Molecular Environment of the Thermal Composite Supernova Remnant G352.7-0.1

Abstract

Galactic supernova remnants (SNRs) play an important role in our understanding of supernovae and their feedback on the interstellar environment. SNR G352.7-0.1 is special for its thermal composite morphology and double-ring structure. We have performed spectroscopic mapping of the ^12 CO and ^13 CO J = 2–1 lines toward G352.7-0.1 with the Atacama Pathfinder Experiment telescope. Broad ^12 CO lines are found in the northeastern ring at a local-standard-of-rest velocity range of ∼−50 to −30 km s ^−1 , suggesting that the remnant is interacting with molecular clouds at ∼−51 km s ^−1 . Thus, we adopt a distance of ∼10.5 kpc for this SNR. The momentum and kinetic energy of the shocked gas along the line of sight are estimated to be ∼10 ^2 M _☉ km s ^−1 and ∼10 ^46 erg, respectively. We also find an expanding structure around the remnant, which is possibly related to the wind-blown bubble of the progenitor star. From Fermi-LAT data in the energy range 0.1–500 GeV, we find no gamma-ray counterparts to G352.7-0.1.

Keywords

• Interstellar medium
• Supernova remnants
• Molecular clouds
• Shocks