Iron and dust in the supernova remnant IC443
Abstract
We observed the supernova remnant IC 443 with the IRSF 1.4-m telescope, using the narrow-band filters tuned for the [Fe II] 1.257, 1.644 µ m, Paβ , and H2 1-0 S(1) lines. Comparing these results with the intensities of thermal emission from the warm dust associated with IC 443, derived by AKARI and Spitzer images, we find that the [Fe II] emission is enhanced relative to the dust emission in the central region of IC 443. The Paβ emission is also detected in the regions where the [Fe II] emission is bright. In contrast, the H2 emission is limb-brightened in the southern ridge. We also derived the highly-ionized Fe line intensity map from the data obtained by Suzaku. From these results, we have investigated the origin of the [Fe II] emission, which is difficult to be explained simply by considering the lifetime of 0.1-µ m silicate dust grains against sputtering destruction and the time for Fe to reach an ionization equilibrium in the hot plasma of IC 443.
- Publication:
-
Proceedings of The Life Cycle of Dust in the Universe: Observations
- Pub Date:
- 2013
- DOI:
- 10.22323/1.207.0086
- Bibcode:
- 2013lcdu.confE..86K