Speaker
Description
We report the discovery of an $\gamma$-ray source in the Galactic plane named LHAASO J1914+1150 with a significance of 10.3$\sigma$ at 2-20 TeV and 12.5$\sigma$ above 25TeV. The best-fit position is R.A. = $288.72^{\circ} \pm 0.3^{\circ}$ and decl. = $11.79^{\circ}\pm 0.03^{\circ}$. Due to the significant diffuse radiation in the Galactic plane, we used a dust template for evaluation. We tested two methods: one with adjustable parameters like normalization factor and spectral index, and another with these parameters fixed as in the First LHAASO catalog. The former approach fails to discern the ductility of LHAASO J1914+1150 due to the stronger diffuse radiation, whereas the latter approach yields an angular size of $0.44^{\circ} \pm 0.05^{\circ}$ (for WCDA) and $0.22^{\circ}\pm0.06^{\circ}$ (for KM2A). The source is proximal to a high-luminosity pulsar, PSR J1915+1150, with an angular separation of approximately 0.11 degrees. This indicates that the TeV emission is likely a consequence of the lepton process in the vicinity of the pulsar, potentially originating from the PWN or pulsar halo.The observations from LHAASO are consistent with the scenario wherein VHE electrons have escaped from the pulsar, diffused into the interstellar medium, and subsequently scattered the interstellar radiation field. Given the substantial distance to the pulsar, the interpretation of the TeV emission within the framework of the pulsar halo scenario necessitates a significant diffusion coefficient to account for the observed size of the LHAASO detection.
