Fifteen Years of High-Resolution Radio Imaging of Supernova 1987A

Abstract

Supernova 1987A in the Large Magellanic Cloud provides a spectacularly detailed view of the aftermath of a core‐collapse explosion. The supernova ejecta initially coasted outward at more than 10% of the speed of light, but in 1990 were observed to decelerate rapidly as they began to encounter dense circumstellar material expelled by the progenitor star The resulting shock has subsequently produced steadily brightening radio synchrotron emission, which is resolved by the Australia Telescope Compact Array (ATCA) into an expanding limb‐brightened shell. Here we present 15 years of ATCA imaging of Supernova 1987A, at an effective angular resolution of 0.”4. We find that the radio remnant has accelerated in its expansion over this period, from ≈ 3600 km s−1 in 1992 to ≈ 5200 km s−1 at the end of 2006. The published diameters of the evolving X‐ray shell have been ∼ 15% smaller than the corresponding radio values, but a simultaneous Fourier analysis of both radio and X‐ray data eliminates this discrepancy, and yields a current diameter for the shell in both wave‐bands of ≈ 1.”7. An asymmetric brightness distribution is seen in radio images at all ATCA epochs: the eastern and western rims have higher fluxes than the northern and southern regions, indicating that most of the radio emission comes from the equatorial plane of the system, where the progenitor star's circumstellar wind is thought to be densest. The eastern lobe is brighter than and further from the supernova site than the western lobe, suggesting an additional asymmetry in the initial distribution of supernova ejecta.