Compact OH(1720 MHz) masers have proven to be excellent signposts for the interaction of supernova remnants with adjacent molecular clouds. Less appreciated has been the weak, extended OH(1720 MHz) emission which accompanies strong compact maser sources. Recent single-dish and interferometric observations reveal the majority of maser-emitting supernova remnants(SNRs) have accompanying regions of extended maser emission. Enhanced OH abundance created by the passing shock is observed both as maser emission and absorption against the strong background of the remnant. Modeling the observed OH profiles gives an estimate of the physical conditions in which weak, extended maser emission arises. I will discuss how we can realize the utility of this extended maser emission, particularly the potential to measure the strength of the post-shock magnetic field via Zeeman splitting over these large-scales.
|Number of pages||5|
|Journal||Proceedings of the International Astronomical Union|
|Publication status||Published - Mar 2007|
|Event||IAU Symposium 242: Astrophysical masers and their environments - Alice Springs, Australia|
Duration: 12 Mar 2007 → 16 Mar 2007
- ISM: magnetic fields
- Supernova remnants