All Figures

Figure 1: The spectral energy distribution of MACHO 47.2496.8 as in Reyniers et al. (2007), but updated with Spitzer SAGE fluxes, revealing the presence of circumstellar dust. Diamonds are the measured magnitudes (from blue to red): Geneva U, B, V and Cousins R taken with C2+Euler; I from DENIS (in gray), SAAO J, H, K, and the Spitzer SAGE fluxes (3.6, 4.5, 5.8, 8.0, and 24 m). The MARCS model is shown in gray, while a smoothed version is shown with a full black line. The I magnitude could not be fitted, possibly due to a phase difference.

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In the text

Figure 2: Distribution of [hs/ls] ( upper panels) and [Pb/hs] ( lower panels) ratios in synthesized populations of intrinsically s-process enhanced post-AGB stars, calculated with different values of , as indicated over each panel. The grey scale is a logarithmic measure of the number distribution of stars over the plotted s-process index. The number density is weighed by the initial mass function and by the time each star spends in an abundance bin, and then normalized for each metallicity. The results are compared to the s-process element ratios observed in MACHO 47.2496.8, indicated by the crosses. The size of the vertical and horizontal lines indicate the observational errors of the data and the arrow indicates that the observed [Pb/hs] ratio is an upper limit.

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In the text

Figure 3: Distribution of [ls/Fe] ( upper panel) and [hs/Fe] ( lower panel) ratios in a synthetic population of intrinsically s-process enhanced post-AGB stars, calculated by assuming . The grey scale is a logarithmic measure of the number distribution of stars over the plotted s-process index. The number density is weighed as described in the caption of Fig. 2. The results are compared to [ls/Fe] and [hs/Fe] ratios measured in MACHO 47.2496.8, indicated by the crosses. The size of the vertical and horizontal lines indicate the errors on the data measurements.

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In the text