  Genuine spectral energy distributions (SEDs) of the central few parsec of the
nearest and brightest active galaxies in the Southern Hemisphere are presented.
They are compiled from very high spatial resolution observations in the radio
(VLBA), the infrared (using adaptive optics and interferometry) and the optical
(HST). The SEDs are characterized by two main emission bumps peaking in the
X-rays and in the infrared respectively, as it is known from optically obscured
galactic nuclei. Yet, the SED shape of the IR largely departs from the one
derived from large aperture data. It reveals two new features: (1) a very sharp
decay at wavelengths shortward of 2 $\mu$m, plausibly a consequence of the
heavy extinction towards the core region and (2) a flattening in the 10-20
$\mu$m range as well as a downturn toward longer wavelengths. Accordingly, the
true bolometric luminosity of these core regions turns out to be about an order
of magnitude lower than previously estimated on the basis of IRAS/ISO data.
These findings indicate that large aperture IR data are largely dominated by
the contribution of the host galaxy. They warn against over-interpretations of
IR/X-ray and IR/optical correlations based on large aperture IR data which are
used to differentiate AGN from normal galaxy populations.
  The new derived IR bolometric luminosities still exceed the output energy
measured in the high energies by factors from 3 to 60. With the expectation
that both luminosities should be comparable within an order of magnitude, the
reduced factors between both suggests that the derived IR luminosities are
getting closer to the genuine power output of the core.
