  Nearby galaxies, spirals as well as irregulars, have been found to be much
larger than previously believed. The structure of the huge spheroid surrounding
dwarf galaxies could give clues to their past gravitational history. Thanks to
wide field imagers, nearby galaxies with diameter of dozens of arcmin can be
effectively surveyed.
  We obtain, from the CFHT archives, a series of i' and g' MegaCam images of IC
1613 in order to determine the stellar surface density of the field and
determine the shape of its spheroid. From the colour magnitude diagram we
select some 36,000 stars, in the first three magnitudes of the red giant
branch. The spatial distribution of these stars is used to establish the
structure of the spheroid.
  The position angle of the major axis of the stellar spheroid is found to be
$\approx 90^\circ$, some 30$^\circ$ from the major axis of the HI cloud
surrounding IC 1613. The surface density profile of the spheroid is not
exponential over all the length of the major axis. A King profile, with a core
radius of 4.5' and a tidal radius of 24' fits the data. The tidal truncation of
the spheroid suggests that IC 1613 is indeed a satellite of M31.
