  Shocks driven by Coronal Mass Ejections (CMEs) are primary agents of space
weather. They can accelerate particles to high energies and can compress the
magnetosphere thus setting in motion geomagnetic storms. For many years, these
shocks were studied only in-situ when they crossed over spacecraft or remotely
through their radio emission spectra. Neither of these two methods provides
information on the spatial structure of the shock nor on its relationship to
its driver, the CME. In the last decade, we have been able to not only image
shocks with coronagraphs but also measure their properties remotely through the
use of spectroscopic and image analysis methods. Thanks to instrumentation on
STEREO and SOHO we can now image shocks (and waves) from the low corona,
through the inner heliosphere, to Earth. Here, we review the progress made in
imaging and analyzing CME-driven shocks and show that joint coronagraphic and
spectrscopic observations are our best means to understand shock physics close
to the Sun.
