Center for Astrophysics Research and Technologies Seminar Series
Methanol Masers Near Supernova Remnants
Presented by Bridget McEwen (UNM)
I will present ongoing work, which involves investigating shocked supernova remnant/molecular cloud interaction environments using both models and observations of masers and other molecules such as ammonia. One major motivation for this project is to understand cosmic ray particle acceleration in SNRs, a mechanism that depends strongly on the density of the acceleration region. This parameter can be determined by using density tracers such as class I methanol maser transition lines, which are thought to arise at the shock front where particle acceleration is thought to occur in SNRs. Recent observations have found class I methanol maser lines, specifically the 44 and 36 GHz lines, associated with shocked regions in SNRs. However, if these transitions can be used as density tracers, we need a better understanding how they arise, specific to the conditions present in SNRs, and how to locate them. I will show modeling results demonstrating how the relative line strengths at 36 and 44 GHz can be used to constrain the density parameter. I will discuss a possible method of locating methanol masers using GBT ammonia observations. Additionally, I will discuss observations of methanol masers in a survey of SNRs, and what can be learned about the relationship between methanol masers and SNR/MC interaction regions applying the modeling that has been completed.
2:00 pm, Thursday, August 21, 2014
PAIS-2540, PAIS
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