  The discovery of extended TeV emission around the Geminga and PSR B0656+14
pulsars, with properties consistent with free particle propagation in the
interstellar medium (ISM), has sparked considerable discussion on the possible
presence of such halos in other systems. Here we make an assessment of the
current TeV source population associated with energetic pulsars, in terms of
size and estimated energy density. Based on two alternative estimators we
conclude that a large majority of the known TeV sources have emission
originating in the zone energetically and dynamically dominated by the pulsar
(i.e. the pulsar wind nebula), rather than from a halo of particles diffusing
in to the ISM. Furthermore, whilst the number of established halos will surely
increase in the future, we find that it is unlikely that such halos contribute
significantly to the total TeV $\gamma$-ray luminosity from electrons
accelerated in PWN.
