학술논문
Observation of gamma rays up to 320 TeV from the middle-aged TeV pulsar wind nebula HESS J1849$-$000
Document Type
Working Paper
Author
Amenomori, M.; Asano, S.; Bao, Y. W.; Bi, X. J.; Chen, D.; Chen, T. L.; Chen, W. Y.; Chen, Xu; Chen, Y.; Cirennima; Cui, S. W.; Danzengluobu; Ding, L. K.; Fang, J. H.; Fang, K.; Feng, C. F.; Feng, Zhaoyang; Feng, Z. Y.; Gao, Qi; Gomi, A.; Gou, Q. B.; Guo, Y. Q.; Guo, Y. Y.; Hayashi, Y.; He, H. H.; He, Z. T.; Hibino, K.; Hotta, N.; Hu, Haibing; Hu, H. B.; Hu, K. Y.; Huang, J.; Jia, H. Y.; Jiang, L.; Jiang, P.; Jin, H. B.; Kasahara, K.; Katayose, Y.; Kato, C.; Kato, S.; Kawahara, I.; Kawashima, T.; Kawata, K.; Kozai, M.; Kurashige, D.; Labaciren; Le, G. M.; Li, A. F.; Li, H. J.; Li, W. J.; Li, Y.; Lin, Y. H.; Liu, B.; Liu, C.; Liu, J. S.; Liu, L. Y.; Liu, M. Y.; Liu, W.; Lu, H.; Meng, X. R.; Meng, Y.; Munakata, K.; Nagaya, K.; Nakamura, Y.; Nakazawa, Y.; Nanjo, H.; Ning, C. C.; Nishizawa, M.; Noguchi, R.; Ohnishi, M.; Okukawa, S.; Ozawa, S.; Qian, X.; Qian, X. L.; Qu, X. B.; Saito, T.; Sakakibara, Y.; Sakata, M.; Sako, T.; Sako, T. K.; Sasaki, T.; Shao, J.; Shibata, M.; Shiomi, A.; Sugimoto, H.; Takano, W.; Takita, M.; Tan, Y. H.; Tateyama, N.; Torii, S.; Tsuchiya, H.; Udo, S.; Wang, H.; Wang, S. F.; Wang, Y. P.; Wangdui; Wu, H. R.; Wu, Q.; Xu, J. L.; Xue, L.; Yang, Z.; Yao, Y. Q.; Yin, J.; Yokoe, Y.; Yu, Y. L.; Yuan, A. F.; Zhai, L. M.; Zhang, H. M.; Zhang, J. L.; Zhang, X.; Zhang, X. Y.; Zhang, Y.; Zhang, Yi; Zhang, Ying; Zhao, S. P.; Zhaxisangzhu; Zhou, X. X.; Zou, Y. H.
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Abstract
Gamma rays from HESS J1849$-$000, a middle-aged TeV pulsar wind nebula (PWN), are observed by the Tibet air shower array and the muon detector array. The detection significance of gamma rays reaches $4.0\, \sigma$ and $4.4\, \sigma$ levels above 25 TeV and 100 TeV, respectively, in units of Gaussian standard deviation $\sigma$. The energy spectrum measured between $40\, {\rm TeV} < E < 320\, {\rm TeV}$ for the first time is described with a simple power-law function of ${\rm d}N/{\rm d}E = (2.86 \pm 1.44) \times 10^{-16}(E/40\, {\rm TeV})^{-2.24 \pm 0.41}\, {\rm TeV}^{-1}\, {\rm cm}^{-2}\, {\rm s}^{-1}$. The gamma-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 of previous studies can be modeled with the leptonic scenario, inverse Compton scattering 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 the hadronic scenario in which gamma rays are generated from the decay of neutral pions produced by collisions between accelerated cosmic-ray protons and the ambient molecular cloud found in the gamma-ray emitting region. The cutoff energy of cosmic-ray protons $E_{\rm p\, cut}$, cut is estimated at ${\rm log}_{10}(E_{\rm p,\, cut}/{\rm TeV}) = 3.73^{+2.98}_{-0.66}$, suggesting that protons are accelerated up to the PeV energy range. Our study thus proposes that HESS J1849$-$000 should be further investigated as a new candidate for a Galactic PeV cosmic-ray accelerator, PeVatron.
Comment: 10 pages, 2 figures, Accepted for publication from the Astrophysical Journal
Comment: 10 pages, 2 figures, Accepted for publication from the Astrophysical Journal