  We have modeled optical to far infrared images, photometry, and spectroscopy
of the object known as Gomez's Hamburger. We reproduce the images and spectrum
with an edge-on disk of mass 0.3M_sun and radius 1600AU, surrounding an A0 III
star at a distance of 280pc. Our mass estimate is in excellent agreement with
recent CO observations. However, our distance determination is more than an
order of magnitude smaller than previous analyses which inaccurately
interpreted the optical spectrum. To accurately model the infrared spectrum we
have extended our Monte Carlo radiation transfer codes to include emission from
polycyclic aromatic hydrocarbon (PAH) molecules and very small grains (VSG). We
do this using pre-computed PAH/VSG emissivity files for a wide range of values
of the mean intensity of the exciting radiation field. When Monte Carlo energy
packets are absorbed by PAHs/VSGs we reprocess them to other wavelengths by
sampling from the emissivity files, thus simulating the absorption and
re-emission process without reproducing lengthy computations of statistical
equilibrium, excitation and de-excitation in the complex many level molecules.
Using emissivity lookup tables in our Monte Carlo codes gives the flexibility
to use the latest grain physics calculations of PAH/VSG emissivity and opacity
that are being continually updated in the light of higher resolution infrared
spectra. We find our approach gives a good representation of the observed PAH
spectrum from the disk of Gomez's Hamburger. Our models also indicate the
PAHs/VSGs in the disk have a larger scaleheight than larger radiative
equilibrium grains, providing evidence for dust coagulation and settling to the
midplane.
