factor ($\sim 10^7$) and the number density nearly equal to the GJ density, and the secondary electron/positron plasma with relatively small bulk streaming Lorentz factor ($\sim 10$ - $10^3$) and the large pair multiplicity ($\sim 10^3$ - $10^5$) in the radio emitting region (e.g., Melrose 1995; Lyutikov, Blandford & Machabeli 1999; Gedalin, Gruman & Melrose 2002). However, the existence of pair starved MSPs suggests that the radio emission mechanisms should be insensitive to the particle number density down to sub-GJ number density. The pulsar radio emission mechanism is still poorly understood, so that the observationally-based constraints are valuable [@M95]. Therefore, another verification for the extent of the MSP multiplicity, especially the existence of the pair starved MSPs is important for the pulsar radio emission mechanisms.

Recently, HESS has discovered a new TeV source, which is located in the close vicinity of the globular cluster Terzan 5 [@HE11]. Several globular clusters, including Terzan 5 also emit GeV $\gamma$-ray [@Ab09b; @KHC10; @Ab10b; @Ta11], which may plausibly be due to a number of MSPs residing in these clusters [@HUM05; @VDC09]. Thus, inverse Compton scattering by the high-energy particles ejected from MSPs are proposed for the origin of the observed TeV emission [@BS07; @VDC09]. 