Ponente
Descripción
Pulsar wind nebulae (PWNe) are bubbles of relativistic particle outflows, primarily composed of electrons and positrons, which are continuously injected from pulsars and often exhibit broadband non-thermal radiation originating from synchrotron and inverse Compton scattering emission. Recently, LHAASO and HAWC observations have detected Ultra-High-Energy (UHE, E>100 TeV) gamma-ray sources associated with PWNe, making them the prime candidates for Galactic leptonic “PeVatrons”, sources capable of accelerating leptons to PeV energies inside our Galaxy.
X-ray synchrotron radiation from TeV-PeV electrons plays a crucial role in constraining the maximum particle energies and new X-ray studies of TeV PWNe suggest that some of them can accelerate particles up to PeV energies. As such, multi-wavelength observations and broadband spectral energy distributions (SED) modelling of PWNe are the key tools for both localizing and probing the properties of the relativistic particle populations.
We present a new study of the second brightest TeV source in the Galactic Center region: the PWN powered by the energetic pulsar PSR J1747−2809 and located inside the composite-type supernova remnant G0.9+0.1. The characteristics observed from X-ray to TeV gamma-rays, including a nearby UHE source observed by HAWC, indicate that G0.9+0.1 is a PeVatron candidate. For the first time NuSTAR has detected hard X-ray emission up to 30 keV, revealing the synchrotron burn-off signature of the relativistic electrons. New insights on the source are provided through multiwavelength SED modeling incorporating radio to TeV data. Preliminary results suggest that the PWN in G0.9-0.1 has not yet interacted with the reverse SNR shock, offering a valuable case study for future observatories such as CTAO, AXIS, and NewAthena.
