V4334 Sgr is a star which underwent a very late Helium shell flash in 1995 [1,2]. The last known similar event was V605Aql in 1919. V4334 Sgr has shown fast and massive changes including the development of a strong infrared excess as a direct result of mass loss and the formation of hot dust. We have monitored V4334 Sgr in the mid-IR since 1997, witnessing the mass loss to vary by a factor of 40 and strong variations in mid-IR brightness as the freshly formed dust cooled. Our data demonstrated that the formation of dust has stopped in mid 2001 and that the circumstellar matter continues to expand quickly. Here we report the first mid-IR spectra from Sept. 2003 which show complex solid state features. Potentially there is also indicate a tentative detection of the [Nesc ii] line at 12.8 μm. The mid-IR monitoring is continuing and is now at the crucial point to witness the increase in the central star’s temperature, when it leaves the asymptotic giant branch for a second time.