), Jacobson, S. (Author), Kotani, T. (Author), Kudo, T. (Author), Kurokawa, T. (Author), Kuzuhara, M. (Author), Matsuno, T. (Author), Nishikawa, J. (Author), Omiya, M. (Author), Placco, V.M (Author), Serizawa, T. (Author), Tamura, M. (Author), Ueda, A. (Author), Vievard, S. (Author), Yoon, J. (Author)
Format: Article
Language:English
Published: Oxford University Press 2022
Subjects:
Online Access:View Fulltext in Publisher
LEADER 03166nam a2200625Ia 4500
001 10.1093-pasj-psab123
008 220510s2022 CNT 000 0 und d
020 |a 00046264 (ISSN) 
245 1 0 |a Silicon and strontium abundances of very metal-poor stars determined from near-infrared spectra 
260 0 |b Oxford University Press  |c 2022 
856 |z View Fulltext in Publisher  |u https://doi.org/10.1093/pasj/psab123 
520 3 |a Silicon and strontium are key elements to explore the nucleosynthesis and chemical evolution of the Galaxy by measurements of very metal-poor stars. There are, however, only a few useful spectral lines of these elements in the optical range that are measurable for such low-metallicity stars. Here we report on abundances of these two elements determined from near-infrared high-resolution spectra obtained with the Subaru Telescope Infrared Doppler instrument. Si abundances are determined for as many as 26 Si lines for six very and extremely metal-poor stars (-4.0 < [Fe/H] <-1.5), which significantly improves the reliability of the abundance measurements. All six stars, including three carbon-enhanced objects, show over-Abundances of Si ([Si/Fe] ∼+0.5). Two stars with [Fe/H] ∼-1.5 have relatively small over-Abundances. The [Mg/Si] ratios agree with the solar value, except for one metal-poor star with carbon excess. Strontium abundances are determined from the triplet lines for four stars, including two for the first time. The consistency of the Sr abundances determined from near-infrared and optical spectra require further examination from additional observations. © 2022 The Author(s) 2022. Published by Oxford University Press on behalf of the Astronomical Society of Japan. 
650 0 4 |a Abundance 
650 0 4 |a Abundances 
650 0 4 |a Carbon 
650 0 4 |a Chemical evolution 
650 0 4 |a Infrared devices 
650 0 4 |a Key elements 
650 0 4 |a Measurements of 
650 0 4 |a Metal-poor star 
650 0 4 |a Near infrared spectra 
650 0 4 |a Near infrared spectroscopy 
650 0 4 |a Nuclear reactions 
650 0 4 |a Nucleosynthesis 
650 0 4 |a Optical range 
650 0 4 |a Silicon 
650 0 4 |a Spectral line 
650 0 4 |a Stars 
650 0 4 |a Stars abundances 
650 0 4 |a Stars: Abundances 
650 0 4 |a Stars: Population II 
650 0 4 |a Strontium 
700 1 |a Aoki, W.  |e author 
700 1 |a Beers, T.C.  |e author 
700 1 |a Harakawa, H.  |e author 
700 1 |a Hirano, T.  |e author 
700 1 |a Hodapp, K.  |e author 
700 1 |a Honda, S.  |e author 
700 1 |a Ishikawa, H.T.  |e author 
700 1 |a Ishizuka, M.  |e author 
700 1 |a Jacobson, S.  |e author 
700 1 |a Kotani, T.  |e author 
700 1 |a Kudo, T.  |e author 
700 1 |a Kurokawa, T.  |e author 
700 1 |a Kuzuhara, M.  |e author 
700 1 |a Matsuno, T.  |e author 
700 1 |a Nishikawa, J.  |e author 
700 1 |a Omiya, M.  |e author 
700 1 |a Placco, V.M.  |e author 
700 1 |a Serizawa, T.  |e author 
700 1 |a Tamura, M.  |e author 
700 1 |a Ueda, A.  |e author 
700 1 |a Vievard, S.  |e author 
700 1 |a Yoon, J.  |e author 
773 |t Publications of the Astronomical Society of Japan