We present the spectral energy distribution (SED) of the preplanetary nebula, IRAS 19475+3119 (hereafter I 19475), from the optical to the far-infrared. We identify emission features due to crystalline silicates in the ISO SWS spectra of the star. We have fitted the SED of I 19475 using a one-dimensional radiative transfer code and find that a shell with inner and outer radii of 8.8x1016 and 4.4x1017 cm and dust temperatures ranging from about 94 to 46 K provides the best fit. The mass of this shell is ≳1[34 cm2/g/κ(100 µm)](δ/200) M☉, where κ(100 µm) is the 100 µm dust mass absorption coefficient (per unit dust mass) and δ is the gas-to-dust ratio. In agreement with results from optical imaging and millimeter-wave observations of CO emission of I 19475, our model fits support an/r3 density law for its dust shell, with important implications for the interaction process between the fast collimated post-AGB winds and the dense AGB envelopes that results in the observed shapes of PPNs and PNs. We find that the observed JCMT flux at submillimeter wavelengths (850 µm) is a factor ∼2 larger than our model flux, suggesting the presence of large dust grains in the dust shell of I 19475 that are not accounted for by our adopted standard MRN grain size distribution.
Stars: Circumstellar Matter - ISM: Dust, Extinction - ISM: reflection nebulae - Stars: AGB and Post-AGB - stars: individual (IRAS 19475+3119) - Stars: Mass Loss