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Gamma rays from HESS J1849$-$000, a middle-aged TeV pulsar wind nebula (PWN),are observed by the Tibet air shower array and the muon detector array. Thedetection significance of gamma rays reaches $4.0\, \sigma$ and $4.4\, \sigma$levels above 25 TeV and 100 TeV, respectively, in units of Gaussian standarddeviation $\sigma$. The energy spectrum measured between $40\, {\rm TeV} < E <320\, {\rm TeV}$ for the first time is described with a simple power-lawfunction of ${\rm d}N/{\rm d}E = (2.86 \pm 1.44) \times 10^{-16}(E/40\, {\rmTeV})^{-2.24 \pm 0.41}\, {\rm TeV}^{-1}\, {\rm cm}^{-2}\, {\rm s}^{-1}$. Thegamma-ray energy spectrum from the sub-TeV ($E < 1\, {\rm TeV}$) to sub-PeV($100\, {\rm TeV} < E < 1\, {\rm PeV}$) ranges including the results ofprevious studies can be modeled with the leptonic scenario, inverse Comptonscattering by high-energy electrons accelerated by the PWN of PSR J1849$-$0001.On the other hand, the gamma-ray energy spectrum can also be modeled with thehadronic scenario in which gamma rays are generated from the decay of neutralpions produced by collisions between accelerated cosmic-ray protons and theambient molecular cloud found in the gamma-ray emitting region. The cutoffenergy of cosmic-ray protons $E_{\rm p\, cut}$, cut is estimated at ${\rmlog}_{10}(E_{\rm p,\, cut}/{\rm TeV}) = 3.73^{+2.98}_{-0.66}$, suggesting thatprotons are accelerated up to the PeV energy range. Our study thus proposesthat HESS J1849$-$000 should be further investigated as a new candidate for aGalactic PeV cosmic-ray accelerator, PeVatron.

Observation of gamma rays up to 320 TeV from the middle-aged TeV pulsar wind nebula HESS J1849$-$000