Multifrequency radio observations of SNR J0536-6735 (N 59B) with associated pulsar

TL;DR

This study presents new radio observations of SNR J0536-6735, revealing its shell morphology, flux density, and a pulsar wind nebula association, despite interference from an embedded HII region.

Contribution

It provides detailed radio-continuum analysis of SNR J0536-6735, including flux, spectral index, and polarization measurements, and confirms the remnant's association with a pulsar wind nebula.

Findings

Shell morphology with 36x29 pc size

Detection of a pulsar wind nebula

Surface brightness at 1 GHz of 2.55x10^-21 W m^-2 Hz^-1 sr^-1

Abstract

We present a study of new Australian Telescope Compact Array (ATCA) observations of supernova remnant, SNR J0536-6735. This remnant appears to follow a shell morphology with a diameter of D=36x29 pc (with 1 pc uncertainty in each direction). There is an embedded Hii region on the northern limb of the remnant which made various analysis and measurements (such as flux density, spectral index and polarisation) difficult. The radio-continuum emission followed the same structure as the optical emission, allowing for extent and flux density estimates at 20 cm. We estimate a surface brightness for the SNR at 1 GHz of 2.55x10^-21 W m^-2 Hz^-1 sr^-1. Also, we detect a distinctive radio-continuum point source which confirms the previous suggestion of this remnant being associated with a pulsar wind nebulae (PWN). The tail of this remnant isn't seen in the radio-continuum images and is only seen in the optical and X-ray images.