Table 7
Abundances of n-capture elements in stars of NGC 362 with UVES spectra; n is the number of lines used in the analysis.
| Star | n | [Y/Fe] ii | rms | n | [Zr/Fe] ii | rms | n | [La/Fe] ii | rms | n | [Ce/Fe] ii | rms | n | [Nd/Fe] ii | rms | n | [Eu/Fe] ii | rms | n | [Dy/Fe] ii | rms |
|
|
|||||||||||||||||||||
| 1037 | 1 | +0.00 | 0.14 | 2 | +0.46 | 0.06 | 1 | +0.30 | 0.16 | 2 | +0.13 | 0.12 | 9 | +0.28 | 0.16 | 1 | +0.66 | 0.12 | 1 | +0.75 | 0.17 |
| 12 017 | 1 | −0.13 | 0.14 | 2 | +0.40 | 0.11 | 1 | +0.17 | 0.16 | 2 | −0.06 | 0.12 | 9 | +0.20 | 0.16 | 1 | +0.57 | 0.12 | 1 | +0.58 | 0.17 |
Notes. For species with only one transition, the scatter is estimated by summing in quadrature the best fit variation obtained by changing temperature, gravity, metal abundance and microturbulent velocity in amounts corresponding to the errors in these parameters. To this, we added a fit error of 0.05 dex in quadrature.
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