  Context. Observations of edge-on disks are an important tool for constraining
general protoplanetary disk properties that cannot be determined in any other
way. However, most radiative transfer models cannot simultaneously reproduce
the spectral energy distributions (SEDs) and resolved scattered light and
submillimeter observations of these systems, due to the differences in geometry
and dust properties at different wavelengths. Aims. We simultaneously constrain
the geometry of the edge-on protoplanetary disk HH 48 NE and the
characteristics of the host star. HH 48 NE is part of the JWST early release
science program Ice Age. This work serves as a stepping stone towards a better
understanding of the disk physical structure and icy chemistry in this
particular source. This kind of modeling lays the groundwork for studying other
edge-on sources to be observed with the JWST. Methods. We fit a parameterized
dust model to HH 48 NE by coupling the radiative transfer code RADMC-3D and an
MCMC framework. The dust structure was fitted independently to a compiled SED,
a scattered light image at 0.8 ${\mu}$m and an ALMA dust continuum observation
at 890 ${\mu}$m. Results. We find that 90% of the dust mass in HH 48 NE is
settled to the disk midplane, less than in average disks, and that the
atmospheric layers of the disk contain exclusively large grains (0.3-10
${\mu}$m). The exclusion of small grains in the upper atmosphere likely has
important consequences for the chemistry due to the deep penetration of
high-energy photons. The addition of a relatively large cavity (ca. 50 au in
radius) is necessary to explain the strong mid-infrared emission, and to fit
the scattered light and continuum observations simultaneously.
