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- W3103641712 abstract "CS 22949--037 is one of the most metal-poor giants known ([Fe/H]$ approx-4.0$), and it exhibits large overabundances of carbon and nitrogen (Norris et al.). Using VLT-UVES spectra of unprecedented quality, regarding resolution and S/N ratio, covering a wide wavelength range (from $lambda = 350$ to 900 nm), we have determined abundances for 21 elements in this star over a wide range of atomic mass. The major new discovery is an exceptionally large oxygen enhancement, [O/Fe] $= 1.97pm0.1$, as measured from the [OI] line at 630.0 nm. We find an enhancement of [N/Fe] of $2.56pm 0.2$, and a milder one of [C/Fe] $= 1.17pm$0.1, similar to those already reported in the literature. This implies $Z_{star}=0.01 Z_{odot}$. We also find carbon isotopic ratios $^{12}$C/$^{13}$C$ =4pm2.0$ and $^{13}$C/$^{14}$N$ =0.03 ^{+0.035}_{-0.015}$, close to the equilibrium value of the CN cycle. Lithium is not detected. Na is strongly enhanced ([Na/Fe] $= +2.1 pm 0.2$), while S and K are not detected. The silicon-burning elements Cr and Mn are underabundant, while Co and Zn are overabundant ([Zn/Fe]$ = +0.7$). Zn is measured for the first time in such an extremely metal-poor star. The abundances of the neutron-capture elements Sr, Y, and Ba are strongly decreasing with the atomic number of the element: [Sr/Fe] $approx +0.3$, [Y/Fe] $approx -0.1$, and [Ba/Fe] $approx -0.6$. Among possible progenitors of CS 22949--037, we discuss the pair-instability supernovae. Such very massive objects indeed produce large amounts of oxygen, and have been found to be possible sources of primary nitrogen. Other scenarios are also discussed. A 30-40$M_{odot}$ supernova, with fallback, seems the most likely progenitor for CS 22949--037." @default.
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- W3103641712 date "2002-05-15" @default.
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- W3103641712 title "First Stars II. Elemental abundances in the extremely metal-poor star CS 22949--037: A diagnostic of early massive supernovae" @default.
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