with the Geminga and Monogem pulsars. In this talk, I will show that<br><br>
these detections have significant implications for our understanding<br><br>
of pulsar emission. First, the spectrum and intensity of these TeV<br><br>
Halos indicates that a large fraction of the pulsar spindown energy is<br><br>
efficiently converted into electron-positron pairs. This provides<br><br>
observational evidence supporting pulsar interpretations of the rising<br><br>
positron fraction observed by PAMELA and AMS-02. Second, the isotropic<br><br>
nature of this emission provides a new avenue for detecting nearby<br><br>
pulsars with radio beams that are not oriented towards Earth. Lastly,<br><br>
I will show that the total emission from all unresolved pulsars<br><br>
produces the majority of the TeV gamma-ray flux observed from the<br><br>
Milky Way.