  We present the 2-D photometric decomposition of the Virgo galaxy IC3328. The
analysis of the global light distribution of this morphologically classified
nucleated dwarf elliptical galaxy (dE1,N) reveals a tightly wound, bi-symmetric
spiral structure with a diameter of 4.5 kpc, precisely centered on the nucleus
of the dwarf. The amplitude of the spiral is only three percent of the dwarf's
surface brightness making it the faintest and smallest spiral ever found in a
galaxy. In terms of pitch angle and arm winding the spiral is similar to the
intermediate-type galaxy M51, but it lacks the dust and prominent HII regions
which signal the presence of gas. The visual evidence of a spiral pattern in an
early-type dwarf galaxy reopens the question on whether these dwarfs are
genuine rotationally supported or anisotropic stellar systems. In the case of
IC3328, we argue for a nearly face-on disk (dS0) galaxy with an estimated
maximum rotation velocity of v_c,max = 55kms-1. The faintness of the spiral and
the small motions within it, suggests that we could be seeing swing-amplified
noise. The other possibility is a tidal origin, caused by the near passage of a
small companion.
