  The study of protoplanetary disks, where the planets are believed to form,
will certainly allow the formation of our Solar System to be understood. To
conduct observations of these objects at the milli-arcsecond scale, infrared
interferometry provides the right performances for T Tauri, FU Ori or Herbig
Ae/Be stars. However, the only information obtained so far are scarce
visibility measurements which are directly tested with models. With the outcome
of recent interferometers, one can foresee obtaining images reconstructed
independently of the models. In fact, several interferometers including IOTA
and AMBER on the VLTI already provide the possibility to recombine three
telescopes at once and thus to obtain the data necessary to reconstruct images.
In this paper, we describe the use of MIRA, an image reconstruction algorithm
developed for optical inter- ferometry data (squared visibilities and closure
phases) by E. Thiebaut. We foresee also to use the spectral information given
by AMBER data to constrain even better the reconstructed images. We describe
the use of MIRA to reconstruct images of young stellar objects out of actual
data, in particular the multiple system GW Orionis (IOTA, 2004), and discuss
the encountered difficulties.
