  FU Orionis-type stars form a small class of variable Young Stellar Objects,
defined by an optical outburst of 5-6 mag followed by gradual fading on a
timescale of decades. Since the phenomenon is connected to the circumstellar
medium the infrared emission spectrum is also expected to change after the
outburst. The fading phase after the outburst is well documented in the
optical/near-infrared, but not at far-infrared wavelengths.
  We investigated the brightness evolution of 7 FU Orionis systems in the 1-200
\mu m wavelength range. We compiled spectral energy distributions (SEDS) using
data from the Infared Space Observatory, 2MASS and MSX (these observations were
performed around 1995-1998). These SEDs were compared with earlier ones based
on IRAS photometry and ground-based observations carried out around 1983.
  During this period of 15 years some objects remained unchanged, while others
became fainter, but only in the near- and mid-infrared part of the spectrum.
Since the wavelength dependence of the fading provides crucial information on
the physics of the phenomenon, we studied in detail the case of V1057 Cyg.
