We present multiwavelength studies of the 106.6 ms \gamma -ray pulsar PSR J1907+06 near the TeV source MGRO J1908+06 .
Timing observations with Fermi result in a precise position determination for the pulsar of R.A. = 19 ^ { \mathrm { h } } 07 ^ { \mathrm { m } } 54 \fs 7 ( 2 ) , decl .
= +06 ^ { \circ } 02′16 ( 2 ) ^ { \prime \prime } placing the pulsar firmly within the TeV source extent , suggesting the TeV source is the pulsar wind nebula of PSR J1907+0602 .
Pulsed \gamma -ray emission is clearly visible at energies from 100 MeV to above 10 GeV .
The phase-averaged power-law index in the energy range E > 0.1 GeV is \Gamma = 1.76 \pm 0.05 with an exponential cutoff energy E _ { c } = 3.6 \pm 0.5 GeV .
We present the energy-dependent \gamma -ray pulsed light curve as well as limits on off-pulse emission associated with the TeV source .
We also report the detection of very faint ( flux density of \simeq 3.4 \mu Jy ) radio pulsations with the Arecibo telescope at 1.5 GHz having a dispersion measure DM = 82.1 \pm 1.1 cm ^ { -3 } pc .
This indicates a distance of 3.2 \pm 0.6 kpc and a pseudo-luminosity of L _ { 1400 } \simeq 0.035 mJy kpc ^ { 2 } .
A Chandra ACIS observation revealed an absorbed , possibly extended , compact ( \lower 2.15 pt \hbox { $ \buildrel < \over { \sim } $ } 4 ^ { \prime \prime } ) X-ray source with significant non-thermal emission at R.A. = 19 ^ { \mathrm { h } } 07 ^ { \mathrm { m } } 54 \fs 76 , decl .
= +06°02′14.6 ^ { \prime \prime } with a flux of 2.3 ^ { +0.6 } _ { -1.4 } \times 10 ^ { -14 } { erg } { cm } ^ { -2 } { s } ^ { -1 } .
From archival ASCA observations , we place upper limits on any arcminute scale 2–10 keV X-ray emission of \sim 1 \times 10 ^ { -13 } { erg } { cm } ^ { -2 } { s } ^ { -1 } .
The implied distance to the pulsar is compatible with that of the supernova remnant G40.5 - 0.5 , located on the far side of the TeV nebula from PSR J1907+0602 , and the S74 molecular cloud on the nearer side which we discuss as potential birth sites .