[en] A spectroscopic study of N132D, a supernova remnant in the Large Magellanic Cloud (LMC), shows that it contains high-velocity filaments characterized by strong emission lines of [0 II], [0 III], and [Ne III] having a maximum range in radial velocities of 4440 km s^-1. The velocity data, combined with the revised size, suggests a maximum age of approx.3400 years, and a probable age of approx.1350 years. It is suggested as a possible source of low energy X-rays and the consequent energy input is 3 x 10⁵¹ ergs. Proper-motion studies of filaments seem feasible. N132 D may have resulted from a Type II supernova if it is physically associated with a grouping of nearby young stars in the bar of the LMC.Spectroscopy of 0525--66.0, a nonthermal radio source 7' northwest of the supernova remnant N49 in the LMC, does not reinforce the conclusion that the former was blasted out of the latter approximately 15,000 years ago. Other arguments concerning the size and shape of the interconnecting filament and the presence of other filaments lead to a similar conclusion. It may be a part of an unrelated supernova remnant.Lasker's spectroscopy and direct photography reinforced by our spectroscopy of the condensation 2' west of the supernova remnant N11 L suggest that they are unrelated. The condensation is the nucleus of an emission-line galaxy with a redshift of +7139 km s^-1