Shock-cloud interaction in the southwestern limb of SN 1006, observations and models

MICELI, M.; ORLANDO, S.; ACERO, F.; DUBNER, G.; KATSUDA, S.; DECOURCHELLE, A.; BOCCHINO, F.

Dublin

Congreso; The X-ray Universe 2014; 2014

European Space Agency

The historical supernova remnant SN 1006 is a powerful source of high-energy particles showing a characteristic bilateral morphology in its nonthermal emission (from radio to TeV gamma-rays). By analyzing the observations of the XMM-Newton Large Program (LP) on SN 1006, together with archive HI observations, we found evidence that clearly indicates that an atomic cloud is interacting with the southwestern rim of the remnant, which is dominated by nonthermal synchrotron emission (Miceli et al. 2014). The southwestern limb therefore presents a unique combination of efficient particle acceleration and high target density, thus being the most promising region for gamma-ray hadronic emission in SN 1006. We further investigate the shock-cloud interaction by analyzing the Chandra LP observations of SN 1006 to obtain dedicated measurements of the proper-motion in the interaction region (Katsuda et al. 2014 in preparation). We finally perform detailed 3-D MHD simulations describing the remnant-cloud interaction and present the comparison between observables synthesized from the model and actual X-ray data. We estimate that hadronic gamma-ray emission from the southwestern limb of SN 1006 will be detectable with the Fermi telescope within a few years.