  Globular clusters (GCs) contain huge number of low mass stars and also large
number of millisecond pulsars (MSPs). Due to the number of stars, the stellar
and MSP winds mix efficiently within the GC. Such mixture of winds leaves GC
and interacts with the galactic medium creating a bow shock nebula around GC.
The bow shock nebula is filled with relativistic leptons accelerated in the
pulsar magnetospheres and/or wind regions. We argue that nebulae around
globular clusters, immersed in relatively dense medium close to the galactic
plane, should have complicated morphology due to interaction with the
surrounding gas. Therefore, TeV $\gamma$-ray sources, related to these nebulae,
are expected to be misaligned in respect to GC cores, as observed in the case
of GC Ter 5. On the other hand, GCs in low density medium, i.e. far away from
the galactic disk, should produce bow shocks at large distances from the GC
cores. The TeV $\gamma$-ray sources around such nebulae are expected to be
almost spherical and centred on the GC cores. We perform numerical calculations
of the TeV $\gamma$-ray emission produced by leptons escaping from the GC Ter
5. It is shown that TeV $\gamma$-ray source related to Ter 5 should be
misaligned in respect to the core of GC as observed by the HESS Collaboration.
