Characterizing the Sites of Hadronic Cosmic Ray Acceleration

Details Characterizing the Sites of Hadronic Cosmic Ray Acceleration Characterizing the Sites of Hadronic Cosmic Ray Acceleration

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21943905p&link_type=abstract

American Astronomical Society, AAS Meeting #219, #439.05

Astronomy and Astrophysics

Astronomy

Scientific paper

It has been argued that supernova remnant (SNRs) shocks are the acceleration sites for galactic cosmic rays. While this has been established for electrons, solid evidence for hadrons constituting the bulk of the cosmic rays have been lacking. Models of hadronic cosmic ray acceleration in SNRs predict a gamma-ray flux density depending on parameters like the environment density and distance. Few reliable estimates of those parameters exist. SNRs with cosmic rays interacting with molecular clouds are expected to be bright gamma-ray sources, and these sites can be traced using 1720 MHz OH masers. The masers give information about the density and kinematical distance estimates. Only 10% of galactic SNRs harbor OH masers, and we have therefore searched for a more frequently occurring SNR/cloud interaction tracer. We have detected 36 GHz and 44 GHz methanol masers associated with a few SNRs. Here we report on the result of a search for methanol masers in 21 SNRs, and in particular the details of our detections in Sgr A East. Combining observations and modeling of methanol masers in SNRs, we aim to better constrain the density and distance to SNRs with TeV emission. The goal is to test the hadronic cosmic ray models and to understand the mechanisms of particle acceleration in SNRs.
This project is supported under NASA-Fermi grant NNX10A055G.

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