  The spectrum of HD46223 was established from the optical to the far UV and
normalized by the spectrum of a non reddened star of same spectral type. The
resulting spectrum is separated into two components. One is the direct
starlight. The second is an additional component of light scattered at small
angles.
  In the optical the spectrum is dominated by direct starlight which decreases
exponentially due to the linear extinction.
  Scattered light begins to be noticeable in the near-UV. The near-UV rise of
the scattered light is interrupted in the bump region. The wavelength
dependence of the scattered light is established in the far-UV, where scattered
light dominates the extinction curve. A 1/lambda^4 dependence is found, proving
the presence of grains small compared to UV wavelengths.
  The mathematic expressions of the different components mentionned above give
a good fit to the extinction curve in the direction of the star. On a
mathematic standpoint the fit can be completed by a Lorentzien for the 2200Ang.
bump region. The physical interpretation of the bump may be more difficult to
achieve since the paper shows the possibility that only scattered light is
extinguished in the bump region.
  Consequences for the grain size distribution which is necessary to explain
the different aspects of scattering in interstellar clouds, for the value of
Rv, and problems raised by this interpretation of the spectrum of HD46223, are
considered at the end of this paper.
