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We present a multiwavelength analysis of the supernova remnant N49 in theLarge Magellanic Cloud. Using high-resolution Hubble Space Telescope WFPC2images of H-alpha, [S II] and [O III] emission, we study the morphology of theremnant and calculate the rms electron densities in different regions. Wedetect an offset of [O III] and H-alpha emission of about 0.5 arcsec, anddiscuss possible scenarios that could give rise to such high values. Thekinematics of the remnant is analyzed by matching individual filaments to theechelle spectra obtained at CTIO. We detect narrow H-alpha emission componentwhich we identify as the diffuse post-shock recombination radiation, anddiscrete broad emission features that correspond to the shocked gas infilaments. The overall expansion of the remnant is about 250 km/s. The denseclouds are shocked up to line-of-sight velocities of 250 km/s and the lessdense gas up to 300 km/s. A few cloudlets have even higher radial velocities,reaching up to 350 km/s. We confirm the presence of the cavity in the remnant,and identify the center of explosion. Using archival Chandra and XMM-Newtondata, we observe the same trends in surface brightness distribution for theoptical and X-ray images. We carry out the spectral analysis of three regionsthat represent the most significant optical features.

Supernova Remnants in the Large Magellanic Clouds IX: Multiwavelength Analysis of the Physical Structure of N49