Radio properties of the low surface brightness SNR G65.2+5.7

摘要

Context. SNR G65.2+5.7 is one of few supernova remnants (SNRs) that have been optically detected. It is exceptionally bright in X-rays and the optical [O 3]-line. Its low surface brightness and large diameter ensure that radio observations of SNRG65.2+5.7 are technically difficult and thus have hardly been completed. Aims. Many physical properties of this SNR, such as spectrum and polarization, can only be investigated by radio observations. Methods. The 11 cm and 6cm continuum and polarization observations of SNRG65.2+5.7 were completed with the Effelsberg 100-m and the Urumqi 25-m telescopes, respectively, to investigate the integrated spectrum, the spectral index distribution, and the magnetic field properties. Archival 21cmdata of the Effelsberg 100-m telescope were also used. Results. The integrated flux densities of G65.2+5.7 at cm and cm are Jy and Jy, respectively. The power-law spectrum ()is well fitted by from 83MHz to 4.8GHz. Spatial spectral variations are small. Along the northern shell, strong depolarizion is observed at both wavelengths. The southern filamentary shell of SNRG65.2+5.7 is polarized by as much as54% at cm. There is significant depolarization at cm and confusion with diffuse polarized Galactic emission. Using equipartition principle, we estimated the magnetic field strength for the southern filamentary shell to be between 20G (filling factor1) and 50G (filling factor0.1). A faint HIshell may be associated with theSNR. Conclusions. Despite its unusually strong X-ray and optical emission and its very low surface brightness, the radio properties of SNRG65.2+5.7 are found to be typical of evolved shell-type SNRs. SNRG65.2+5.7 may be expanding in a pre-blown cavity as indicated by a deficit of HI gas and a possible HI-shell. Key words: ISM: supernova remnants - ISM: magnetic fields - radio continuum: ISM - radiation mechanisms: non-thermal