SEARCH FOR GAMMA RAYS ABOVE 100 TeV FROM THE CRAB NEBULA WITH THE TIBET AIR SHOWER ARRAY AND THE 100 m<sup>2</sup>MUON DETECTOR

Amenomori, M.; Bi, X. J.; Chen, D.; Chen, T. L.; Chen, W. Y.; Cui, S. W.; Danzengluobu,; Ding, L. K.; Feng, C.; Feng, Z.; Feng, Z. Y.; Gou, Q. B.; Guo, Y. Q.; He, H. H.; He, Ze; Hibino, K.; Hotta, N.; Hu, Haibing; Hu, H. B.; Huang, J.; Jia, H. Y.; Jiang, L.; Kajino, F.; Kasahara, K.; Katayose, Y.; Kato, C.; Kawata, K.; Kozai, M.; Labaciren,; Le, G. M.; Li, A. F.; Li, H. J.; Li, W. J.; Liu, C.; Liu, J. S.; Liu, M. Y.; Lü, H.; Meng, X. R.; Miyazaki, Tetsuya; Mizutani, K.; Munakata, K.; Nakajima, T.; Nakamura, Yuya; Nanjo, H.; Nakamura, Masaki; Niwa, T.; Ohnishi, M.; Ohta, I.; Ozawa, S.; Qian, X. L.; Qu, X. B.; Saito, T.; Saito, Takayuki; Sakata, M.; Sako, T. K.; Shao, J.; Shibata, M.; Shirai, T.; Sugimoto, H.; Takita, M.; Tan, Y. H.; Tateyama, N.; Torii, Shoji; Tsuchiya, H.; Udo, S.; Wang, H.; Wu, H. R.; Xue, L.; Yamamoto, Y.; Yamauchi, K.; Yang, Zhen; Yasue, S.; Yuan, A. F.; Yuda, T.; Zhai, L. M.; Zhang, H. M.; Zhang, J. L.; Zhang, X. Y.; Zhang, Y.; Zhang, Yi; Zhang, Ying; Zhaxisangzhu,; Zhou, X. X.

doi:10.1088/0004-637x/813/2/98

Cited by 28 publications

(11 citation statements)

References 18 publications

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“…The spectrum measured by the Tibet AS þ MD well follows the data of the HEGRA experiment and extends to the sub-PeV energy regime without a cutoff sign. The integral fluxes observed by the Tibet AS þ MD array are also calculated to be Fð>100 TeVÞ ¼ ð3.29 þ1.06 −0.87 Þ × 10 −15 cm −2 s −1 and Fð>250 TeVÞ ¼ ð5.72 þ5.72 −3.48 Þ×10 −16 cm −2 s −1 , respectively, which are consistent with and lower than the previous upper limits given by the CASA-MIA experiment [13] and Tibet AS with 100 m 2 prototype MD [15], respectively.…”

supporting

confidence: 85%

“…In 2007, a prototype underground water-Cherenkov-type MD with a detection area of 100 m 2 for two cells was built beneath the Tibet-III array. With this MD, we determined the most stringent flux upper limit for Crab photons of >140 TeV [15].…”

mentioning

confidence: 99%

“…Our [14], respectively. The magenta arrows with plus mark show the previous upper limits at the 90% confidence level given by the Tibet AS and the 100 m 2 prototype MD [15]. The green squares, open squares, blue solid triangles, and blue crosses show flux points observed with three Cherenkov telescopes: HEGRA [12], MAGIC [29], H.E.S.S.…”

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confidence: 99%

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Highest Energy Astrophysical Photons Detected

Ong

2019

Physics

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We report on the highest energy photons from the Crab Nebula observed by the Tibet air shower array with the underground water-Cherenkov-type muon detector array. Based on the criterion of a muon number measured in an air shower, we successfully suppress 99.92% of the cosmic-ray background events with energies E > 100 TeV. As a result, we observed 24 photonlike events with E > 100 TeV against 5.5 background events, which corresponds to a 5.6σ statistical significance. This is the first detection of photons with E > 100 TeV from an astrophysical source.

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supporting

confidence: 85%

mentioning

confidence: 99%

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Highest Energy Astrophysical Photons Detected

Ong

2019

Physics

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“…The particles of the shower can be detected via either scintillation counters (used by the Tibet Air Shower Array, Amenomori et al 2015), resistive plate chambers (used by the Astrophysical Radiation with Ground-based Observatory at Yang Ba Jing, argo-ybj, Bartoli et al 2013) or water Cherenkov detectors. The latter has proven to be the most sensitive method and was successfully explored by the Milagro experiment between 1999 and 2008 (Abdo et al, 2009b).…”

Section: Particle Samplermentioning

confidence: 99%

Revealing the Most Energetic Light from Pulsars and Their Nebulae

Fidalgo

2019

Springer Theses

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© David Carreto Fidalgo, 2018 157 8.1 The young and energetic gamma-ray pulsar psr j0631+1036 158 8.2 Observational hints of a TeV pulsar wind nebula 161 9 MAGIC observations of PSR J0631: analysis and results 165 9.1 Data set and quality selection 166 9.2 Moonlight data and extended source analysis 168 9.3 Analysis results and discussion 172 Summary and conclusions 177 Appendix 183 A Interaction processes in very-high-energy astrophysics 185 B Pulsar timing 191 C The on-site analysis chain of MAGIC 195 D Details on the Crab pulsar analysis 201 References 207 viii Thesis advisor: Abstract Background. The observation of Very-High-Energy (vhe, >100 GeV) gamma raysis key in studying the non-thermal sources of radiation in our Universe. Pulsars and Pulsar Wind Nebulae (pwne) are two source classes that are known to emit vhe gamma rays. While pulsar wind nebulae are the dominant vhe gamma-ray source class in our galaxy, only two pulsars have been detected above 100 GeV so far. Most pulsar models explain gamma-ray emission via synchro-curvature radiation in the radiation-reaction limited regime, which leads to a sharp cut-off in the pulsar spectrum at energies of a few GeV.However, the detection of pulsed emission from the Crab pulsar up to hundreds of GeV by magic and veritas, suggests that classical pulsar models do not provide a full picture of the emission mechanisms at work. TeV pulsar wind nebulae, on the other hand, are observed via their inverse Compton radiation and are primarily found around young and energetic pulsars located towards the inner Milky Way. Detections of TeV pwne in the outer part of our galaxy are scarce, but could provide valuable input for the connection between the interstellar radiation field and the pwn luminosity.Aims. The principle goal of this thesis is to study the very-high-energy emission of the Crab pulsar. We aim to answer the long-standing question up to what energies pulsars are able to radiate and what is the emission mechanism behind it. We further exploit the pulsed vhe emission from the Crab to investigate fundamental physics testing for Lorentz Invariance Violation (liv), in terms of a wavelength dependent speed of light. To deepen our understanding of the pulsar emission mechanism at the highest energies, further pulsars have to be discovered above 100 GeV. To this end we search among pulsars already detected at around 1 GeV for the best candidates to emit gamma-rays in the vhe range.Another aim of this thesis is to discover a new pulsar wind nebula towards the outer part of our galaxy with the magic telescopes.ix Thesis advisor:Methods. We analyzed more than 400 hours of good-quality data of the Crab pulsar obtained by the magic telescopes between 2007 and 2016. This unprecedented large data set allowed us to effectively explore the Crab pulse profile and spectrum above 400 GeV.To test for Lorentz invariance violation, primarily foreseen by theories of quantum gravity, we modeled the vhe emission of the Crab pulsar and employed Bayesian inference to derive lower limits on...

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“…Our MC simulation reproduces well the experimental data obtained by the prototype muon detector. With the prototype muon detector, we set the most stringent upper limit on gamma-ray flux above 140 TeV from the Crab [22].…”

Section: Pos(icrc2017)831mentioning

confidence: 99%

The Tibet AS+MD Project; status report 2017

Takita¹,

Amenomori²,

Bi³

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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We built a large (approximately 4,000 m 2 ) water Cherenkov-type muon detector array under the existing Tibet air shower array at 4,300 m above sea level, to observe 10-1000 TeV gamma rays from cosmic-ray accelerators in our Galaxy with wide field of view at very low background level. A gamma-ray induced air shower has significantly less muons compared with a cosmic-ray induced one. Therefore, we can effectively discriminate between primary gamma rays and cosmicray background events by means of counting number of muons in an air shower event by the muon detector array. We make a status report on the experiment.

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SEARCH FOR GAMMA RAYS ABOVE 100 TeV FROM THE CRAB NEBULA WITH THE TIBET AIR SHOWER ARRAY AND THE 100 m²MUON DETECTOR

Cited by 28 publications

References 18 publications

Highest Energy Astrophysical Photons Detected

Highest Energy Astrophysical Photons Detected

Revealing the Most Energetic Light from Pulsars and Their Nebulae

The Tibet AS+MD Project; status report 2017

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SEARCH FOR GAMMA RAYS ABOVE 100 TeV FROM THE CRAB NEBULA WITH THE TIBET AIR SHOWER ARRAY AND THE 100 m2MUON DETECTOR

Cited by 28 publications

References 18 publications

Highest Energy Astrophysical Photons Detected

Highest Energy Astrophysical Photons Detected

Revealing the Most Energetic Light from Pulsars and Their Nebulae

The Tibet AS+MD Project; status report 2017

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SEARCH FOR GAMMA RAYS ABOVE 100 TeV FROM THE CRAB NEBULA WITH THE TIBET AIR SHOWER ARRAY AND THE 100 m²MUON DETECTOR