  Current gamma-ray observatories have made substantial advances in the study
of potential cosmic ray accelerators such as supernova remnants (SNRs), but the
study of cosmic rays in flight from their parent accelerators remains a topic
of great interest. The Fermi Gamma-ray Space Telescope (FGST) discovered a four
square degree region of gamma-ray emission between 3 GeV and 100 GeV. This
structure lies between the Cygnus OB2 association and the gamma-Cygni SNR,
which is bright in gamma rays above 10 GeV. The atmospheric Cherenkov
observatory VERITAS also sees VHE (> 100 GeV) gamma-ray emission from the
direction gamma-Cygni (VER J2019+407). We discuss the relationship of VER
J2019+407 to both the gamma-Cygni SNR and the cocoon. Toy model simulations are
used to evaluate prospects for detecting the cocoon at very high energies with
VERITAS, as well as ways in which cocoon emission at these energies could
impact measurements of the morphology and spectrum of VER J2019+407.
