Very-high-energy Gamma-ray Observations Of Synchrotron-dominated Supernova Remnants With H.E.S.S.

Details Very-high-energy Gamma-ray Observations Of Synchrotron-dominated Supernova Remnants With H.E.S.S. Very-high-energy Gamma-ray Observations Of Synchrotron-dominated Supernova Remnants With H.E.S.S.

Sep 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011head...12.4506c&link_type=abstract

American Astronomical Society, HEAD meeting #12, #45.06

Astronomy and Astrophysics

Astronomy

Scientific paper

Supernova remnants (SNRs) are expected to produce very-high-energy (VHE; E > 100 GeV) gamma rays through interactions of high-energy particles with the surrounding medium and photon fields. VHE gamma-ray emission has indeed been discovered, by ground-based imaging atmospheric Cherenkov telescopes such as the H.E.S.S. telescope array, from a number of SNRs, establishing them as a prominent source class in the VHE domain. Of particular interest are the handful of SNRs whose X-ray spectra are dominated by non-thermal synchrotron emission; of these, the H.E.S.S. array has detected VHE gamma-ray emission from RX J1713.7-3946, RX J0852.0-4622 (Vela Jr.), RCW 86, SN 1006 and HESS J1731-347. The shell-type SNRs G1.9+0.3 and G330.2+1.0 also belong to this subclass and are further notable for their young ages (< 1 kyr), especially G1.9+0.3, which was recently determined to be the youngest SNR in the Galaxy ( 100 yr). These unique characteristics motivated investigations with H.E.S.S. to search for VHE gamma rays. The results of the H.E.S.S. observations and analyses will be presented, along with implications for potential particle acceleration scenarios, and discussed in comparison with the previously detected VHE gamma-ray shells.

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