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With the advent of state-of-the-art 3D radiation transfer codes, it is
becoming easier to reproduce the spectral energy distributions and images
of young stellar objects. On the other hand, the price to pay is the
increasingly difficulty to explore large sections of parameter space,
and to determine which parameters are actually constrained by the observations.
In this talk, I will discuss our previous work on interpreting the
spectral energy distributions of young stellar objects, and how we plan to
expand this work in future, including the modeling of images. Our main goal
is to provide a rapid initial exploration of parameter space in order to
understand what parameter degeneracies are present. I will also briefly
discuss a new Monte-Carlo radiation transfer code that we are developing
as part of this project, and which will include the latest techniques in
the field (AMR, PAH emission, parallel code).
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