Properties of the fullerene C60-containing PN Lin49 in the SMC

Masaaki Otsuka, F. Kemper, J. Bernard-Salas, J. Cami, B. Ochsendorf, E. Peeters, R. Sahai, I. Aleman, M.L. Ferreira & A.G.G.M. Tielens

Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan

We performed a detail spectroscopic analysis of the fullerene C60-containing planetary nebula Lin49 in the Small Magellanic Cloud using the VLT 8.2-m XSHOOTER and the Spitzer/IRS. The aim of this research is to By fittings to the stellar absorption lines, we derived stellar abundances, effective temperature, and surface gravity of the central star. Based on nebular emission lines, we calculated nebular abundances of 9 elements. From these analyses, we found that the central star and the dusty nebula are C-rich and metal-deficient (Z~0.0001). The progenitor might be an old population. Compared to the nebular [S,Ar/H] abundances of ~-1.2, the extremely lower nebular [Fe/H] abundance (-2.9) suggests that most the Fe-atoms might be captured by Fe-rich dust grains. Using the synthesized spectrum of the central star, we constructed the SED model with CLOUDY to obtain central star's luminosity and the nebular gas and dust masses. Comparing to the theoretical model results of the AGB nucleosynthesis, the progenitor could be an initially ~1.3 solar mass star. The effective temperature and the size of nebula in C60 SMC PNe including Lin49 are cooler and smaller than non-C60 SMC PNe, while we do not find distinct difference in elemental abundances between them.

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