  The recent discovery of the so-called TeV halos has attracted much attention.
The morphology of the emission requires that the region is characterized by
severe suppression of the diffusion coefficient. This finding raises many
questions as to its origin: 1) is the suppressed diffusion to be attributed to
instabilities induced by the same radiating particles? 2) or does it actually
show that the diffusion coefficient is small throughout the disc of the Galaxy?
In both cases, one would expect that the surroundings of supernova remnants
(SNRs) should also show evidence of reduced diffusion coefficient, since most
remnants are located in the disc and are expected to be sites of effective
particle acceleration. Should we expect the existence of regions of extended
$\gamma$-ray emission from these regions as well? Here we investigate the
transport of cosmic rays (CRs) escaped from SNRs in order to assess the
viability of the idea of having a cocoon of suppressed diffusion around them. A
comparison of our results with the $\gamma$-ray emission from the regions
around HB9 and W28 does not provide solid evidence of reduced diffusivity.
However, if indeed the phenomenon of reduced diffusivity occurs around SNRs
surrounded by molecular clouds, our calculations show that the effects on the
grammage of Galactic CRs can be significant.
