The supernova remnant G0.9+0.1 has long been inferred to contain a central energetic pulsar .
In observations with the NRAO Green Bank Telescope at 2 GHz , we have detected radio pulsations from PSR J1747–2809 .
The pulsar has a rotation period of 52 ms , and a spin-down luminosity of \dot { E } = 4.3 \times 10 ^ { 37 } erg s ^ { -1 } , the second largest among known Galactic pulsars .
With a dispersion measure of \mbox { DM } = 1133 pc cm ^ { -3 } , PSR J1747–2809 is distant , at \approx 13 kpc according to the NE2001 electron density model , although it could be located as close as the Galactic center .
The pulse profile is greatly scatter-broadened at a frequency of 2 GHz , so that it is effectively undetectable at 1.4 GHz , and is very faint , with period-averaged flux density of 40 \mu Jy at 2 GHz .