Pulsar Wind Nebulae (PWNe) are generally believed to be the sites generating high energy galactic cosmic rays. PSR B1706-44 is a young pulsar having emission detected from radio band to gamma-ray band. In the X-ray band, its PWN shows a typical structure for young PWN with a torus/jet structure. To further understand such structure, this research focuses on the radio emission and magnetic field of this PWN, at 3cm and 6cm using the Australia Telescope Compact Array (ATCA). We generated radio images at 10" and 20" resolutions (compatible with Chandra X-ray Observations) and discovered a two-lobe structure with highly (~40%) linearly polarized emission. A brighter (~ 30 mJy at 6cm) lobe to the east of the pulsar has a diameter of ~1.5'. Another lobe to the west shows a linear morphology extending ~1.5' southwest. Most of the radio emission is found beyond the X-ray PWN, and there is no significant emission at the X-ray torus and jet position. Besides, we found that the PWN has a toroidal magnetic field structure and the radio spectral index is around -0.3, which are compatible with what simulations suggested for young PWNe.
American Astronomical Society Meeting Abstracts #235
- Pub Date:
- January 2020