  Asteroids and comets (planetesimals) are created in gas- and dust-rich
protoplanetary discs. The presence of these planetesimals around main-sequence
stars is usually inferred from the detection of excess continuum emission at
infrared wavelengths from dust grains produced by destructive processes within
these discs. Modelling of the disc structure and dust grain properties for
those discs is often hindered by the absence of any meaningful constraint on
the location and spatial extent of the disc. Multi-wavelength, spatially
resolved imaging is thus invaluable in refining the interpretation of these
systems. Observations of HD 48682 at far-infrared (Spitzer,Herschel) and
sub-millimetre (JCMT, SMA) wavelengths indicated the presence of an extended,
cold debris disc with a blackbody temperature of 57.9 +\- 0.7 K. Here, we
combined these data to perform a comprehensive study of the disc architecture
and its implications for the dust grain properties. The deconvolved images
revealed a cold debris belt, verified by combining a 3D radiative transfer dust
continuum model with image analysis to replicate thestructure using a single,
axisymmetric annulus. A Markov chain Monte Carlo analysis calculated the
maximum likelihood of HD 48682's disc radius (Rdisc = 89 +17 -20 au),
fractional width(DeltaRdisc = 0.41 +0.27 -0.20), position angle (theta = 66.3
+4.5 -4.9 degrees), and inclination (phi = 112.5 +4.2 -4.2 degrees). HD 48682
has been revealed to host a collisionally active, broad disc whose emission is
dominated by small dust grains, smin approx. 0.6 microns, and a size
distribution exponent of 3.60 +\- 0.02.
