Supernova remnant candidates in the Small Magellanic Cloud

Far‐Ultraviolet and Hα Spectroscopy of SNR 0057−7226 in the Small Magellanic Cloud HiiRegion N66

“…Einstein X-ray observations showed a bright source in N66 tentatively identified as a SNR (Inoue, Koyama, & Tanaka 1983;Wang & Wu 1992). Radio observations by Mills et al (1982) showed bright, extended, thermal emission at 408, 843, and 5000 MHz corresponding to the H ii region but no clear sign of the SNR. Optical observations also showed only the extremely bright nebular emission but no filamentary structure associated with the SNR.…”

Origins of the Molonglo Radio Observatory ? The Cross and the MOST

“…Fortunately no 'cleaning' of the maps was necessary for the early programs because the directly synthesised beam was relatively clean and publishable maps could be produced shortly after the 12 hour observations ceased. This 'raw' beam was used for much of the early work, particularly for the very successful searches for supernova remnants in the Magellanic Clouds, starting with the SMC, the first major program of the MOST (Mills et al 1982). Further developments, results and future prospects are described elsewhere (see e.g.…”

Supernovae. Part II: the aftermath

“…'Scaled from LMC value by ratio of their luminosities. Mills, Little, Durdin, and Kesteven, 1982. that a typical event expel & 1 Mo at a velocity near 10 km/s, Type II's normally involving more mass but smaller velocities than Type I s. The associated kinetic energy, -10 ' ergs, when followed via any of the standard inodels of SNR evolution (Gull, 1973;Rosenberg and Scheuer, 1973; Mansfield and Salpeter, 1974;McKee 1974;; and many recent ones discussed in NATO81), results in a remnant that should remain visible for -10 yr.…”