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