Ultra-high-energy ${\hat{I}}^3$-ray emission associated with the tail of a bow-shock pulsar wind nebula

Abstract

In this study, we present a comprehensive analysis of an unidentified point-like ultra-high-energy (UHE) ${\hat{I}}^3$-ray source, designated as 1LHAASO J1740+0948u, situated in the vicinity of the middle-aged pulsar PSR J1740+1000. The detection significance reached 17.1$\ddot{I}ƒ$ (9.4$\ddot{I}ƒ$) above 25TeV (100TeV). The source energy spectrum extended up to 300TeV, which was well fitted by a log-parabola function with $N0=(1.93\pm 0.23)\times 10^{-16}\mathrm{Te}{\mathrm{V}}^{-1}\mathrm{c}{\mathrm{m}}^{-2}{\mathrm{s}}^{-2}$, $\hat{I}\pm =2.14\pm 0.27$, and ${\hat{I}}^2=1.20\pm 0.41$ at E0 = 30TeV. The associated pulsar, PSR J1740+1000, resides at a high galactic latitude and powers a bow-shock pulsar wind nebula (BSPWN) with an extended X-ray tail. The best-fit position of the gamma-ray source appeared to be shifted by $0.2^{\circ }$ with respect to the pulsar position. As the (i) currently identified pulsar halos do not demonstrate such offsets, and (ii) centroid of the gamma-ray emission is approximately located at the extension of the X-ray tail, we speculate that the UHE ${\hat{I}}^3$-ray emission may originate from re-accelerated electron/positron pairs that are advected away in the bow-shock tail.

Corrected spelling errors in several author names