We propose CAM CVF spectral mapping of NGC4945 and IC342 in order to
follow-up and complement our ISO SWS and PHT-S studies of these starburst
galaxies. Active star formation in NGC4945 has been shown e.g. by the
detection of the [NeII] and [Ne III] lines at 12.8 and 15.5 micron. Our
current model for NGC4945 assumes a nucleus in a post-burst phase surrounded
by a starburst disk. The spectra of NGC4945 are also rich in prominent
PAH/dust features. Comparable results are to be expected for IC342.
However, due to the large aperture of the SWS spectrometer it is not
possible to disentangle the relative contributions from the burned-out
nucleus and the surrounding starburst regions to the Neon line emission.
It is also impossible to judge where exactly the PAH features, which are
generally believed to be good starburst tracers, arise: in the starburst
region itself or rather in photodissociation fronts at its outskirts.
It is therefore crucial to obtain spatially resolved information using the
CAM LW CVF to cover the [NeII] and [NeIII] lines and many of the PAH
features with adequate s/n and spatial resolution.