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 interferometry
data (squared visibilities and closure phases) by E. Thiébaut. 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.