PoS - Proceedings of Science
Volume 444 - 38th International Cosmic Ray Conference (ICRC2023) - Gamma-ray Astronomy (GA)
Possible VHE gamma emission from PWN tail of PSR J1740+1000
R. Xu
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Pre-published on: July 25, 2023
Published on:
Abstract
In this report, we present an analysis of a gamma source with very high energy (VHE) in close proximity to the PSR J1740+1000. Our observations, carried out using the LHAASO-KM2A instrument, yielded a remarkably high significance level exceeding 12$\sigma$ (5.4$\sigma$) above 25 TeV (100 TeV). The precise fitting position was determined as $\rm{RA}= 265.01\pm0.03^{\circ},\rm{Dec}=9.79\pm0.04^{\circ}$, exhibiting an offset of approximately $0.22^{\circ}$ from the pulsar's location and aligning almost perfectly with the trace of its proper motion.In power-law shape,$\alpha$ and $N_0$ are $3.15\pm0.17$ and $0.37\pm0.04\times10^{-16}\rm TeV^{-1},cm^{-2},s^{-1}$ at $50\,TeV$,respectively.

The pulsar most associated with our observations is PSR J1740+1000, which is a middle-aged pulsar exhibiting a prominent X-ray tail. This pulsar is located at the high galactic latitude and it is considered a important potential pulsar halo candidate by the HAWC Collaboration. Nevertheless, our analysis did not reveal any significant extension. Considering the positional coincidence, we favor the hypothesis that the origin of the gamma emission lies within the pulsar wind nebula (PWN) tail. However, it is crucial to note that alternative explanations, such as a distant off-beam pulsar, contributing to the halo, cannot be conclusively ruled out totally.
DOI: https://doi.org/10.22323/1.444.0607
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