AAS 200th meeting, Albuquerque, NM, June 2002
Session 15. SNRs and PNe
Display, Monday, June 3, 2002, 9:20am-6:30pm, SW Exhibit Hall

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[15.06] Chandra Observation of SNR N49B in the Large Magellanic Cloud

S. Park, D. N. Burrows, G. P. Garmire, J. A. Nousek (Pennsylvania State University), J. P. Hughes (Rutgers University), P. O. Slane (CfA)

The supernova remnant (SNR) N49B in the Large Magellanic Cloud has been observed with the Advanced CCD Imaging Spectrometer (ACIS) on board Chandra X-Ray Observatory. The superb angular resolution of the Chandra/ACIS resolves complex filaments and knots across the SNR. These bright features are soft (typically E < 2 keV) and no obvious hard continuum is evident.

We present the equivalent width (EW) images for the atomic species O, Ne, and Mg. The EW images indicate the presence of Mg-rich ejecta material around the central regions of the SNR. This result implies the metal-rich ejecta are still important in N49B although the derived Sedov age is relatively old. The low EWs for the circumferential shell-like filaments suggest that these bright features are emission from the shocked circumstellar medium rather than from metal-rich ejecta. Spatially-resolved spectra extracted from various regions over the SNR confirm the abundance distribution as implied by the EW maps. The regional spectra imply significant variations in the fitted absorbing column, plasma temperature, and the ionization state across the SNR. These results indicate that N49B is interacting with spatially associated dense molecular clouds.

The author(s) of this abstract have provided an email address for comments about the abstract: park@astro.psu.edu

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Bulletin of the American Astronomical Society, 34
© 2002. The American Astronomical Soceity.