Discovery of the Energetic Pulsar J1747–2809 in the Supernova Remnant G0.9+0.1

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 Ė = 4.3×1037 erg s−1, the second largest among known Galactic pulsars. With a dispersion measure of DM = 1133 pc cm−3, PSR J1747–2809 is distant, at ≈ 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 40μJy at 2 GHz. Subject headings: ISM: individual (G0.9+0.1) – pulsars: individual (PSR J1747–2809) – stars: neutron