Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...20915611k&link_type=abstract
2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #156.11; Bulletin of the American Astronomical Society,
Astronomy and Astrophysics
Astronomy
1
Scientific paper
The Large Magellanic Cloud (LMC), with its low foreground absorption and proximity, offers the ideal site to study a large sample of supernova remnants (SNRs) in detail, both spatially and energetically. It is possible to obtain a relatively complete sample of SNRs in the LMC to examine both global properties and the subclasses of SNRs. Toward this goal, we have identified new SNRs using multi-wavelength data. The newly recognized SNRs are generally fainter than the known sample, and may represent a previously missed population.
We have obtained X-ray images and spectra of three of these recently identified SNRs using the XMM observatory. These data, in conjunction with pre-existing optical emission-line images and spectra and radio continuum data, are used to determine the physical conditions of the warm ionized gas and the hot ionized gas. We compare the morphologies of the SNRs in the different waveband. The physical properties of the warm ionized shell are determined from the Hα surface brightness and the SNR expansion velocity. The X-ray spectra were fit with a Raymond-Smith thermal plasma model and the physical conditions of the hot gas are derived from the model fits. We find that the pressure of the hot gas is greater than that in the warm shell by about an order of magnitude, implying that these remnants are in the pressure-driven expansion stage. We also discuss the ages and classifications of the remnants.
This work was supported by the National Science Foundation under grant 0353843.
Klimek Matthew
Points Sean D.
Smith Christopher
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