The Supernova Remnant and Superbubble Components of the N206 Complex

Details The Supernova Remnant and Superbubble Components of the N206 Complex The Supernova Remnant and Superbubble Components of the N206 Complex

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...205.7005w&link_type=abstract

American Astronomical Society Meeting 205, #70.05; Bulletin of the American Astronomical Society, Vol. 36, p.1463

Astronomy and Astrophysics

Astronomy

Scientific paper

Supernovae (SNe), through their diffuse supernova remnants (SNRs), are primarily responsible for the injection of energy and heavy elements into the interstellar medium (ISM). The consequences of these injections are far-reaching. SNe provide most of the hot gas component of the ISM, and through collective inputs to structures such as superbubbles (SBs), can transfer hot gas into a galaxy halo. The energy and heavy elements influence future generations of star formation in a galaxy and have a profound effect on galaxy evolution.
We have undertaken a large project to examine the dispersal of energy and heavy elements into a host galaxy by its population of SNRs and SBs, using the populations of therse objects in the Large and Small Magellanic Clouds (LMC, SMC). As part of this study, we have examined of the neighboring N206 SNR (SNR B 0532-71.0) and N206 superbubble (DEM L 221) at optical, X-ray and radio wavelengths.
The N206 SNR was recently found to posess an elongated, radially-oriented radio feature. Utilizing the HST, Chandra, and XMM-Newton, we have obtained optical emission-line images and spatially resolved X-ray spectral maps for this SNR. Our findings imply the SNR is in the mid to late stages of its evolution. X-ray emission associated with the radio "linear feature" strongly suggests it to be a pulsar-wind nebula (PWN). A small-diameter X-ray source is discovered at the outer tip of this feature, which, with the feature's elongated morphology, suggests a bow-shock PWN structure.
X-ray emission from the N206 superbubble had been detected with ROSAT. Using the higher sensitivity of XMM, we were able to obtain detailed spectral results for ths SB. We combine this information with ground-based optical emission-line and radio HI data to form a complete picture of this SB and its possible enhancements of X-ray emission from internal SNRs.

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