LMC N132D

LMC N132D is a prominent supernova remnant located in the Large Magellanic Cloud, a satellite galaxy of the Milky Way Galaxy, in the constellation of Dorado. It lies approximately 170,000 light-years away. It is one of the brightest and most studied oxygen-rich SNRs in the LMC, known for its complex morphology and high-energy emissions across multiple wavelengths.

Observation

LMC N132D is a very high-energy gamma-ray source, detected by the High Energy Stereoscopic System with an angular resolution of ~0.05 degrees. Its power-law spectrum extends beyond 8 TeV without a cutoff, unusual for a remnant of its age, making it a key target for studying particle acceleration in mature SNRs. It is located near the center of the galaxy, 1.5 degrees west of the Tarantula Nebula. The nebula emits X-rays, and its material travels at a speed of 2000 km/s.

Significance

LMC N132D offers critical insights into core-collapse supernovae, shock interactions with the interstellar medium, and non-thermal processes in SNRs. Its oxygen-rich ejecta and association with molecular clouds provide clues about the progenitor star's environment and evolution. The remnant's gamma-ray emission challenges models of particle acceleration, as its mature age contrasts with its high-energy output.