Detailed abundance study of four s-process enriched post-AGB stars in the Large Magellanic Cloud

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Table 4

Expected equivalent widths of the strongest He lines (at 4471.50, 5875.65 and 5876.50 Å), and iron abundances for the best atmosphere model for a range of effective temperatures for J050632.

T_eff	Expected EW (mÅ)			log ϵ_FeI^a	log ϵ_FeII^a
(K)	4471.50	5875.65	5876.50	(dex)	(dex)

6250	0.7	0.3	0.3	5.69 ± 0.23	6.20 ± 0.23
6500	4.6	1.1	1.2	5.89 ± 0.20	6.25 ± 0.20
6750	10.5	2.8	3.0	6.09 ± 0.18	6.28 ± 0.15
7000	17.6	5.6	6.0	6.34 ± 0.17	6.37 ± 0.12

Notes.

^(a)

The listed errors are the line-to-line scatter. The Fe i abundance is based on the measurements of 63 lines and that of Fe ii on 30.

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