Table 1 Chemical abundances of J1124+4535

From: Evidence for the accretion origin of halo stars with an extreme r-process enhancement

Element X log(NX/NH + 12) [X/Fe] N lines σ
Fe i 6.23 0.00 95 0.10
Fe ii 6.23 0.00 10 0.09
C (CH) 6.74 −0.42 0.20
Na i 4.08 −0.89 2 0.13
Mg i 6.02 −0.31 3 0.09
Si I 6.06 −0.18 4 0.08
Ca i 4.98 −0.09 12 0.08
Sc ii 1.73 −0.15 6 0.09
Ti i 3.63 −0.05 8 0.09
Ti ii 3.81 0.13 7 0.10
Cr i 4.04 −0.33 6 0.08
Mn i 3.84 −0.32 4 0.10
Ni i 4.60 −0.35 6 0.10
Zn i 2.92 −0.37 2 0.09
Sr ii 1.24 −0.36 2 0.10
Y ii 0.76 −0.18 4 0.13
Zr ii 1.44 0.13 2 0.14
Ba ii 1.15 0.24 4 0.12
La ii 0.51 0.68 6 0.09
Ce ii 0.72 0.41 4 0.13
Pr ii 0.20 0.75 4 0.13
Nd ii 0.81 0.66 15 0.14
Sm ii 0.52 0.83 14 0.13
Eu ii 0.35 1.10 1 0.10
Gd ii 0.63 0.83 2 0.13
Dy ii 0.74 0.91 2 0.15
Er ii <0.7 <1.05 1
Th ii <−0.16 <1.09 1
  1. Abundance ratios for J1124+4535 as derived from Subaru/HDS spectra. The abundance of Fe i and solar abundances from literature37 are adopted for obtaining [X/Fe]. The error is the quadratic sum of the random error and errors due to the stellar parameter uncertainties (δTeff = 100 K, δlog g = 0.3 dex and δVmicro = 0.3 km s−1, where δTeff is the uncertainty of effective temperature, δlog g is the uncertainty of surface gravity, and δVmicro is the uncertainty of the microturbulent velocity). The random error is estimated to be συ \(N_{\mathrm{lines}}^{-1/2}\), where συ is the dispersion around the mean abundance obtained from different lines for each species, and Nlines is the number of lines used to derive abundance. The συ of Fe i is adopted for species with Nlines < 3. For C and Eu abundances measured by spectral synthesis, the errors are estimated based on comparison with synthetic spectra.