Resumen
This work presents a study of two supernova remnants belonging to the Large Magellanic Cloud, N49 and N11L, based on the spectroscopic mapping of their physical properties. Long slit spectroscopy was used to collect data from a grid of different positions covering the whole nebula by positioning the slit on different and equally spaced declinations. The data were obtained with the 4.1 m SOAR telescope (Southern Astrophysical Research Telescope), in Chile. The spectral coverage was about 3500-8000 Å. For each object, about 50 emission lines were measured on the spectra, allowing to build maps of many interesting line intensity ratios. The maps of electron density and temperature were obtained using the [S II] λ 6717/λ 6731 and [O III] (λ 5007+λ 4959)/λ 4363 line ratio sensors, respectively. N49 presents a strong density gradient with the density varying from 600 cm^{-3} at the North-West to more than 3000 cm^{-3} at the South-East. The electron temperature distribution shows a rough spherical symmetry with the higher values found at the centre. In N11L the electron density varies from less than 100 cm^{-3} to about 400 cm^{-3}, with the higher values found on the bright filaments. These maps were used to build a picture of the structure of these two supernova remnants.
