Speaker
Peter Eger
(MPIK Heidelberg)
Description
The shell-type supernova remnant (SNR) RX J1713.7-3946 is one of the brightest TeV gamma-ray sources in the Galaxy detected by the High Energy Stereoscopic System (H.E.S.S.). Despite extensive multi-wavelength coverage in gamma-rays, X-rays and lower energy regimes, the nature of the underlying gamma-ray radiation mechanisms is still under debate.
Here, we present new precision measurements, based on 150 hours of observations performed with the H.E.S.S. array in its 4-telescope configuration, and make use of new superior analysis techniques. The new results feature an improvement in the exposure by factors of 2 (sky images) to 4 (spectra) over previous measurements. These data allow for spectral and morphological studies at unprecedented precision, yielding the most detailed TeV gamma-ray analysis of any extended object in the sky. The angular resolution of better than 0.05 deg allows us to perform for the first time a detailed investigation of morphological differences between TeV gamma rays and X-rays.
| Registration number following "ICRC2015-I/" | 527 |
|---|---|
| Collaboration | H.E.S.S. |
Author
Peter Eger
(MPIK Heidelberg)
Co-authors
David Berge
(NIKHEF (NL))
Prof.
Felix Aharonian
(MPIK Heidelberg, DIAS)
Mr
Mark Bryan
(GRAPPA, Univ. of Amsterdam)
Dr
R. D. Parsons
(MPIK Heidelberg)
Stefan Funk
(Stanford University and SLAC)
Victor Zabalza
(University of Leicester)
Dr
Yasunobu Uchiyama
(Rikkyo University)
