Simulated AXAF HETG observation of the supernova remnant E0102-72 in the Small Magellanic Cloud (distance = 59.9 kpc). A Lucy deconvolved Rosat HRI image was used as the basis of the MARX simulation. In the original image, the edges of the ring are unresolved and, while the deconvolution process probably brings us closer to the reality, the image that AXAF produces may show much more small scale structure (< 5 arcsec). The input spectrum was modeled as single component, non-equilibrium ionization model loosely based on ASCA observations by Hayashi et al. 1994 PASJ, 46, L121.
Figure 1. - This image shows the complete spectrum of the SNR as it would be observed with the ACIS-S imaging array. The fainter replicated images of the remnant correspond to higher orders of bright emission lines in the spectrum. Click on the image to see a larger version.
Figure 2. - This image shows an expanded view of the 0th order of the spectrum. AXAF's superior spatial resolution will actually be capable of resolving finer structure in the remnant than this image depicts.
Simulation courtesy of John Houck (MIT/ASC)
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