AAS 199th meeting, Washington, DC, January 2002
Session 126. Supernova Remnants
Display, Thursday, January 10, 2002, 9:20am-4:00pm, Monroe/Lincoln

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[126.09] Chandra Observation of the Galactic Oxygen-Rich Supernova Remnant G292.0+1.8

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

We present results from the observation of the young Galactic supernova remnant (SNR) G292.0+1.8 with the Chandra/ACIS. In the 0.3 - 8 keV energy band, the high resolution ACIS images reveal a complex morphology consisting of the knots and filaments, as well as the limb-brightened blast wave around the periphery of the SNR. Imaging in the soft (0.3-2 keV) and hard (>2 keV) X-ray bands shows the presence of a hard point-like source surrounded by a diffuse nebula that are believed to be a pulsar and its wind nebula. We present the equivalent width (EW) maps for the elemental species O, Ne, Mg, Si, S, and Ar that have allowed us to identify regions of enhanced metallicity in the SNR. We find that the ejecta knots in G292.0+1.8 are typically bright in O, Ne, and Mg lines, and weaker Si, S, and Ar, with little Fe. Spectra from small regions indicate that emission from metal-rich ejecta can be distinguished from that of shocked ISM: e.g., the brightest emission near the center of the SNR shows solar to sub-solar abundances, indicating a shocked ISM origin while some others fitted with high metal abundances implying emission from the ejecta. Generally, ejecta temperature (kT ~ 1 keV) is higher than shocked ISM (kT ~ 0.6 keV), in agreement with the model with an SN explosion in the presence of dense circumstellar material.

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

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