Discovery of the Energetic Pulsar J1747-2809 in the Supernova Remnant G0.9+0.1
Abstract
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} = 4.3×10^{37} 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 40 μJy at 2 GHz.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- July 2009
- DOI:
- 10.1088/0004-637X/700/1/L34
- arXiv:
- arXiv:0906.3289
- Bibcode:
- 2009ApJ...700L..34C
- Keywords:
-
- ISM: individual: G0.9+0.1;
- pulsars: individual: PSR J1747–2809;
- stars: neutron;
- Astrophysics - Galaxy Astrophysics;
- Astrophysics - High Energy Astrophysical Phenomena
- E-Print:
- minor changes from v1 - matches published version