The Impact of a Supernova Remnant on a Molecular Cloud

The SOFIA data of IC 443 can be found in the IRSA SOFIA Archive , and consist of:

• GREAT observations towards clump C and G, indicated in the figure, provide velocity resolved CO(11-10), CO(13-12) and CO(16-15) lines which are well suited to study the warm molecular gas of a shock (Project ID: 01_0156 ). There is also complementary CO data up to CO(7-6) from Herschel and ground-based observations.
• GREAT also did a deep integration (noise rms = 0.031 K) to detect line emission from iron hydride (FeH) towards clump G (Project ID: 02_0076 ). As a supernova can provide a high Fe abundance when interacting with the molecular cloud, the non-detection can be an interesting constraint on the shock models and formation of this hydride. The formation of this hydride is still unknown while it is found in stellar atmospheres, and used to study the physical conditions of these atmospheres.
• The H2 S(5) pure rotational line was observed and spectrally resolved with the EXES towards the clumps B1, B2, C and G and is a good tracer of the shocks in the region (Project ID: 75_0018 ; Reach et al. 2019).