Kavli Affiliate: Eric Miller
| First 5 Authors: Xi Long, Xi Long, , ,
| Summary:
We present results from the Chandra X-ray Observatory Large Project (878 ks
in 28 observations) of the Large Magellanic Cloud supernova remnant N132D. We
measure the expansion of the forward shock in the bright southern rim to be
$0.!^primeprime10 pm 0.!^primeprime02$ over the $sim14.5$ yr
baseline, which corresponds to a velocity of $1620pm400~mathrmkm,s^-1$
after accounting for several instrumental effects. We measure an expansion of
$0.!^primeprime23 pm 0.!^primeprime02$ and a shock velocity of
$3840pm260~mathrmkm,s^-1$ for two features in an apparent blowout region
in the northeast. The emission-measure-weighted average temperature inferred
from X-ray spectral fits to regions in the southern rim is $0.95pm0.17$ keV,
consistent with the electron temperature implied by the shock velocity after
accounting for Coulomb equilibration and adiabatic expansion. In contrast, the
emission-measure-weighted average temperature for the northeast region is
$0.77pm0.04$ keV, which is significantly lower than the value inferred from
the shock velocity. We fit 1-D evolutionary models for the shock in the
southern rim and northeast region, using the measured radius and propagation
velocity into a constant density and power-law profile circumstellar medium. We
find good agreement with the age of $sim2500$ years derived from optical
expansion measurements for explosion energies of $1.5-3.0 times
10^51,mathrmerg$, ejecta masses of $2-6 ,mathrmM_odot$ and ambient
medium densities of $sim0.33-0.66$ $mathrmamu~cm^-3$ in the south and
$sim0.01-0.02$ $mathrmamu~cm^-3$ in the northeast assuming a constant
density medium. These results are consistent with previous studies that
suggested the progenitor of N132D was an energetic supernova that exploded into
a pre-existing cavity.
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