학술논문
Observation of Gamma Rays up to 320 TeV from the Middle-aged TeV Pulsar Wind Nebula HESS J1849−000
Document Type
article
Author
M. Amenomori; S. Asano; Y. W. Bao; X. J. Bi; D. Chen; T. L. Chen; W. Y. Chen; Xu Chen; Y. Chen; Cirennima; S. W. Cui; Danzengluobu; L. K. Ding; J. H. Fang; K. Fang; C. F. Feng; Zhaoyang Feng; Z. Y. Feng; Qi Gao; A. Gomi; Q. B. Gou; Y. Q. Guo; Y. Y. Guo; Y. Hayashi; H. H. He; Z. T. He; K. Hibino; N. Hotta; Haibing Hu; H. B. Hu; K. Y. Hu; J. Huang; H. Y. Jia; L. Jiang; P. Jiang; H. B. Jin; K. Kasahara; Y. Katayose; C. Kato; S. Kato; I. Kawahara; T. Kawashima; K. Kawata; M. Kozai; D. Kurashige; Labaciren; G. M. Le; A. F. Li; H. J. Li; W. J. Li; Y. Li; Y. H. Lin; B. Liu; C. Liu; J. S. Liu; L. Y. Liu; M. Y. Liu; W. Liu; H. Lu; X. R. Meng; Y. Meng; K. Munakata; K. Nagaya; Y. Nakamura; Y. Nakazawa; H. Nanjo; C. C. Ning; M. Nishizawa; R. Noguchi; M. Ohnishi; S. Okukawa; S. Ozawa; X. Qian; X. L. Qian; X. B. Qu; T. Saito; Y. Sakakibara; M. Sakata; T. Sako; T. K. Sako; T. Sasaki; J. Shao; M. Shibata; A. Shiomi; H. Sugimoto; W. Takano; M. Takita; Y. H. Tan; N. Tateyama; S. Torii; H. Tsuchiya; S. Udo; H. Wang; S. F. Wang; Y. P. Wang; Wangdui; H. R. Wu; Q. Wu; J. L. Xu; L. Xue; Z. Yang; Y. Q. Yao; J. Yin; Y. Yokoe; Y. L. Yu; A. F. Yuan; L. M. Zhai; H. M. Zhang; J. L. Zhang; X. Zhang; X. Y. Zhang; Y. Zhang; Yi Zhang; Ying Zhang; S. P. Zhao; Zhaxisangzhu; X. X. Zhou; Y. H. Zou
Source
The Astrophysical Journal, Vol 954, Iss 2, p 200 (2023)
Subject
Language
English
ISSN
1538-4357
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 σ and 4.4 σ levels above 25 TeV and 100 TeV, respectively, in units of the Gaussian standard deviation σ . The energy spectrum measured between 40 TeV < E < 320 TeV for the first time is described with a simple power-law function of ${dN}/{dE}={(2.86\pm 1.44)\times {10}^{-16}(E/40\,\mathrm{TeV})}^{-2.24\pm 0.41}\,{\mathrm{TeV}}^{-1}\,{\mathrm{cm}}^{-2}\,{{\rm{s}}}^{-1}$ . The gamma-ray energy spectrum from the sub-TeV ( E < 1 TeV) to sub-PeV (100 TeV < E < 1 PeV) ranges, including the results of previous studies, can be modeled with the leptonic scenario, i.e., 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 _p,cut is estimated as ${\mathrm{log}}_{10}({E}_{{\rm{p}},\mathrm{cut}}/\mathrm{TeV})={3.73}_{-0.66}^{+2.98}$ , 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 as a Galactic PeV cosmic-ray accelerator, or “PeVatron.”