  We present a study on the effects of the intracluster medium (ICM) on the
interstellar medium (ISM) of 10 Virgo cluster galaxies using {\it Spitzer}
far-infrared (FIR) and VLA radio continuum imaging. Relying on the FIR-radio
correlation {\it within} normal galaxies, we use our infrared data to create
model radio maps which we compare to the observed radio images. For 6 of our
sample galaxies we find regions along their outer edges that are highly
deficient in the radio compared with our models. We believe these observations
are the signatures of ICM ram pressure. For NGC 4522 we find the radio deficit
region to lie just exterior to a region of high radio polarization and flat
radio spectral index, however the total radio continuum in this region does not
appear significantly enhanced. This scenario seems consistent for other
galaxies with radio polarization data in the literature. We also find that
galaxies having local radio deficits appear to have enhanced global radio
fluxes. Our preferred physical picture is that the observed radio deficit
regions arise from the ICM wind sweeping away cosmic-ray (CR) electrons and the
associated magnetic field, thereby creating synchrotron tails observed for some
of our galaxies. CR particles are also re-accelerated by ICM-driven shocklets
behind the observed radio deficit regions which in turn enhances the remaining
radio disk brightness. The high radio polarization and lack of coincidental
signatures in the total synchrotron power in these regions arises from shear,
and possibly mild compression, as the ICM wind drags and stretches the magnetic
field.
