Speaker
Description
RX J1713.7−3946 is the poster-child cosmic-ray accelerator and is among the brightest X- and gamma-ray non-thermal emitters. Both the X-rays and the gamma-rays reveal a shell morphology that is brighter in the western half of the remnant where the shock is partly in interaction with dense clumps traced by $^{12}$CO radio observations.
Thanks to its high surface brightness and large angular size, it is one of the few targets where GeV and TeV spatially resolved spectroscopy is possible. Here we report on a new Fermi-LAT analysis from 200 MeV to 2 TeV with 7.5 years of data that benefits from the improved Pass8 LAT performances.
We will focus on the results from the spectroscopic analysis, revealing a spectral difference (at ∼4sigma) between the Eastern region (low density medium) and the Western region where the clumps are observed. The hard spectral slope in the East can be explained by Inverse Compton emission while for the softer Western region an additional component, on top of the Inverse Compton one derived from the Eastern half, is needed. This second component could be ascribed to the hadronic emission from the regions of interaction.
