  The complete mid- to far- infrared continuum energy distribution collected
with the Infrared Space Observatory of the Seyfert 2 prototype NGC 5252 is
presented. ISOCAM images taken in the 3--15 micron range show a resolved
central source that is consistent at all bands with a region of about 1.3 kpc
in size. Due to the lack of on going star formation in the disk of the galaxy,
this resolved emission is associated with either dust heated in the nuclear
active region or with bremsstrahlung emission from the nuclear and extended
ionised gas. The size of the mid-IR emission contrasts with the standard
unification scenario envisaging a compact dusty structure surrounding and
hiding the active nucleus and the broad-line region. The mid-IR data are
complemented with ISOPHOT aperture photometry in the 25--200 micron range. The
overall IR spectral energy distribution is dominated by a well-defined
component peaking at about 100$ micron, a characteristic temperature of T ~20
K, and an associated dust mass of 2.5 x 10E7 Msun, which greatly dominates the
total dust mass content of the galaxy. The heating mechanism of this dust is
probably the interstellar radiation field. After subtracting the contribution
of this cold dust component, the bulk of the residual emission is attributed to
dust heated within the nuclear environment. Its luminosity consistently
accounts for the reprocessing of the X-ray to UV emission derived for the
nucleus of this galaxy. The comparison of NGC 5252 spectral energy distribution
with current torus models favors large nuclear disk structure on the kiloparsec
scale.
