  We present results from a global view on the colliding-wind binary WR 147. We
analysed new optical spectra of WR 147 obtained with Gran Telescopio CANARIAS
and archive spectra from the Hubble Space Telescope by making use of modern
atmosphere models accounting for optically thin clumping. We adopted a
grid-modelling approach to derive some basic physical characteristics of both
stellar components in WR 147. For the currently accepted distance of 630 pc to
WR 147, the values of mass-loss rate derived from modelling its optical spectra
are in acceptable correspondence with that from modelling its X-ray emission.
However, they give a lower radio flux than observed. A plausible solution for
this problem could be if the volume filling factor at large distances from the
star (radio-formation region) is smaller than close to the star
(optical-formation region). Adopting this, the model can match well both
optical and thermal radio emission from WR 147. The global view on the
colliding-wind binary WR 147 thus shows that its observational properties in
different spectral domains can be explained in a self-consistent physical
picture.
