H.E.S.S. detection of the PSR J0855−4644 nebula

is a TeV source located in the Galactic plane. The region consists of a supernova remnant (SNR, with a shell-like morphology, commonly referred to as Vela Junior, and a pulsar named Pulsars are among the most efficient leptonic accelerators in our Galaxy, making this region particularly interesting to study. We utilise the most recent data taken by the High Energy Stereoscopic System ( to investigate any emission associated with the pulsar in this region We applied a full forward-folding method on the data. Utilising 3D modelling techniques, we evaluated the TeV emission towards the various components of this complex system. The distinct energy-dependent morphology observed in our data motivates further investigation of this source. We resolved the emission in the Vela Junior region into various components, several of which correspond to the SNR itself. In particular, we find a new extended component coincident with the position of The spectrum follows a power-law distribution with a best-fit index of Γ_E = 1.81 , which differs from the properties of the surrounding stat emission of the Vela Junior SNR. A one-zone leptonic joint fit between the X-rays (from XMM-Newton) and (from leads to a lower limit on the magnetic field of 1.6μG and a spectral index of α=1.88 in line with expectations of pulsar wind nebulae (PWNe). In this paper, we report the first detection of the PWN of at TeV energies with the experiment, at a significance of 12.2σ. This is attributed to the advanced techniques of the 3D analysis. Based on the pulsar’s characteristics, its PWN is consistent with the known TeV PWNe population in the Galaxy.