Michael Rutkowski

“A Look at the Supernova Remnant 1E0102.2-7219 with the Chandra X-Ray Observatory”

We present 230ks of Chandra X-ray Observatory ACIS observations of the supernova remnant 1E 0102.2-7219 in the Small Magellanic Cloud with an unprecedented signal-to-noise ratio for this remnant. No compact object was found. We present an upper limit on the X-ray (0.1-10 keV) luminosity (3æ) for regions that comprises the majority of the interior, to the ejecta shell, between 0.2-1.0 times greater than a Cas A-like Neutron Star, assuming a power law or blackbody spectrum, respectively. However, there is a small central region of primarily thermal emission for which we determined an upper limit on the X-ray luminosity to be more than six times brighter than a Cas A-like Neutron Star. This region is centered at RA
01h04m02s :015,DEC -72±01'55".82 (J2000). We investigated the morphology of the X-ray shell, found an extensive ionization proØle with evidence of complex Ølmentary structure and little structural variation in the emission of the ionized elements of Hydrogen-like and Helium-Like Neon, Oxygen, and Magnesium. Furthermore, by measuring the shift in the shell peak emission over a time baseline º 4:5 years, we determined an average kinematic expansion
rate for the remnant, as a function of the angular position about a geometric center of the remnant. We derived an average expansion age for the remnant which varies signiØcantly as a function of azimuthal direction.