Table 7
Pb abundance upper limits Pbup of the programme stars, together with the Pb indices, [Pbup/hs] and [Pbup/ls], and the effective temperature.
| Object | [Fe/H] | log ϵ(PbIup) | [PbIup/Fe] | log ϵ(PbIIup) | [PbIIup/Fe] | [Pbup/hs] | [Pbup/ls] | Teff (K) |
|
|
||||||||
| IRAS 05113+1347 | –0.49 | <2.65 | <1.44 | <–0.21 | <0.11 | 5500 | ||
| IRAS 05341+0852 | –0.54 | <3.15 | <2.10 | <–0.14 | <0.23 | 6750 | ||
| IRAS 06530-0213 | –0.32 | <4.10 | <2.73 | <4.19 | <2.76 | <0.69 | <0.98 | 7375 |
| IRAS 07134+1005 | –0.91 | <2.79 | <2.01 | <0.38 | <0.37 | 7250 | ||
| IRAS 07430+1115 | –0.31 | <2.50 | <1.07 | <–0.48 | <–0.23 | 6000 | ||
| IRAS 08143-4406a | –0.43 | <3.20 | <1.90 | <0.32 | <0.13 | 7000 | ||
| IRAS 08281-4850 | –0.26 | <4.20 | <2.74 | <4.20 | <2.71 | <1.13 | <1.14 | 7875 |
| IRAS 13245-5036 | –0.26 | <4.40 | <2.94 | <0.91 | <1.38 | 9500 | ||
| IRAS 14325-6428 | –0.56 | <3.79 | <2.60 | <1.27 | <1.35 | 8000 | ||
| IRAS 14429-4539 | –0.64 | <4.40 | <2.83 | <1.36 | <1.54 | 9375 | ||
| IRAS 17279-1119 | –0.64 | <2.75 | <1.51 | <0.59 | <0.77 | 7250 | ||
| IRAS 19500-1709 | –0.59 | <3.89 | <2.72 | <1.38 | <1.35 | 8000 | ||
| IRAS 22223+4327 | –0.30 | <3.25 | <1.82 | <0.94 | <0.48 | 6500 | ||
| IRAS 22272+5435 | –0.77 | <2.70 | <1.72 | <–0.18 | <0.11 | 5750 | ||
|
|
||||||||
| J004441.04-732136.4 | –1.34 | <3.00 | <2.58 | <0.00 | <0.52 | 6250 | ||
| J050632.10-714229.8 | –1.22 | <2.05 | <1.52 | <0.45 | <0.10 | 6750 | ||
| J052043.86-692341.0 | –1.15 | <2.00 | <1.40 | <–0.45 | <–0.27 | 5750 | ||
| J053250.69-713925.8 | –1.22 | <2.23 | <1.70 | <–0.24 | <0.19 | 5500 | ||
| J051213.81-693537.1 | –0.56 | <3.30 | <2.11 | <0.37 | <0.78 | 5875 | ||
| J051848.86-700246.9 | –1.03 | <2.62 | <1.93 | <–0.19 | <0.47 | 6000 | ||
Notes. We adopt the solar Pb abundance of log ϵ(Pb) = 1.75 dex from Asplund et al. (2009). The abundances of Pb I and Pb II are determined via the 4057.807 Å and 5608.853 Å spectral lines, respectively. The last six rows indicate the Pbup results of six post-AGB stars in the Magellanic Clouds from De Smedt et al. (2014, 2015).
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