  The COMPTEL observations of the diffuse galactic 1.809 MeV emission
attributed to the radioactive decay of 26Al have confirmed the diffuse nature
of this interstellar emission line. One of the most significant features of the
reconstructed intensity pattern is a flux enhancement in the direction of the
Cygnus region. This region is fairly young and contains a wealth of massive
stars, most of them grouped in the Cygnus OB associations. Multi-frequency
model fitting strongly supports the hypothesis of massive stars and their
descendent supernovae being the dominant sources of interstellar 26Al as
observed by COMPTEL.
  Massive stars and supernovae are known to impart a large amount of kinetic
energy into the surrounding ISM which lead to shockregions and large cavities.
In addition, a large fraction of the electro-magnetic radiation of massive
stars lies in the extreme ultra-violet causing photoionisation of the
surrounding interstellar medium.
  We applied a population synthesis model in combination with an analytic model
of the expansion of superbubbles to the Cygnus OB associations. The model
predicts the expected 1.809 MeV flux and the gamma-ray line intensity due to
interstellar 60Fe. We compute the sizes and expansion parameters of the
expected HI-structures and the free-free emission intensities due to the
photoionizing radiation from massive stars within this region of the sky. We
discuss our present understanding of the Cygnus region with respect to the
massive star census and history. Our model assigns about 70% of the 1.809 MeV
intensity to six known OB associations, about 20% to known isolated sources and
roughly 10% to an unkown diffuse component.
