Constraining Explosion Type of Young Supernova Remnants Using 24 μm Emission Morphology
The Astrophysical Journal Letters, Volume 771, Issue 2, article id. L38, 6 pp. (2013).
Published in Jul 2013
Determination of the explosion type of supernova remnants (SNRs) can be challenging, as SNRs are hundreds to thousands of years old and supernovae are classified based on spectral properties days after explosion. Previous studies of thermal X-ray emission from Milky Way and Large Magellanic Cloud SNRs have shown that Type Ia and core-collapse (CC) SNRs have statistically different symmetries, and thus these sources can be typed based on their X-ray morphologies. In this Letter, we extend the same technique, a multipole expansion technique using power ratios, to infrared (IR) images of SNRs to test whether they can be typed using the symmetry of their warm dust emission as well. We analyzed archival Spitzer Space Telescope Multiband Imaging Photometer 24 μm observations of the previously used X-ray sample, and we find that the two classes of SNRs separate according to their IR morphologies. The Type Ia SNRs are statistically more circular and mirror symmetric than the CC SNRs, likely due to the different circumstellar environments and explosion geometries of the progenitors. Broadly, our work indicates that the IR emission retains information of the explosive origins of the SNR and offers a new method to type SNRs based on IR morphology.
Astrophysics - High Energy Astrophysical Phenomena; Astrophysics - Solar and Stellar Astrophysics; ISM: supernova remnants; infrared: ISM; methods: data analysis; techniques: image processing
ISM: supernova remnants; infrared: ISM; methods: data analysis; techniques: image processing
Astrophysics - High Energy Astrophysical Phenomena; Astrophysics - Solar and Stellar Astrophysics