  We study the broad-band spectral energy distribution (SED) of the
prototypical low-mass active galactic nucleus (AGN) in NGC 4395. We jointly
model the optical through mid-infrared SED with a combination of galaxy and AGN
light, and find that on arcsecond scales, the AGN dominates at most
wavelengths. However, there is still some ambiguity about emission from the
galaxy, owing partially to the strong short-term variability of the black hole.
We investigate the use of smooth and clumpy-torus models in order to
disentangle the nuclear infrared emission, as well as exploring the use of
poloidal wind emission to account for the blue spectral slope observed in the
near-IR. Even when simultaneously fitting the full optical-IR spectral range,
we find that degeneracies still remain in the best-fit models. We conclude that
high spatial resolution and wider wavelength coverage with the James Webb Space
Telescope is needed to understand the mid-infrared emission in this complex
highly-variable object, which is the best nearby example to provide a blueprint
to finding other low-mass AGN via their mid-infrared emission in the future.
