  The detection with of the Atacama Large Millimeter Array (ALMA) of dust-rich
high redshift galaxies whose cold dust emission is spatially disconnected from
the ultraviolet emission bears a challenge for modelling their spectral energy
distributions (SED) with codes based on an energy budget between the stellar
and dust components. We test the validity of energy balance modelling on a
nearby resolved galaxy with vastly different ultraviolet and infrared spatial
distributions and infer what information can be reliably retrieved from the
analysis of the full spectral energy distribution. We use 15 broadband images
of the Antennae Galaxies ranging from far-ultraviolet to far-infrared and
divide Arp 244 into 58 square ~1 kpc$^2$ regions. We fit the data with CIGALE
to determine the star formation rate, stellar mass and dust attenuation of each
region. We compare these quantities for the addition of the 58 regions to the
ones obtained for Arp 244 as a whole and find that both estimates are
consistent within one sigma. We present the spatial distribution of these
physical parameters as well as the shape of the attenuation curve across the
Antennae Galaxies . We also observe a flattening of the attenuation curves with
increasing attenuation and dust surface density in agreement with the
predictions of hydrodynamical simulations coupled with radiative transfer
modelling.
