The electron density structure and kinematics of the supernova remnant N49

Supernova remnants commonly display strong internal inhomogeneities in physical properties; however, most of the observational studies found in the literature are limited to integrated data for extragalactic objects or data from very specific parts of the galactic objects. Thus, important information may be lost. We studied the spatial variation of the electron density and the kinematics of N49, the brightest supernova remnant in the Large Magellanic Cloud, based on spatial resolve observations sampling the whole object. The detected gradient in density confirmed a previous inference based on the decrease in the brightness ratio between the X-ray and radio emission from east and west and is consistent with the presence of a molecular cloud on the south-east border. We were able to fit the radial profile of the near side velocity using a self-similar solution of a blast wave travelling through a non-homogeneous medium characterized by a power-law density distribution.