VLBI observations of supernova remnants in Messier 82

We have used the European VLBI Network(EVN) at 18cm to study ve of the more compact radio sources in the starburst galaxy M82. The angular resolution of the observations is 15 mas, corresponding to 0.2 pc at the distance of M82. The observations reveal shells ranging in diameter from 40 mas to 90 mas (0.6 to 1.4 pc) although the strongest source (41.95+575) is only marginally resolved by these measurements (20 10 mas). We have found clear evidence for expansion in one of the shell sources (43.31+592) by re-analysing, in wide-eld mode, EVN data observed in 1986. Between 1986 and 1997 this source has increased its diameter by 13:6 2 mas corresponding to an average expansion velocity of 9850 1500 km s ?1. If we assume the remnant is in free expansion, this is consistent with a supernova event in the early 1960s. Hence this remnant is almost certainly younger than the strongest, most compact source (41.95+575) which was known to be present in the 1960s. 41.95+575 shows no clear evidence for expansion (<4000 km s ?1), consistent with a greater age; this is further evidence of its anomalous status. Comparison of the EVN images with earlier MERLIN data is also consistent with expansion in at least two other of the sources. We discuss the ux density variability of the compact sources in M82 and conclude that, with the exception of 41.95+575 and two transient sources, there is little evidence for signiicant changes in ux density of most of the remnants since the early 1980s.