Flux upper limits of diffuse TeV gamma rays from the Galactic plane using the effective area of the Tibet-II and -III arrays

Amenomori, M.; Ayabe, S.; Cui, S. W.; Danzengluobu,; Ding, L. K.; Ding, X. H.; Feng, C. F.; Feng, Z.; Gao, X. Y.; Geng, Q. X.; Guo, H. W.; He, H. H.; He, M.; Hibino, K.; Hotta, N.; Hu, Haibing; Huang, J.; Huang, Q.; Izumi, Mitsuru; Jia, H. Y.; Kajino, F.; Kasahara, K.; Katayose, Y.; Kato, C.; Kawata, K.; Labaciren,; Le, G. M.; Li, J. Y.; Lü, H.; Lu, S. L.; Meng, X. R.; Mizutani, K.; Mu, J.; Munakata, K.; Nagai, A.; Nanjo, H.; Nakamura, Masaki; Ohnishi, M.; Ohta, I.; Onuma, H.; Ouchi, T.; Ozawa, S.; Ren, J. R.; Saito, T.; Sakata, M.; Sasaki, Takashi; Shibata, M.; Shirai, T.; Sugimoto, H.; Takita, M.; Tan, Y. H.; Tateyama, N.; Torii, Shoji; Tsuchiya, H.; Udo, S.; Utsugi, Toshihiro; Wang, B. S.; Wang, H.; Wang, X.; Wang, Y. G.; Wu, H. R.; Xue, L.; Yamamoto, Y.; Yan, C. T.; Yang, X. C.; Yasue, S.; Ye, Z. H.; Yu, G. C.; Yuan, A. F.; Yuda, T.; Zhang, H. M.; Zhang, J. L.; Zhang, N. J.; Y., Zhang, X.; Zhang, Y.; Zhaxisangzhu,; Zhou, X. X.

doi:10.1016/j.asr.2005.08.049

Cited by 18 publications

(6 citation statements)

References 14 publications

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“…This is intriguing, as an unphysical break in the TeV proton spectrum would be necessary to produce any such feature with hadronic γ-ray emission. For clarity, we do not show relevant (but less sensitive) results from Whipple [34], HEGRA [35], TIBET-II or TIBET-III [36], noting that our model is consistent with the upper-limits of each study. PeV γ-ray constraints from CASA-MIA [37] and KAS-CADE [38] may be relevant if we did not include an exponentially suppressed e + e − spectrum above 100 TeV.…”

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confidence: 64%

Pulsar TeV Halos Explain the Diffuse TeV Excess Observed by Milagro

Linden

Buckman

2018

Phys. Rev. Lett.

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Milagro observations have found bright, diffuse TeV emission concentrated along the galactic plane of the Milky Way. The intensity and spectrum of this emission is difficult to explain with current models of hadronic γ-ray production, and has been named the "TeV excess." We show that TeV emission from pulsars naturally explains this excess. Recent observations have detected "TeV halos" surrounding pulsars that are either nearby or particularly luminous. Extrapolating this emission to the full population of Milky Way pulsars indicates that the ensemble of "subthreshold" sources necessarily produces bright TeV emission diffusively along the Milky Way plane. Models indicate that the TeV halo γ-ray flux exceeds that from hadronic γ rays above an energy of ∼500 GeV. Moreover, the spectrum and intensity of TeV halo emission naturally matches the TeV excess. Finally, we show that upcoming HAWC observations will resolve a significant fraction of the TeV excess into individual TeV halos, conclusively confirming, or ruling out, this model.

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confidence: 64%

Pulsar TeV Halos Explain the Diffuse TeV Excess Observed by Milagro

Linden

Buckman

2018

Phys. Rev. Lett.

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“…On the other hand, air shower arrays providing a large FOV and a very high duty cycle look more adequate for sky survey purposes. Many air shower experiments have set upper limits to diffuse gamma-rays, such as Tibet ASγ at TeV energies (Amenomori et al 2006), and EAS-TOP (Aglietta et al 1992), KASCADE (Haungs et al 2006),and CASA-MIA (Borione et al 1998) at energies >100 TeV. The Milagro detector has made the first positive observation of the diffuse gamma-ray flux from the Galactic plane, measuring the integral flux above 3.5 TeV in the region 40°< l < 100°, b 5 | | <° (Atkins et al 2005).…”

Section: Introductionmentioning

confidence: 99%

Study of the Diffuse Gamma-Ray Emission From the Galactic Plane With Argo-Ybj

Bartoli¹,

Bernardini²,

Bi³

et al. 2015

ApJ

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The events recorded by ARGO-YBJ in more than fiveyears of data collection have been analyzed to determine the diffuse gamma-ray emission in the Galactic plane at Galactic longitudes 25°< l < 100°and Galactic latitudes b 5 | | <°. The energy range covered by this analysis, from ∼350 GeV to ∼2 TeV, allows the connection of the region explored by Fermi with the multi-TeV measurements carried out by Milagro. Our analysis has been focused on two selected regions of the Galactic plane, i.e., 40°< l < 100°and 65°< l < 85°(the Cygnus region), where Milagro observed an excess with respect to the predictions of current models. Great care has been taken in order to mask the most intense gamma-ray sources, including the TeV counterpart of the Cygnus cocoon recently identified by ARGO-YBJ, and to remove residual contributions. The ARGO-YBJ results do not show any excess at sub-TeV energies corresponding to the excess found by Milagro, and are consistent with the predictions of the Fermi model for the diffuse Galactic emission. From the measured energy distribution we derive spectral indices and the differential flux at 1 TeV of the diffuse gamma-ray emission in the sky regions investigated.

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“…We also searched for multi-TeV diffuse gamma rays from the galactic plane [6,20]. As there was no significant signal, flux upper limits were obtained.…”

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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Flux upper limits of diffuse TeV gamma rays from the Galactic plane using the effective area of the Tibet-II and -III arrays

Cited by 18 publications

References 14 publications

Pulsar TeV Halos Explain the Diffuse TeV Excess Observed by Milagro

Pulsar TeV Halos Explain the Diffuse TeV Excess Observed by Milagro

Study of the Diffuse Gamma-Ray Emission From the Galactic Plane With Argo-Ybj

The Tibet AS+MD Project; status report 2017

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