Ponente
Descripción
The study of UHE $\gamma$-ray emission plays a key role in identifying the astrophysical accelerators responsible for producing $\sim$ PeV particles and shaping the Galactic cosmic-ray population. SNR G69.7+1.0 has recently attracted attention due to its association with the LHAASO source 1LHAASO J2002+3244, which emits above 100 TeV. This spatial coincidence provides a unique opportunity to investigate particle acceleration in supernova remnants (SNRs). While young SNRs are efficient cosmic ray accelerators, direct evidence for their role as PeVatrons remains unclear. We present preliminary results from the first NuSTAR observation of SNR G69.7+1.0, aimed at characterizing its hard X-ray emission, constraining its spectral properties, and probing the maximum energies of accelerated particles. These results are complemented by multi-wavelength data to assess the physical conditions under which SNRs may become PeVatrons.
