Supernova Remnants in the N19 Complex of the Small Magellanic Cloud

Details Supernova Remnants in the N19 Complex of the Small Magellanic Cloud Supernova Remnants in the N19 Complex of the Small Magellanic Cloud

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aas...20713212w&link_type=abstract

American Astronomical Society Meeting 207, #132.12; Bulletin of the American Astronomical Society, Vol. 37, p.1381

Astronomy and Astrophysics

Astronomy

Scientific paper

We have analyzed Chandra data for supernova remnants (SNRs) within the N19 H II complex in the Small Magellanic Cloud, supplemented by optical emission-line images and echelle spectroscopy. Our observations include the known SNR MCRX J0047.2-7308 (SNR B0045-73.4), confirm the SNR candidate MCRX J0046.6-7308 (SNR B0045-7325), and strengthen the case for a large, extended SNR identified as candidate MCRX J0047.5-7308.
We find that the abundances inferred from spectral model fits to the X-ray emission from these SNRs and SNR candidates are consistent in each case with remnants of massive-star progenitors. We observe a possible point source within J0047.2-7308, embedded in a region of hard emission, suggestive of a possible embedded PWN. As these three remnants, all with massive-star origins, appear to be spatially located within the N19 H II complex, we infer that a small OB association may be the source of these phenomena. To expand on this assessment, we estimate the number of massive stars within N19 and project their energy input to the region. We find that a stellar-wind created superbubble is unlikely to have formed, but that the further expansion of the SNRs in the region may lead to superbubble formation on a timescale of < 0.3 Myr from the first supernova.
RMW gratefully acknowledges support from SAO grant G03-4094A, and NASA grant NNG05GC97G issued through the LTSA Program.

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