Discovery of the energetic pulsar J1747-2809 in the supernova remnant G0.9+0.1

TL;DR

This paper reports the discovery of a highly energetic pulsar, PSR J1747-2809, in the supernova remnant G0.9+0.1, using radio observations that reveal its rotation period, luminosity, and distance, contributing to understanding pulsar populations.

Contribution

The study presents the first detection of radio pulsations from PSR J1747-2809, confirming its nature as an energetic pulsar within G0.9+0.1 and providing detailed measurements of its properties.

Findings

Pulsar has a 52 ms rotation period.

Spin-down luminosity is 4.3e37 erg/s.

Distant at approximately 13 kpc, possibly near Galactic center.

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 4.3e37 erg/s, the second largest among known Galactic pulsars. With a dispersion measure of 1133 pc/cc, 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 uJy at 2 GHz.