We propose to study the spectral energy distribution of the
infrared emission from shock induced heating of dust in the
Tycho supernova remnant. By compairing the IR
emission from grains downstream of a shock front with the
local heating rate we expect to be able to determine the
characteristic size of the grains as a function of downstream
position.

By detailed mapping of two active regions of the shock front
and a scan across the center of the remnant we should be able
to determine dust properties both upstream and downstream of
a shock wave. By looking at many different continuum bands we
hope to be able to investigate different grain sizes and thereby
determine grain destruction mechanismes and timescales.