Ponente
Descripción
At the edge of the Galactic supernova remnant (SNR) Vela Junior lies the pulsar PSR J0855-4644. Pulsars are among the most efficient particle accelerators in our Galaxy, making the study of this region of interest. PSR J0855-4644 has remarkable X-ray and radio features, revealing a pulsar wind nebula (PWN) structure along with a bow shock nebula. PSR J0855–4644 stands out as one of the highest Ė/d$^{2}$ pulsars from which no GeV gamma-ray pulsations have been detected, despite its proximity (<900 pc), high spin-down luminosity (>10$^{36}$ erg/s), and jet-like structures. It lies in a complex environment near the SNR shock, offering a unique opportunity to study the evolution of the PWN and particle acceleration physics.
In this contribution, we present a full forward-folding analysis of data from the H.E.S.S. gamma-ray telescopes to announce the discovery of a TeV gamma-ray counterpart of the PWN of PSR J0855-4644. This is possible from the substantial on-source livetime combined with advanced 3D analysis and modeling techniques, allowing the emission in the Vela Junior region to be resolved into distinct components. For the first time, we are able to disentangle the emission from the PWN from the supernova remnant emission in part due to its significantly different gamma-ray spectrum (power law index <2) extending up to tens of TeV. We present the PWN very-high-energy spectrum and morphology and discuss the object multi-wavelength characteristics in the landscape of PWN.
