Author: "Ohnishi, M" - Searchworks@Jio Institute Digital Library Search Results

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2,430 results on '"Ohnishi, M"'

1. Characteristics of temporal variability of long-duration bursts of high-energy radiation associated with thunderclouds on the Tibetan plateau

Author: Tsuchiya, H., Hibino, K., Kawata, K., Ohnishi, M., Takita, M., Munakata, K., Kato, C., Shimoda, S., Shi, Q., Wang, S., Han, C., and Zhai, L.
Subjects: Physics - Geophysics, Astrophysics - Earth and Planetary Astrophysics, Physics - Atmospheric and Oceanic Physics
Abstract: From 1998 to 2017, neutron monitors located at an altitude of 4300 m on the Tibetan plateau detected 127 long-duration bursts of high-energy radiation in association with thunderclouds. These bursts typically lasted for 10 to 40 minutes, and 89\% of them occurred between 10:00 and 24:00 local time. They were also found to be more likely to occur at night, especially during 18:00$-$06:00 local time period. The observed diurnal and seasonal variations in burst frequency were consistent with the frequencies of lightning and precipitation on the Tibetan plateau. Based on 19 years of data, the present study suggests that an annual variation in burst frequency has a periodicity of $\sim$16 years and a lag of $\sim$3 years relative to solar activity., Comment: 28 pages, accepted for publication in Progress in Earth and Planetary Science
Published: 2024
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2. On the source contribution to the Galactic diffuse gamma rays above 398 TeV detected by the Tibet AS{\gamma} experiment

Author: Kato, S., Chen, D., Huang, J., Kawashima, T., Kawata, K., Mizuno, A., Ohnishi, M., Sako, T., Sako, T. K., Takita, M., and Yokoe, Y.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Potential contribution from gamma-ray sources to the Galactic diffuse gamma rays observed above 100 TeV (sub-PeV energy range) by the Tibet AS{\gamma} experiment is an important key to interpreting recent multi-messenger observations. This paper reveals a surprising fact: none of the 23 Tibet AS{\gamma} diffuse gamma-ray events above 398TeV within the Galactic latitudinal range of |b| < 10 deg. come from the 43 sub-PeV gamma-ray sources reported in the 1LHAASO catalog, which proves that these sources are not the origins of the Tibet AS{\gamma} diffuse gamma-ray events. No positional overlap between the Tibet AS{\gamma} diffuse gamma-ray events and the sub-PeV LHAASO sources currently supports the diffusive nature of the Tibet AS{\gamma} diffuse gamma-ray events, although their potential origin in the gamma-ray sources yet unresolved in the sub-PeV energy range cannot be ruled out., Comment: 5 pages, 2 figures Accepted for publication from The Astrophysical Journal Letters. arXiv admin note: text overlap with arXiv:2309.16078
Published: 2024

3. Nobeyama Cygnus-X Survey: Physical Properties of C$^{18}$O clumps in DR-6(W), DR-9 and DR-13S regions

Author: Toledano--Juárez, I., de la Fuente, E., Kawata, K., Trinidad, M. A., Tafoya, D., Yamagishi, M., Takekawa, S., Ohnishi, M., Nishimura, A., Kato, S., Sako, T., Takita, M., and Yadav, R. K.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: Cygnus-X is considered a region of interest for high-energy astrophysics, since the Cygnus OB2 association has been confirmed as a PeVatron in the Cygnus cocoon. In this research note, we present new high-resolution (16'') $^{12,13}$CO(J=1$\rightarrow$0) and C$^{18}$O (J=1$\rightarrow$0) observations obtained with the Nobeyama 45-m radiotelescope, to complement the Nobeyama Cygnus-X Survey. We discovered 19 new C$^{18}$O clumps associated with the star-forming regions DR-6W, DR-9, and DR13S. We present the physical parameters of these clumps, which are consistent with the neighboring covered regions. We confirm the clumpy nature of these regions and of a filament located between DR6 and DR6W. These results strongly suggest that star formation occurs in these regions with clumps of sizes $\sim$10$^{-1}$ pc, masses $\sim$10$^2$ M$_\odot$, and H$_2$ densities of $\sim$10$^4$ cm$^{-3}$., Comment: 8 pages, 3 Figures, 1 Table. https://pos.sissa.it/444/631/pdf
Published: 2023

4. Quantitative constraint on the source contribution to the Galactic diffuse gamma rays detected by the Tibet air shower array

Author: Kato, S., Chen, D., Huang, J., Kawashima, T., Kawata, K., Mizuno, A., Ohnishi, M., Sako, T., Sako, T. K., Takita, M., and Yokoe, Y.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The fraction of the contribution from yet-unresolved gamma-ray sources in the Galactic diffuse gamma rays observed by the Tibet air shower array is an important key to interpreting recent multi-messenger observations. This paper shows a surprising fact: no Tibet diffuse events above 398TeV come from the gamma-ray sources newly detected above 100 TeV by LHAASO. Based on this observational fact, the contribution of sources unresolved by LHAASO to the Tibet diffuse events is estimated to be less than 31% above 398TeV with a 99% confidence level. Our result shows that unresolved sources make only a sub-dominant contribution to the Tibet diffuse events above 398 TeV and a large fraction of the events are truly a diffusive nature., Comment: Calculations in Eq-(2) should have used the probability p that a Tibet diffuse gamma-ray event is of unresolved-source origin, but the parameter p in Eq-(2) is the probability that a gamma-ray event above 398 TeV from a source marginally detected by LHAASO is detected by the Tibet. This mistake leads to a wrong estimate of the limit on the source fraction to the Tibet diffuse gamma-ray events
Published: 2023

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

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., and Zou, Y. H.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
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$-$000 should be further investigated as a new candidate for a Galactic PeV cosmic-ray accelerator, PeVatron., Comment: 10 pages, 2 figures, Accepted for publication from the Astrophysical Journal
Published: 2023
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6. Measurement of the Gamma-Ray Energy Spectrum beyond 100 TeV from the HESS J1843$-$033 Region

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., 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., 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., Liu, X. L., Lou, Y. -Q., Lu, H., Meng, X. R., Meng, Y., Munakata, K., Nagaya, K., Nakamura, Y., Nakazawa, Y., Nanjo, H., Ning, C. C., Nishizawa, M., Ohnishi, M., Okukawa, S., Ozawa, S., Qian, L., Qian, X., Qian, X. L., Qu, X. B., Saito, T., Sakakibara, Y., Sakata, M., Sako, T., Sako, T. K., 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, Y. P., Wangdui, Wu, H. R., Wu, Q., Xu, J. L., Xue, L., Yang, Z., Yao, Y. Q., Yin, J., Yokoe, Y., Yu, N. P., Yuan, A. F., Zhai, L. M., Zhang, C. P., Zhang, H. M., Zhang, J. L., Zhang, X., Zhang, X. Y., Zhang, Y., Zhang, Yi, Zhang, Ying, Zhao, S. P., Zhaxisangzhu, and Zhou, X. X.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: HESS J1843$-$033 is a very-high-energy gamma-ray source whose origin remains unidentified. This work presents, for the first time, the energy spectrum of gamma rays beyond $100\, {\rm TeV}$ from the HESS J1843$-$033 region using the data recorded by the Tibet air shower array and its underground muon detector array. A gamma-ray source with an extension of $0.34^{\circ} \pm 0.12^{\circ}$ is successfully detected above $25\, {\rm TeV}$ at $(\alpha,\, \delta) = (281.09^{\circ}\pm 0.10^{\circ},\, -3.76^{\circ}\pm 0.09^{\circ})$ near HESS J1843$-$033 with a statistical significance of $6.2\, \sigma$, and the source is named TASG J1844$-$038. The position of TASG J1844$-$038 is consistent with those of HESS J1843$-$033, eHWC J1842$-$035, and LHAASO J1843$-$0338. The measured gamma-ray energy spectrum in $25\, {\rm TeV} < E < 130\, {\rm TeV}$ is described with ${\rm d}N/{\rm d}E = (9.70\pm 1.89)\times 10^{-16} (E/40\, {\rm TeV})^{-3.26\pm 0.30}\, {\rm TeV}^{-1} {\rm cm}^{-2} {\rm s}^{-1}$, and the spectral fit to the combined spectra of HESS J1843$-$033, LHAASO J1843$-$0338, and TASG J1844$-$038 implies the existence of a cutoff at $49.5\pm 9.0\, {\rm TeV}$. Associations of TASG J1844-038 with SNR G28.6$-$0.1 and PSR J1844-0346 are also discussed in detail for the first time., Comment: 11 pages, 4 figures, 1 table
Published: 2023
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7. First High-speed Video Camera Observations of a Lightning Flash Associated with a Downward Terrestrial Gamma-ray Flash

Author: Abbasi, R. U., Saba, M. M. F., Belz, J. W., Krehbiel, P. R., Rison, W., Kieu, N., da Silva, D. R., Rodeheffer, Dan, Stanley, M. A., Remington, J., Mazich, J., LeVon, R., Smout, K., Petrizze, A., Abu-Zayyad, T., Allen, M., Arai, Y., Arimura, R., Barcikowski, E., Bergman, D. R., Blake, S. A., Buckland, I., Cheon, B. G., Chikawa, M., Fujii, T., Fujisue, K., Fujita, K., Fujiwara, R., Fukushima, M., Furlich, G., Globus, N., Gonzalez, R., Hanlon, W., Hayashida, N., He, H., Hibino, K., Higuchi, R., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ito, H., Ivanov, D., Iwakura, H., Iwasaki, A., Jeong, H. M., Jeong, S., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kasami, S., Kawakami, S., Kawata, K., Kharuk, I., Kido, E., Kim, H. B., Kim, J. H., Kim, S. W., Kimura, Y., Komae, I., Kubota, Y., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lee, K. H., Lubsandorzhiev, B., Lundquist, J. P., Matsumiya, H., Matsuyama, T., Matthews, J. N., Mayta, R., Myers, I., Nagataki, S., Nakai, K., Nakamura, R., Nakamura, T., Nakamura, Y., Nakazawa, A., Nishio, E., Nonaka, T., Oda, H., Ogio, S., Ohnishi, M., Ohoka, H., Oku, Y., Okuda, T., Omura, Y., Ono, M., Oshima, A., Ozawa, S., Park, I. H., Potts, M., Pshirkov, M. S., Rodriguez, D. C., Rott, C., Rubtsov, G. I., Ryu, D., Sagawa, H., Sakaki, N., Sako, T., Sakurai, N., Sato, K., Seki, T., Sekino, K., Shah, P. D., Shibasaki, Y., Shibata, N., Shibata, T., Shikita, J., Shimodaira, H., Shin, B. K., Shin, H. S., Shinto, D., Smith, J. D., Sokolsky, P., Stokes, B. T., Stroman, T. A., Takahashi, K., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, K., Tanaka, M., Tanoue, Y., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsuda, R., Tsunesada, Y., Udo, S., Uehama, T., Urban, F., Warren, D., Wong, T., Yamamoto, M., Yamazaki, K., Yashiro, K., Yoshida, F., Zhezher, Y., and Zundel, Z.
Subjects: Physics - Atmospheric and Oceanic Physics, Astrophysics - Instrumentation and Methods for Astrophysics, High Energy Physics - Experiment
Abstract: In this paper, we present the first high-speed video observation of a cloud-to-ground lightning flash and its associated downward-directed Terrestrial Gamma-ray Flash (TGF). The optical emission of the event was observed by a high-speed video camera running at 40,000 frames per second in conjunction with the Telescope Array Surface Detector, Lightning Mapping Array, interferometer, electric-field fast antenna, and the National Lightning Detection Network. The cloud-to-ground flash associated with the observed TGF was formed by a fast downward leader followed by a very intense return stroke peak current of -154 kA. The TGF occurred while the downward leader was below cloud base, and even when it was halfway in its propagation to ground. The suite of gamma-ray and lightning instruments, timing resolution, and source proximity offer us detailed information and therefore a unique look at the TGF phenomena.
Published: 2022
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8. Search for Spatial Correlations of Neutrinos with Ultra-High-Energy Cosmic Rays

Author: The ANTARES collaboration, Albert, A., Alves, S., André, M., Anghinolfi, M., Ardid, M., Ardid, S., Aubert, J. -J., Aublin, J., Baret, B., Basa, S., Belhorma, B., Bendahman, M., Bertin, V., Biagi, S., Bissinger, M., Boumaaza, J., Bouta, M., Bouwhuis, M. C., Brânzaş, H., Bruijn, R., Brunner, J., Busto, J., Caiffi, B., Calvo, D., Capone, A., Caramete, L., Carr, J., Carretero, V., Celli, S., Chabab, M., Chau, T. N., Moursli, R. Cherkaoui El, Chiarusi, T., Circella, M., Coleiro, A., Coniglione, R., Coyle, P., Creusot, A., Díaz, A. F., Distefano, C., Di Palma, I., Domi, A., Donzaud, C., Dornic, D., Drouhin, D., Eberl, T., van Eeden, T., van Eijk, D., Khayati, N. El, Enzenhöfer, A., Fermani, P., Ferrara, G., Filippini, F., Fusco, L., Gatelet, Y., Gay, P., Glotin, H., Gozzini, R., Ruiz, R. Gracia, Graf, K., Guidi, C., Hallmann, S., van Haren, H., Heijboer, A. J., Hello, Y., Hernández-Rey, J. J., Hößl, J., Hofestädt, J., Huang, F., Illuminati, G., James, C. W., Jisse-Jung, B., de Jong, M., de Jong, P., Kadler, M., Kalekin, O., Katz, U., Khan-Chowdhury, N. R., Kouchner, A., Kreykenbohm, I., Kulikovskiy, V., Lahmann, R., Breton, R. Le, LeStum, S., Lefèvre, D., Leonora, E., Levi, G., Lopez-Coto, D., Loucatos, S., Maderer, L., Manczak, J., Marcelin, M., Margiotta, A., Marinelli, A., Martínez-Mora, J. A., Martino, B., Melis, K., Migliozzi, P., Moussa, A., Muller, R., Nauta, L., Navas, S., Nezri, E., Fearraigh, B. Ó, Păun, A., Păvălaş, G. E., Pellegrino, C., Perrin-Terrin, M., Pestel, V., Piattelli, P., Pieterse, C., Poirè, C., Popa, V., Pradier, T., Randazzo, N., Real, D., Reck, S., Riccobene, G., Romanov, A., Sánchez-Losa, A., Greus, F. Salesa, Samtleben, D. F. E., Sanguineti, M., Sapienza, P., Schnabel, J., Schumann, J., Schüssler, F., Seneca, J., Spurio, M., Stolarczyk, Th., Taiuti, M., Tayalati, Y., Tingay, S. J., Vallage, B., Van Elewyck, V., Versari, F., Viola, S., Vivolo, D., Wilms, J., Zavatarelli, S., Zegarelli, A., Zornoza, J. D., Zúñiga, J., collaboration, The IceCube, Abbasi, R., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Alameddine, J. M., Alispach, C., Alves Jr., A. A., Amin, N. M., Andeen, K., Anderson, T., Anton, G., Argüelles, C., Ashida, Y., Axani, S., Bai, X., V., A. Balagopal, Barbano, A., Barwick, S. W., Bastian, B., Basu, V., Baur, S., Bay, R., Beatty, J. J., Becker, K. -H., Tjus, J. Becker, Bellenghi, C., BenZvi, S., Berley, D., Bernardini, E., Besson, D. Z., Binder, G., Bindig, D., Blaufuss, E., Blot, S., Boddenberg, M., Bontempo, F., Borowka, J., Böser, S., Botner, O., Böttcher, J., Bourbeau, E., Bradascio, F., Braun, J., Brinson, B., Bron, S., Brostean-Kaiser, J., Browne, S., Burgman, A., Burley, R. T., Busse, R. S., Campana, M. A., Carnie-Bronca, E. G., Chen, C., Chen, Z., Chirkin, D., Choi, K., Clark, B. A., Clark, K., Classen, L., Collin, G. H., Conrad, J. M., Coppin, P., Correa, P., Cowen, D. F., Cross, R., Dappen, C., Dave, P., De Clercq, C., DeLaunay, J. J., López, D. Delgado, Dembinski, H., Deoskar, K., Desai, A., Desiati, P., de Vries, K. D., de Wasseige, G., de With, M., DeYoung, T., Diaz, A., Díaz-Vélez, J. C., Dittmer, M., Dujmovic, H., Dunkman, M., DuVernois, M. A., Dvorak, E., Ehrhardt, T., Eller, P., Erpenbeck, H., Evans, J., Evenson, P. A., Fan, K. L., Fazely, A. R., Fedynitch, A., Feigl, N., Fiedlschuster, S., Fienberg, A. T., Filimonov, K., Finley, C., Fischer, L., Fox, D., Franckowiak, A., Friedman, E., Fritz, A., Fürst, P., Gaisser, T. K., Gallagher, J., Ganster, E., Garcia, A., Garrappa, S., Gerhardt, L., Ghadimi, A., Glaser, C., Glauch, T., Glüsenkamp, T., Gonzalez, J. G., Goswami, S., Grant, D., Grégoire, T., Griswold, S., Günther, C., Gutjahr, P., Haack, C., Hallgren, A., Halliday, R., Halve, L., Halzen, F., Minh, M. Ha, Hanson, K., Hardin, J., Harnisch, A. A., Haungs, A., Hebecker, D., Helbing, K., Henningsen, F., Hettinger, E. C., Hickford, S., Hignight, J., Hill, C., Hill, G. C., Hoffman, K. D., Hoffmann, R., Hokanson-Fasig, B., Hoshina, K., Huber, M., Huber, T., Hultqvist, K., Hünnefeld, M., Hussain, R., Hymon, K., In, S., Iovine, N., Ishihara, A., Jansson, M., Japaridze, G. S., Jeong, M., Jin, M., Jones, B. J. P., Kang, D., Kang, W., Kang, X., Kappes, A., Kappesser, D., Kardum, L., Karg, T., Karl, M., Karle, A., Kauer, M., Kellermann, M., Kelley, J. L., Kheirandish, A., Kin, K., Kintscher, T., Kiryluk, J., Klein, S. R., Koirala, R., Kolanoski, H., Kontrimas, T., Köpke, L., Kopper, C., Kopper, S., Koskinen, D. J., Koundal, P., Kovacevich, M., Kowalski, M., Kozynets, T., Kun, E., Kurahashi, N., Lad, N., Gualda, C. Lagunas, Lanfranchi, J. L., Larson, M. J., Lauber, F., Lazar, J. P., Lee, J. W., Leonard, K., Leszczyńska, A., Li, Y., Lincetto, M., Liu, Q. R., Liubarska, M., Lohfink, E., Mariscal, C. J. Lozano, Lucarelli, F., Ludwig, A., Luszczak, W., Lyu, Y., Ma, W. Y., Madsen, J., Mahn, K. B. M., Makino, Y., Mancina, S., Martinez-Soler, I., Maruyama, R., Mase, K., McElroy, T., McNally, F., Mead, J. V., Meagher, K., Mechbal, S., Medina, A., Meier, M., Meighen-Berger, S., Micallef, J., Mockler, D., Montaruli, T., Moore, R. W., Morse, R., Moulai, M., Naab, R., Nagai, R., Naumann, U., Necker, J., Nguyên, L. V., Niederhausen, H., Nisa, M. U., Nowicki, S. C., Pollmann, A. Obertacke, Oehler, M., Oeyen, B., Olivas, A., O'Sullivan, E., Pandya, H., Pankova, D. V., Park, N., Parker, G. K., Paudel, E. N., Paul, L., Heros, C. Pérez de los, Peters, L., Peterson, J., Philippen, S., Pieper, S., Pittermann, M., Pizzuto, A., Plum, M., Popovych, Y., Porcelli, A., Rodriguez, M. Prado, Price, P. B., Pries, B., Przybylski, G. T., Raab, C., Rack-Helleis, J., Raissi, A., Rameez, M., Rawlins, K., Rea, I. C., Rehman, A., Reichherzer, P., Reimann, R., Renzi, G., Resconi, E., Reusch, S., Rhode, W., Richman, M., Riedel, B., Roberts, E. J., Robertson, S., Roellinghoff, G., Rongen, M., Rott, C., Ruhe, T., Ryckbosch, D., Cantu, D. Rysewyk, Safa, I., Saffer, J., Herrera, S. E. Sanchez, Sandrock, A., Santander, M., Sarkar, S., Satalecka, K., Schaufel, M., Schindler, S., Schmidt, T., Schneider, A., Schneider, J., Schröder, F. G., Schumacher, L., Schwefer, G., Sclafani, S., Seckel, D., Seunarine, S., Sharma, A., Shefali, S., Silva, M., Skrzypek, B., Smithers, B., Snihur, R., Soedingrekso, J., Soldin, D., Spannfellner, C., Spiczak, G. M., Spiering, C., Stachurska, J., Stamatikos, M., Stanev, T., Stein, R., Stettner, J., Steuer, A., Stezelberger, T., Stürwald, T., Stuttard, T., Sullivan, G. W., Taboada, I., Ter-Antonyan, S., Tilav, S., Tischbein, F., Tollefson, K., Tönnis, C., Toscano, S., Tosi, D., Trettin, A., Tselengidou, M., Tung, C. F., Turcati, A., Turcotte, R., Turley, C. F., Twagirayezu, J. P., Ty, B., Elorrieta, M. A. 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I., Miramonti, L., Mollerach, S., Montanet, F., Morejon, L., Morello, C., Mostafá, M., Müller, A. L., Muller, M. A., Mulrey, K., Mussa, R., Muzio, M., Namasaka, W. M., Nasr-Esfahani, A., Nellen, L., Nicora, G., Niculescu-Oglinzanu, M., Niechciol, M., Nitz, D., Nosek, D., Novotny, V., Nožka, L., Nucita, A., Núñez, L. A., Oliveira, C., Palatka, M., Pallotta, J., Papenbreer, P., Parente, G., Parra, A., Pawlowsky, J., Pech, M., Pȩkala, J., Pelayo, R., Peña-Rodriguez, J., Martins, E. E. Pereira, Armand, J. Perez, Bertolli, C. Pérez, Perlin, M., Perrone, L., Petrera, S., Petrucci, C., Pierog, T., Pimenta, M., Pirronello, V., Platino, M., Pont, B., Pothast, M., Privitera, P., Prouza, M., Puyleart, A., Querchfeld, S., Rautenberg, J., Ravignani, D., Reininghaus, M., Ridky, J., Riehn, F., Risse, M., Rizi, V., de Carvalho, W. Rodrigues, Rojo, J. Rodriguez, Roncoroni, M. J., Rossoni, S., Roth, M., Roulet, E., Rovero, A. C., Ruehl, P., Saftoiu, A., Saharan, M., Salamida, F., Salazar, H., Salina, G., Gomez, J. D. Sanabria, Sánchez, F., Santos, E. M., Santos, E., Sarazin, F., Sarmento, R., Sarmiento-Cano, C., Sato, R., Savina, P., Schäfer, C. M., Scherini, V., Schieler, H., Schimassek, M., Schimp, M., Schlüter, F., Schmidt, D., Scholten, O., Schoorlemmer, H., Schovánek, P., Schulte, J., Schulz, T., Sciutto, S. J., Scornavacche, M., Segreto, A., Sehgal, S., Shellard, R. C., Sigl, G., Silli, G., Sima, O., Smau, R., Šmída, R., Sommers, P., Soriano, J. F., Squartini, R., Stadelmaier, M., Stanca, D., Stanič, S., Stasielak, J., Stassi, P., Streich, A., Suárez-Durán, M., Sudholz, T., Suomijärvi, T., Supanitsky, A. D., Szadkowski, Z., Tapia, A., Taricco, C., Timmermans, C., Tkachenko, O., Tobiska, P., Peixoto, C. J. Todero, Tomé, B., Torrès, Z., Travaini, A., Travnicek, P., Trimarelli, C., Tueros, M., Ulrich, R., Unger, M., Vaclavek, L., Vacula, M., Galicia, J. F. Valdés, Valore, L., Varela, E., Vásquez-Ramírez, A., Veberič, D., Ventura, C., Quispe, I. D. Vergara, Verzi, V., Vicha, J., Vink, J., Vorobiov, S., Wahlberg, H., Watanabe, C., Watson, A. A., Wiencke, L., Wilczyński, H., Wittkowski, D., Wundheiler, B., Yushkov, A., Zapparrata, O., Zas, E., Zavrtanik, D., Zavrtanik, M., Zehrer, L., collaboration, The Telescope Array, Abu-Zayyad, T., Allen, M., Arai, Y., Arimura, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Buckland, I., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., Fujisue, K., Fujita, K., Fujiwara, R., Fukushima, M., Fukushima, R., Furlich, G., Globus, N., Gonzalez, R., Hanlon, W., Hayashi, M., Hayashida, N., He, H., Hibino, K., Higuchi, R., Honda, K., Ikeda, D., Inadomi, T., Inoue, N., Ishii, T., Ito, H., Ivanov, D., Iwakura, H., Iwasaki, A., Jeong, H. M., Jeong, S., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kasami, S., Kawakami, S., Kawana, S., Kawata, K., Kharuk, I., Kido, E., Kim, H. B., Kim, J. H., Kim, S. W., Kimura, Y., Kishigami, S., Kubota, Y., Kurisu, S., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lee, K. H., Lubsandorzhiev, B., Machida, K., Matsumiya, H., Matsuyama, T., Matthews, J. N., Mayta, R., Minamino, M., Mukai, K., Myers, I., Nagataki, S., Nakai, K., Nakamura, R., Nakamura, T., Nakamura, Y., Nakazawa, A., Nishio, E., Nonaka, T., Oda, H., Ogio, S., Ohnishi, M., Ohoka, H., Oku, Y., Okuda, T., Omura, Y., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Potts, M., Pshirkov, M. S., Remington, J., Rodriguez, D. C., Rubtsov, G. I., Ryu, D., Sagawa, H., Sahara, R., Saito, Y., Sakaki, N., Sako, T., Sakurai, N., Sano, K., Sato, K., Seki, T., Sekino, K., Shah, P. D., Shibasaki, Y., Shibata, F., Shibata, N., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Shinto, D., Smith, J. D., Sokolsky, P., Sone, N., Stokes, B. T., Stroman, T. A., Takagi, Y., Takahashi, Y., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Tanoue, Y., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsuda, R., Tsunesada, Y., Uchihori, Y., Udo, S., Uehama, T., Urban, F., Warren, D., Wong, T., Yamamoto, M., Yamazaki, K., Yashiro, K., Yoshida, F., Yoshioka, Y., Zhezher, Y., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: For several decades, the origin of ultra-high-energy cosmic rays (UHECRs) has been an unsolved question of high-energy astrophysics. One approach for solving this puzzle is to correlate UHECRs with high-energy neutrinos, since neutrinos are a direct probe of hadronic interactions of cosmic rays and are not deflected by magnetic fields. In this paper, we present three different approaches for correlating the arrival directions of neutrinos with the arrival directions of UHECRs. The neutrino data is provided by the IceCube Neutrino Observatory and ANTARES, while the UHECR data with energies above $\sim$50 EeV is provided by the Pierre Auger Observatory and the Telescope Array. All experiments provide increased statistics and improved reconstructions with respect to our previous results reported in 2015. The first analysis uses a high-statistics neutrino sample optimized for point-source searches to search for excesses of neutrinos clustering in the vicinity of UHECR directions. The second analysis searches for an excess of UHECRs in the direction of the highest-energy neutrinos. The third analysis searches for an excess of pairs of UHECRs and highest-energy neutrinos on different angular scales. None of the analyses has found a significant excess, and previously reported over-fluctuations are reduced in significance. Based on these results, we further constrain the neutrino flux spatially correlated with UHECRs., Comment: 39 pages, 7 figures, 4 tables; updated source files including xml authorlist
Published: 2022
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9. Observation of Variations in Cosmic Ray Single Count Rates During Thunderstorms and Implications for Large-Scale Electric Field Changes

Author: Abbasi, R. U., Abu-Zayyad, T., Allen, M., Arai, Y., Arimura, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Buckland, I., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., Fujii, T., Fujisue, K., Fujita, K., Fujiwara, R., Fukushima, M., Fukushima, R., Furlich, G., Globus, N., Gonzalez, R., Hanlon, W., Hayashi, M., Hayashida, N., Hibino, K., Higuchi, R., Honda, K., Husseini, N., Ikeda, D., Inadomi, T., Inoue, N., Ishii, T., Ito, H., Ivanov, D., Iwakura, H., Iwasaki, A., Jeong, H. M., Jeong, S., Johnson, H., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kasami, S., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kharuk, I., Kido, E., Kim, H. B., Kim, J. H., Kim, M. H., Kim, S. W., Kimura, Y., Kishigami, S., Kubota, Y., Kurisu, S., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lee, K. H., LeVon, R., Lubsandorzhiev, B., Lundquist, J. P., Machida, K., Matsumiya, H., Matsuyama, T., Matthews, J. N., Mayta, R., Mazich, J., Minamino, M., Mukai, K., Myers, I., Myers, P., Nagataki, S., Nakai, K., Nakamura, R., Nakamura, T., Nakamura, Y., Nakazawa, A., Nishio, E., Nonaka, T., OBrien, K., Oda, H., Ogio, S., Ohnishi, M., Ohoka, H., Oku, Y., Okuda, T., Omura, Y., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Potts, M., Pshirkov, M. S., Remington, J., Rodriguez, D. C., Rubtsov, G. I., Ryu, D., Sagawa, H., Sahara, R., Saito, Y., Sakaki, N., Sako, T., Sakurai, N., Sano, K., Sato, K., Seki, T., Sekino, K., Shah, P. D., Shibasaki, Y., Shibata, F., Shibata, N., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Shinto, D., Smith, J. D., Sokolsky, P., Sone, N., Stokes, B. T., Stroman, T. A., Takagi, Y., Takahashi, Y., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Tanoue, Y., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsuda, R., Tsunesada, Y., Uchihori, Y., Udo, S., Uehama, T., Urban, F., Wong, T., Yamamoto, M., Yamazaki, K., Yang, J., Yashiro, K., Yoshida, F., Yoshioka, Y., Zhezher, Y., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment, Physics - Atmospheric and Oceanic Physics
Abstract: We present the first observation by the Telescope Array Surface Detector (TASD) of the effect of thunderstorms on the development of cosmic ray single count rate intensity over a 700 km$^{2}$ area. Observations of variations in the secondary low-energy cosmic ray counting rate, using the TASD, allow us to study the electric field inside thunderstorms, on a large scale, as it progresses on top of the 700 km$^{2}$ detector, without dealing with the limitation of narrow exposure in time and space using balloons and aircraft detectors. In this work, variations in the cosmic ray intensity (single count rate) using the TASD, were studied and found to be on average at the $\sim(0.5-1)\%$ and up to 2\% level. These observations were found to be both in excess and in deficit. They were also found to be correlated with lightning in addition to thunderstorms. These variations lasted for tens of minutes; their footprint on the ground ranged from 6 to 24 km in diameter and moved in the same direction as the thunderstorm. With the use of simple electric field models inside the cloud and between cloud to ground, the observed variations in the cosmic ray single count rate were recreated using CORSIKA simulations. Depending on the electric field model used and the direction of the electric field in that model, the electric field magnitude that reproduces the observed low-energy cosmic ray single count rate variations was found to be approximately between 0.2-0.4 GV. This in turn allows us to get a reasonable insight on the electric field and its effect on cosmic ray air showers inside thunderstorms.
Published: 2021
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10. Indications of a Cosmic Ray Source in the Perseus-Pisces Supercluster

Author: Telescope Array Collaboration, Abbasi, R. U., Abu-Zayyad, T., Allen, M., Arai, Y., Arimura, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Buckland, I., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., Fujii, T., Fujisue, K., Fujita, K., Fujiwara, R., Fukushima, M., Fukushima, R., Furlich, G., Globus, N., Gonzalez, R., Hanlon, W., Hayashi, M., Hayashida, N., Hibino, K., Higuchi, R., Honda, K., Ikeda, D., Inadomi, T., Inoue, N., Ishii, T., Ito, H., Ivanov, D., Iwakura, H., Iwasaki, A., Jeong, H. M., Jeong, S., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kasami, S., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kharuk, I., Kido, E., Kim, H. B., Kim, J. H., Kim, M. H., Kim, S. W., Kimura, Y., Kishigami, S., Kubota, Y., Kurisu, S., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lee, K. H., Lubsandorzhiev, B., Lundquist, J. P., Machida, K., Matsumiya, H., Matsuyama, T., Matthews, J. N., Mayta, R., Minamino, M., Mukai, K., Myers, I., Nagataki, S., Nakai, K., Nakamura, R., Nakamura, T., Nakamura, Y., Nakazawa, A., Nishio, E., Nonaka, T., Oda, H., Ogio, S., Ohnishi, M., Ohoka, H., Oku, Y., Okuda, T., Omura, Y., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Potts, M., Pshirkov, M. S., Remington, J., Rodriguez, D. C., Rubtsov, G. I., Ryu, D., Sagawa, H., Sahara, R., Saito, Y., Sakaki, N., Sako, T., Sakurai, N., Sano, K., Sato, K., Seki, T., Sekino, K., Shah, P. D., Shibasaki, Y., Shibata, F., Shibata, N., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Shinto, D., Smith, J. D., Sokolsky, P., Sone, N., Stokes, B. T., Stroman, T. A., Takagi, Y., Takahashi, Y., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Tanoue, Y., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsuda, R., Tsunesada, Y., Uchihori, Y., Udo, S., Uehama, T., Urban, F., Wong, T., Yamamoto, M., Yamazaki, K., Yang, J., Yashiro, K., Yoshida, F., Yoshioka, Y., Zhezher, Y., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The Telescope Array Collaboration has observed an excess of events with $E \ge 10^{19.4} ~{\rm eV}$ in the data which is centered at (RA, dec) = ($19^\circ$, $35^\circ$). This is near the center of the Perseus-Pisces supercluster (PPSC). The PPSC is about $70 ~{\rm Mpc}$ distant and is the closest supercluster in the Northern Hemisphere (other than the Virgo supercluster of which we are a part). A Li-Ma oversampling analysis with $20^\circ$-radius circles indicates an excess in the arrival direction of events with a local significance of about 4 standard deviations. The probability of having such excess close to the PPSC by chance is estimated to be 3.5 standard deviations. This result indicates that a cosmic ray source likely exists in that supercluster., Comment: 8 pages, 4 figures, 1 table
Published: 2021

11. Detectability of southern gamma-ray sources beyond 100 TeV with ALPAQUITA, the prototype experiment of ALPACA

Author: Kato, S., Condori, C. A. H., Fuente, E. dela, Gomi, A., Hibino, K., Hotta, N., Toledano-Juarez, I., Katayose, Y., Kato, C., Kawata, K., Kihara, W., Ko, Y., Koi, T., Kojima, H., Kurashige, D., Lozoya, J., Orozco-Luna, F., Mayta, R., Miranda, P., Munakata, K., Nakada, H., Nakamura, Y., Nakazawa, Y., Nina, C., Nishizawa, M., Ogio, S., Ohnishi, M., Ohura, T., Okukawa, S., Oshima, A., Raljevich, M., Rivera, H., Saito, T., Sako, T., Sako, T. K., Shibata, S., Shiomi, A., Subieta, M., Tajima, N., Takano, W., Takita, M., Tameda, Y., Tanaka, K., Ticona, R., Torres, H., Tsuchiya, H., Tsunesada, Y., Udo, S., Yamazaki, K., and Yokoe, Y.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Andes Large-area PArticle detector for Cosmic-ray physics and Astronomy (ALPACA) is an international experiment that applies southern very-high-energy (VHE) gamma-ray astronomy to determine the origin of cosmic rays around the knee energy region ($10^{15}\, {\rm eV} - 10^{16}\, {\rm eV}$). The experiment consists of an air shower (AS) array with a surface of $83, 000\, {\rm m}^2$ and an underground water Cherenkov muon detector (MD) array covering $5, 400\, {\rm m}^2$. The experimental site is at the Mt. Chacaltaya plateau in La Paz, Bolivia, with an altitude of $4, 740\, {\rm m}$ corresponding to $572\, {\rm g}/{\rm cm}^2$ atmospheric thickness. As the prototype experiment of ALPACA, the ALPAQUITA experiment aims to begin data acquisition in late 2021. The ALPAQUITA array consists of a smaller AS array ($18, 450\, {\rm m}^2$) and underground MD ($900\, {\rm m}^2$), which are now under construction. ALPAQUITA's sensitivity to gamma-ray sources is evaluated with Monte Carlo simulations. The simulation finds that five gamma-ray sources observed by H.E.S.S. and HAWC experiments will be detected by ALPAQUITA beyond 10 TeV and one out of these five - HESS J1702-420A - above 300 TeV in one calendar year observation. The latter finding means that scientific discussions can be made on the emission mechanism of gamma rays beyond 100 TeV from southern sources on the basis of the observational results of this prototype experiment., Comment: This is the manuscript accepted by Experimental Astronomy. For the published article, see https://doi.org/10.1007/s10686-021-09796-8
Published: 2021
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12. Potential PeVatron supernova remnant G106.3+2.7 seen in the highest-energy gamma rays

Author: Amenomori, M., 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, Gou, Q. B., Guo, Y. Q., Guo, Y. Y., He, H. H., He, Z. T., Hibino, K., Hotta, N., Hu, Haibing, Hu, H. B., Huang, J., Jia, H. Y., Jiang, L., Jin, H. B., Kasahara, K., Katayose, Y., Kato, C., Kato, S., Kawata, K., Kihara, W., Ko, Y., Kozai, M., Labaciren, Le, G. M., Li, A. F., Li, H. J., Li, W. J., Lin, Y. H., Liu, B., Liu, C., Liu, J. S., Liu, M. Y., Liu, W., Lou, Y. -Q., Lu, H., Meng, X. R., Munakata, K., Nakada, H., Nakamura, Y., Nanjo, H., Nishizawa, M., Ohnishi, M., Ohura, T., Ozawa, S., Qian, X. L., Qu, X. B., Saito, T., Sakata, M., Sako, T. K., 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., Wu, H. R., Xue, L., Yamamoto, Y., Yang, Z., Yokoe, Y., 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, and Zhou, X. X.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Cosmic rays (protons and other atomic nuclei) are believed to gain energies of petaelectronvolts (PeV) and beyond at astrophysical particle accelerators called 'PeVatrons' inside our Galaxy. Although a characteristic feature of a PeVatron is expected to be a hard gamma-ray energy spectrum that extends beyond 100 teraelectronvolts (TeV) without a cutoff, none of the currently known sources exhibits such a spectrum due to the low maximum energy of accelerated cosmic rays or insufficient detector sensitivity around 100 TeV. Here we report the observation of gamma-ray emission from the supernova remnant G106.3+2.7 above 10 TeV. This work provides flux data points up to and above 100 TeV and indicates that the very-high-energy gamma-ray emission above 10 TeV is well correlated with a molecular cloud rather than the pulsar PSR J2229+6114. Regarding the gamma-ray emission mechanism of G106.3+2.7, this morphological feature appears to favor a hadronic origin via the {\pi}0 decay caused by accelerated relativistic protons over a leptonic one via the inverse-Compton scattering by relativistic electrons. Furthermore, we point out that an X-ray flux upper limit on the synchrotron spectrum would provide important information to firmly establish the hadronic scenario as the mechanism of particle acceleration at the source., Comment: Published in Nature Astronomy
Published: 2021
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13. Gamma-ray Observation of the Cygnus Region in the 100 TeV Energy Region

Author: Amenomori, M., 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., He, H. H., He, Z. T., Hibino, K., Hotta, N., Hu, Haibing, Hu, H. B., Huang, J., Jia, H. Y., Jiang, L., Jiang, P., Jin, H. B., Kasahara, K., Katayose, Y., Kato, C., Kato, S., 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., Liu, X. L., Lou, Y. -Q., Lu, H., Meng, X. R., Munakata, K., Nakada, H., Nakamura, Y., Nakazawa, Y., Nanjo, H., Ning, C. C., Nishizawa, M., Ohnishi, M., Ohura, T., Okukawa, S., Ozawa, S., Qian, L., Qian, X., Qian, X. L., Qu, X. B., Saito, T., Sakata, M., Sako, T., Sako, T. K., 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, Y. P., Wangdui, Wu, H. R., Wu, Q., Xu, J. L., Xue, L., Yamamoto, Y., Yang, Z., Yao, Y. Q., Yin, J., Yokoe, Y., Yu, N. P., Yuan, A. F., Zhai, L. M., Zhang, C. P., Zhang, H. M., Zhang, J. L., Zhang, X., Zhang, X. Y., Zhang, Y., Zhang, Yi, Zhang, Ying, Zhao, S. P., Zhaxisangzhu, and Zhou, X. X.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report observations of gamma-ray emissions with energies in the 100 TeV energy region from the Cygnus region in our Galaxy. Two sources are significantly detected in the directions of the Cygnus OB1 and OB2 associations. Based on their positional coincidences, we associate one with a pulsar PSR J2032+4127 and the other mainly with a pulsar wind nebula PWN G75.2+0.1 with the pulsar moving away from its original birthplace situated around the centroid of the observed gamma-ray emission. This work would stimulate further studies of particle acceleration mechanisms at these gamma-ray sources., Comment: Accepted for publication in the Physical Review Letters
Published: 2021
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14. First Detection of sub-PeV Diffuse Gamma Rays from the Galactic Disk: Evidence for Ubiquitous Galactic Cosmic Rays beyond PeV Energies

Author: Amenomori, M., 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, Gou, Q. B., Guo, Y. Q., Guo, Y. Y., He, H. H., He, Z. T., Hibino, K., Hotta, N., Hu, Haibing, Hu, H. B., Huang, J., Jia, H. Y., Jiang, L., Jin, H. B., Kasahara, K., Katayose, Y., Kato, C., Kato, S., Kawata, K., Kihara, W., Ko, Y., Kozai, M., Labaciren, Le, G. M., Li, A. F., Li, H. J., Li, W. J., Lin, Y. H., Liu, B., Liu, C., Liu, J. S., Liu, M. Y., Liu, W., Lou, Y. -Q., Lu, H., Meng, X. R., Munakata, K., Nakada, H., Nakamura, Y., Nanjo, H., Nishizawa, M., Ohnishi, M., Ohura, T., Ozawa, S., Qian, X. L., Qu, X. B., Saito, T., Sakata, M., Sako, T. K., 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., Wu, H. R., Xue, L., Yamamoto, Y., Yang, Z., Yokoe, Y., 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, and Zhou, X. X.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report, for the first time, the long-awaited detection of diffuse gamma rays with energies between 100 TeV and 1 PeV in the Galactic disk. Particularly, all gamma rays above 398 TeV are observed apart from known TeV gamma-ray sources and compatible with expectations from the hadronic emission scenario in which gamma rays originate from the decay of $\pi^0$'s produced through the interaction of protons with the interstellar medium in the Galaxy. This is strong evidence that cosmic rays are accelerated beyond PeV energies in our Galaxy and spread over the Galactic disk., Comment: Accepted for publication in the Physical Review Letters
Published: 2021
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15. Surface detectors of the TAx4 experiment

Author: Telescope Array Collaboration, Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Arai, Y., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., Fujii, T., Fujisue, K., Fujita, K., Fujiwara, R., Fukushima, M., Fukushima, R., Furlich, G., Hanlon, W., Hayashi, M., Hayashida, N., Hibino, K., Higuchi, R., Honda, K., Ikeda, D., Inadomi, T., Inoue, N., Ishii, T., Ito, H., Ivanov, D., Iwakura, H., Jeong, H. M., Jeong, S., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kasami, S., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kim, M. H., Kim, S. W., Kimura, Y., Kishigami, S., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lee, K. H., Lubsandorzhiev, B., Lundquist, J. P., Machida, K., Matsumiya, H., Matsuyama, T., Matthews, J. N., Mayta, R., Minamino, M., Mukai, K., Myers, I., Nagataki, S., Nakai, K., Nakamura, R., Nakamura, T., Nakamura, Y., Nonaka, T., Oda, H., Ogio, S., Ohnishi, M., Ohoka, H., Oku, Y., Okuda, T., Omura, Y., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Remington, J., Rodriguez, D. C., Rubtsov, G. I., Ryu, D., Sagawa, H., Sahara, R., Saito, Y., Sakaki, N., Sako, T., Sakurai, N., Sano, K., Sato, K., Seki, T., Sekino, K., Shah, P. D., Shibata, F., Shibata, N., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Shinto, D., Smith, J. D., Sokolsky, P., Sone, N., Stokes, B. T., Stroman, T. A., Suzawa, T., Takagi, Y., Takahashi, Y., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Tanoue, Y., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsuda, R., Tsunesada, Y., Uchihori, Y., Udo, S., Uehama, T., Urban, F., Wong, T., Yada, K., Yamamoto, M., Yamazaki, K., Yang, J., Yashiro, K., Yoshida, F., Zhezher, Y., and Zundel, Z.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Instrumentation and Detectors
Abstract: Telescope Array (TA) is the largest ultrahigh energy cosmic-ray (UHECR) observatory in the Northern Hemisphere. It explores the origin of UHECRs by measuring their energy spectrum, arrival-direction distribution, and mass composition using a surface detector (SD) array covering approximately 700 km$^2$ and fluorescence detector (FD) stations. TA has found evidence for a cluster of cosmic rays with energies greater than 57 EeV. In order to confirm this evidence with more data, it is necessary to increase the data collection rate.We have begun building an expansion of TA that we call TAx4. In this paper, we explain the motivation, design, technical features, and expected performance of the TAx4 SD. We also present TAx4's current status and examples of the data that have already been collected., Comment: 26 pages, 17 figures, submitted to Nuclear Inst. and Methods in Physics Research, A
Published: 2021
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16. Hadronic interaction model dependence in cosmic Gamma-ray flux estimation using an extensive air shower array with a muon detector

Author: Okukawa, S., Anzorena, M., Asano, S., Condori, C. A. H., de la Fuente, E., Gomi, A., Hibino, K., Hotta, N., Jimenez-Meza, A., Katayose, Y., Kato, C., Kato, S., Kawashima, T., Kawata, K., Koi, T., Kojima, H., Kurashige, D., Lozoya, J., Mayta, R., Miranda, P., Munakata, K., Nagaya, K., Nakamura, Y., Nakazawa, Y., Nina, C., Nishizawa, M., Ogio, S., Ohnishi, M., Oshima, A., Raljevic, M., Rivera, H., Saito, T., Sakakibara, Y., Sako, T., Sako, T. K., Shibata, S., Shiomi, A., Subieta, M., Tajima, N., Takano, W., Takita, M., Tameda, Y., Tanaka, K., Ticona, R., Toledano-Juarez, I., Tsuchiya, H., Tsunesada, Y., Udo, S., Yamazaki, K., and Yokoe, Y.
Published: 2023
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17. Observations of the Origin of Downward Terrestrial Gamma-Ray Flashes

Author: Belz, J. W., Krehbiel, P. R., Remington, J., Stanley, M. A., Abbasi, R. U., LeVon, R., Rison, W., Rodeheffer, D., Collaboration, the Telescope Array Scientific, Abu-Zayyad, T., Allen, M., Barcikowski, E., Bergman, D. R., Blake, S. A., Byrne, M., Cady, R., Cheon, B. G., Chikawa, M., di Matteo, A., Fujii, T., Fujita, K., Fujiwara, R., Fukushima, M., Furlich, G., Hanlon, W., Hayashi, M., Hayashi, Y., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inadomi, T., Inoue, N., Ishii, T., Ito, H., Ivanov, D., Iwakura, H., Jeong, H. M., Jeong, S., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kasami, S., Kawai, H., Kawakami, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lee, K. H., Lubsandorzhiev, B., Lundquist, J. P., Machida, K., Matsumiya, H., Matthews, J. N., Matuyama, T., Mayta, R., Minamino, M., Mukai, K., Myers, I., Nagataki, S., Nakai, K., Nakamura, R., Nakamura, T., Nakamura, Y., Nonaka, T., Oda, H., Ogio, S., Ohnishi, M., Ohoka, H., Oku, Y., Okuda, T., Omura, Y., Ono, M., Oshima, A., Ozawa, S., Park, I. H., Potts, M., Pshirkov, M. S., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sahara, R., Saito, K., Saito, Y., Sakaki, N., Sako, T., Sakurai, N., Sano, K., Seki, T., Sekino, K., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Smith, J. D., Sokolsky, P., Sone, N., Stokes, B. T., Stroman, T. A., Takagi, Y., Takahashi, Y., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, K., Tanaka, M., Tanoue, Y., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Uchihori, Y., Udo, S., Uehama, T., Urban, F., Wallace, M., Wong, T., Yamamoto, M., Yamaoka, H., Yamazaki, K., Yashiro, K., Yosei, M., Yoshii, H., Zhezher, Y., and Zundel, Z.
Subjects: Physics - Atmospheric and Oceanic Physics, Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract: In this paper we report the first close, high-resolution observations of downward-directed terrestrial gamma-ray flashes (TGFs) detected by the large-area Telescope Array cosmic ray observatory, obtained in conjunction with broadband VHF interferometer and fast electric field change measurements of the parent discharge. The results show that the TGFs occur during strong initial breakdown pulses (IBPs) in the first few milliseconds of negative cloud-to-ground and low-altitude intracloud flashes, and that the IBPs are produced by a newly-identified streamer-based discharge process called fast negative breakdown. The observations indicate the relativistic runaway electron avalanches (RREAs) responsible for producing the TGFs are initiated by embedded spark-like transient conducting events (TCEs) within the fast streamer system, and potentially also by individual fast streamers themselves. The TCEs are inferred to be the cause of impulsive sub-pulses that are characteristic features of classic IBP sferics. Additional development of the avalanches would be facilitated by the enhanced electric field ahead of the advancing front of the fast negative breakdown. In addition to showing the nature of IBPs and their enigmatic sub-pulses, the observations also provide a possible explanation for the unsolved question of how the streamer to leader transition occurs during the initial negative breakdown, namely as a result of strong currents flowing in the final stage of successive IBPs, extending backward through both the IBP itself and the negative streamer breakdown preceding the IBP., Comment: Typo fixed and reference added. Manuscript is 36 pages. Supplemental Information is 42 pages. This paper is to be published in the Journal of Geophysical Research: Atmospheres. Online data repository: Open Science Framework DOI: 10.17605/OSF.IO/Z3XDA
Published: 2020
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18. Search for Large-scale Anisotropy on Arrival Directions of Ultra-high-energy Cosmic Rays Observed with the Telescope Array Experiment

Author: Telescope Array Collaboration, Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., di Matteo, A., Fujii, T., Fujisue, K., Fujita, K., Fujiwara, R., Fukushima, M., Furlich, G., Hanlon, W., Hayashi, M., Hayashida, N., Hibino, K., Higuchi, R., Honda, K., Ikeda, D., Inadomi, T., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Iwakura, H., Jeong, H. M., Jeong, S., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kasami, S., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kim, M. H., Kim, S. W., Kishigami, S., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lee, K. H., Lubsandorzhiev, B., Lundquist, J. P., Machida, K., Matsumiya, H., Matsuyama, T., Matthews, J. N., Mayta, R., Minamino, M., Mukai, K., Myers, I., Nagataki, S., Nakai, K., Nakamura, R., Nakamura, T., Nakamura, Y., Nonaka, T., Oda, H., Ogio, S., Ohnishi, M., Ohoka, H., Oku, Y., Okuda, T., Omura, Y., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Remington, J., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sahara, R., Saito, Y., Sakaki, N., Sako, T., Sakurai, N., Sano, K., Seki, T., Sekino, K., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Smith, J. D., Sokolsky, P., Sone, N., Stokes, B. T., Stroman, T. A., Suzawa, T., Takagi, Y., Takahashi, Y., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Tanoue, Y., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Uchihori, Y., Udo, S., Uehama, T., Urban, F., Wong, T., Yada, K., Yamamoto, M., Yamazaki, K., Yang, J., Yashiro, K., Yosei, M., Zhezher, Y., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Motivated by the detection of a significant dipole structure in the arrival directions of ultrahigh-energy cosmic rays above 8 EeV reported by the Pierre Auger Observatory (Auger), we search for a large-scale anisotropy using data collected with the surface detector array of the Telescope Array Experiment (TA). With 11 years of TA data, a dipole structure in a projection of the right ascension is fitted with an amplitude of 3.3+- 1.9% and a phase of 131 +- 33 degrees. The corresponding 99% confidence-level upper limit on the amplitude is 7.3%. At the current level of statistics, the fitted result is compatible with both an isotropic distribution and the dipole structure reported by Auger., Comment: 6 pages, 3 figures, 1 table, Proofed title. Added journal reference and DOI
Published: 2020
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19. Measurement of the Proton-Air Cross Section with Telescope Array's Black Rock Mesa and Long Ridge Fluorescence Detectors, and Surface Array in Hybrid Mode

Author: Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., di Matteo, A., Fujii, T., Fujisue, K., Fujita, K., Fujiwara, R., Fukushima, M., Furlich, G., Hanlon, W., Hayashi, M., Hayashida, N., Hibino, K., Higuchi, R., Honda, K., Ikeda, D., Inadomi, T., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Iwakura, H., Jeong, H. M., Jeong, S., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kasami, S., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kim, M. H., Kim, S. W., Kishigami, S., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lee, K. H., Lubsandorzhiev, B., Lundquist, J. P., Machida, K., Matsumiya, H., Matsuyama, T., Matthews, J. N., Mayta, R., Minamino, M., Mukai, K., Myers, I., Nagataki, S., Nakai, K., Nakamura, R., Nakamura, T., Nakamura, Y., Nonaka, T., Oda, H., Ogio, S., Ohnishi, M., Ohoka, H., Oku, Y., Okuda, T., Omura, Y., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Remington, J., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sahara, R., Saito, Y., Sakaki, N., Sako, T., Sakurai, N., Sano, K., Seki, T., Sekino, K., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Smith, J. D., Sokolsky, P., Sone, N., Stokes, B. T., Stroman, T. A., Suzawa, T., Takagi, Y., Takahashi, Y., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Tanoue, Y., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Uchihori, Y., Udo, S., Uehama, T., Urban, F., Wong, T., Yada, K., Yamamoto, M., Yamazaki, K., Yang, J., Yashiro, K., Yosei, M., Zhezher, Y., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Ultra high energy cosmic rays provide the highest known energy source in the universe to measure proton cross sections. Though conditions for collecting such data are less controlled than an accelerator environment, current generation cosmic ray observatories have large enough exposures to collect significant statistics for a reliable measurement for energies above what can be attained in the lab. Cosmic ray measurements of cross section use atmospheric calorimetry to measure depth of air shower maximum ($X_{\mathrm{max}}$), which is related to the primary particle's energy and mass. The tail of the $X_{\mathrm{max}}$ distribution is assumed to be dominated by showers generated by protons, allowing measurement of the inelastic proton-air cross section. In this work the proton-air inelastic cross section measurement, $\sigma^{\mathrm{inel}}_{\mathrm{p-air}}$, using data observed by Telescope Array's Black Rock Mesa and Long Ridge fluorescence detectors and surface detector array in hybrid mode is presented. $\sigma^{\mathrm{inel}}_{\mathrm{p-air}}$ is observed to be $520.1 \pm 35.8$[Stat.] $^{+25.0}_{-40}$[Sys.]~mb at $\sqrt{s} = 73$ TeV. The total proton-proton cross section is subsequently inferred from Glauber formalism and is found to be $\sigma^{\mathrm{tot}}_{\mathrm{pp}} = 139.4 ^{+23.4}_{-21.3}$ [Stat.]$ ^{+15.0}_{-24.0}$[Sys.]~mb.
Published: 2020
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20. Evidence for a Supergalactic Structure of Magnetic Deflection Multiplets of Ultra-High Energy Cosmic Rays

Author: Telescope Array Collaboration, Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., di Matteo, A., Fujii, T., Fujisue, K., Fujita, K., Fujiwara, R., Fukushima, M., Furlich, G., Hanlon, W., Hayashi, M., Hayashida, N., Hibino, K., Higuchi, R., Honda, K., Ikeda, D., Inadomi, T., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Iwakura, H., Jeong, H. M., Jeong, S., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kasami, S., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kim, M. H., Kim, S. W., Kishigami, S., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lee, K. H., Lubsandorzhiev, B., Lundquist, J. P., Machida, K., Matsumiya, H., Matsuyama, T., Matthews, J. N., Mayta, R., Minamino, M., Mukai, K., Myers, I., Nagataki, S., Nakai, K., Nakamura, R., Nakamura, T., Nakamura, Y., Nonaka, T., Oda, H., Ogio, S., Ohnishi, M., Ohoka, H., Oku, Y., Okuda, T., Omura, Y., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Remington, J., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sahara, R., Saito, Y., Sakaki, N., Sako, T., Sakurai, N., Sano, K., Seki, T., Sekino, K., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Smith, J. D., Sokolsky, P., Sone, N., Stokes, B. T., Stroman, T. A., Suzawa, T., Takagi, Y., Takahashi, Y., Takamura, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Tanoue, Y., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Uchihori, Y., Udo, S., Uehama, T., Urban, F., Wong, T., Yada, K., Yamamoto, M., Yamazaki, K., Yang, J., Yashiro, K., Yosei, M., Zhezher, Y., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Evidence for a large-scale supergalactic cosmic ray multiplet (arrival directions correlated with energy) structure is reported for ultra-high energy cosmic ray (UHECR) energies above 10$^{19}$ eV using seven years of data from the Telescope Array (TA) surface detector and updated to 10 years. Previous energy-position correlation studies have made assumptions regarding magnetic field shapes and strength, and UHECR composition. Here the assumption tested is that, since the supergalactic plane is a fit to the average matter density of the local Large Scale Structure (LSS), UHECR sources and intervening extragalactic magnetic fields are correlated with this plane. This supergalactic deflection hypothesis is tested by the entire field-of-view (FOV) behavior of the strength of intermediate-scale energy-angle correlations. These multiplets are measured in spherical cap section bins (wedges) of the FOV to account for coherent and random magnetic fields. The structure found is consistent with supergalactic deflection, the previously published energy spectrum anisotropy results of TA (the hotspot and coldspot), and toy-model simulations of a supergalactic magnetic sheet. The seven year data post-trial significance of this supergalactic structure of multiplets appearing by chance, on an isotropic sky, is found by Monte Carlo simulation to be 4.2$\sigma$. The ten years of data post-trial significance is 4.1$\sigma$. Furthermore, the starburst galaxy M82 is shown to be a possible source of the TA Hotspot, and an estimate of the supergalactic magnetic field using UHECR measurements is presented.
Published: 2020

21. First Detection of Photons with Energy Beyond 100 TeV from an Astrophysical Source

Author: Amenomori, M., 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, Gou, Q. B., Guo, Y. Q., He, H. H., He, Z. T., Hibino, K., Hotta, N., Hu, Haibing, Hu, H. B., Huang, J., Jia, H. Y., Jiang, L., Jin, H. B., Kajino, F., Kasahara, K., Katayose, Y., Kato, C., Kato, S., Kawata, K., Kozai, M., Labaciren, Le, G. M., Li, A. F., Li, H. J., Li, W. J., Lin, Y. H., Liu, B., Liu, C., Liu, J. S., Liu, M. Y., Lou, Y. -Q., Lu, H., Meng, X. R., Mitsui, H., Munakata, K., Nakamura, Y., Nanjo, H., Nishizawa, M., Ohnishi, M., Ohta, I., Ozawa, S., Qian, X. L., Qu, X. B., Saito, T., Sakata, M., Sako, T. K., Sengoku, Y., Shao, J., Shibata, M., Shiomi, A., Sugimoto, H., Takita, M., Tan, Y. H., Tateyama, N., Torii, S., Tsuchiya, H., Udo, S., Wang, H., Wu, H. R., Xue, L., Yagisawa, K., Yamamoto, Y., Yang, Z., Yuan, A. F., Zhai, L. M., Zhang, H. M., Zhang, J. L., Zhang, X., Zhang, X. Y., Zhang, Y., Zhang, Yi, Zhang, Ying, Zhaxisangzhu, and Zhou, X. X.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: 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 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 photon-like events with $E>100$ TeV against 5.5 background events, which corresponds to 5.6$\sigma$ statistical significance. This is the first detection of photons with $E>100$ TeV from an astrophysical source., Comment: April 4, 2019; Submitted to the Physical Review Letters
Published: 2019
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22. Search for Ultra-High-Energy Neutrinos with the Telescope Array Surface Detector

Author: Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., di Matteo, A., Fujii, T., Fujisue, K., Fujita, K., Fujiwara, R., Fukushima, M., Furlich, G., Hanlon, W., Hayashi, M., Hayashi, Y., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ito, H., Ivanov, D., Jeong, H. M., Jeong, S., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kishigami, S., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lee, K. H., Lubsandorzhiev, B., Lundquist, J. P., Machida, K., Martens, K., Matsuyama, T., Matthews, J. N., Mayta, R., Minamino, M., Mukai, K., Myers, I., Nagasawa, K., Nagataki, S., Nakai, K., Nakamura, R., Nakamura, T., Nonaka, T., Oda, H., Ogio, S., Ohnishi, M., Ohoka, H., Okuda, T., Omura, Y., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Remington, J., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sahara, R., Saito, K., Saito, Y., Sakaki, N., Sako, T., Sakurai, N., Scott, L. M., Seki, T., Sekino, K., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Smith, J. D., Sokolsky, P., Stokes, B. T., Stratton, S. R., Stroman, T. A., Suzawa, T., Takagi, Y., Takahashi, Y., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Tanoue, Y., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Uchihori, Y., Udo, S., Urban, F., Wong, T., Yada, K., Yamamoto, M., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoshii, H., Zhezher, Y., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present an upper limit on the flux of ultra-high-energy down-going neutrinos for $E > 10^{18}\ \mbox{eV}$ derived with the nine years of data collected by the Telescope Array surface detector (05-11-2008 -- 05-10-2017). The method is based on the multivariate analysis technique, so-called Boosted Decision Trees (BDT). Proton-neutrino classifier is built upon 16 observables related to both the properties of the shower front and the lateral distribution function., Comment: 10 pages, 4 figures, accepted to JETP
Published: 2019
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23. Search for point sources of ultra-high energy photons with the Telescope Array surface detector

Author: Telescope Array Collaboration, Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., diMatteo, A., Fujii, T., Fujita, K., Fujiwara, R., Fukushima, M., Furlich, G., Hanlon, W., Hayashi, M., Hayashi, Y., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Jeong, H. M., Jeong, S., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kishigami, S., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lee, K. H., Lubsandorzhiev, B., Lundquist, J. P., Machida, K., Martens, K., Matsuyama, T., Matthews, J. N., Mayta, R., Minamino, M., Mukai, K., Myers, I., Nagataki, S., Nakai, K., Nakamura, R., Nakamura, T., Nonaka, T., Oda, H., Ogio, S., Ohnishi, M., Ohoka, H., Okuda, T., Omura, Y., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Remington, J., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sahara, R., Saito, K., Saito, Y., Sakaki, N., Sako, T., Sakurai, N., Scott, L. M., Seki, T., Sekino, K., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Smith, J. D., Sokolsky, P., Stokes, B. T., Stratton, S. R., Stroman, T. A., Suzawa, T., Takagi, Y., Takahashi, Y., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Tanoue, Y., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Tsutsumi, K., Uchihori, Y., Udo, S., Urban, F., Wong, T., Yada, K., Yamamoto, M., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoshii, H., Zhezher, Y., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The surface detector (SD) of the Telescope Array (TA) experiment allows one to indirectly detect photons with energies of order $10^{18}$ eV and higher and to separate photons from the cosmic-ray background. In this paper we present the results of a blind search for point sources of ultra-high energy (UHE) photons in the Northern sky using the TA SD data. The photon-induced extensive air showers (EAS) are separated from the hadron-induced EAS background by means of a multivariate classifier based upon 16 parameters that characterize the air shower events. No significant evidence for the photon point sources is found. The upper limits are set on the flux of photons from each particular direction in the sky within the TA field of view, according to the experiment's angular resolution for photons. Average 95% C.L. upper limits for the point-source flux of photons with energies greater than $10^{18}$, $10^{18.5}$, $10^{19}$, $10^{19.5}$ and $10^{20}$ eV are $0.094$, $0.029$, $0.010$, $0.0073$ and $0.0058$ km$^{-2}$yr$^{-1}$ respectively. For the energies higher than $10^{18.5}$ eV, the photon point-source limits are set for the first time. Numerical results for each given direction in each energy range are provided as a supplement to this paper., Comment: accepted to MNRAS, 11 pages, 4 figures, 2 tables; results in text-file format are supplemented to paper source
Published: 2019
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24. Study of water Cherenkov detector to improve the angular resolution of an air-shower array for ultra-high-energy gamma-ray observation

Author: Nakada, H., Shiomi, A., Ohnishi, M., Sako, T. K., Hibino, K., and Katayose, Y.
Published: 2022
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25. Constraints on the diffuse photon flux with energies above $10^{18}$ eV using the surface detector of the Telescope Array experiment

Author: Telescope Array Collaboration, Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., di Matteo, A., Fujii, T., Fujita, K., Fukushima, M., Furlich, G., Goto, T., Hanlon, W., Hayashi, M., Hayashi, Y., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Jeong, H. M., Jeong, S., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kishigami, S., Kitamura, S., Kitamura, Y., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lee, K. H., Lubsandorzhiev, B., Lundquist, J. P., Machida, K., Martens, K., Matsuyama, T., Matthews, J. N., Mayta, R., Minamino, M., Mukai, K., Myers, I., Nagasawa, K., Nagataki, S., Nakamura, R., Nakamura, T., Nonaka, T., Oda, H., Ogio, S., Ogura, J., Ohnishi, M., Ohoka, H., Okuda, T., Omura, Y., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Piskunov, M. S., Pshirkov, M. S., Remington, J., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sahara, R., Saito, K., Saito, Y., Sakaki, N., Sakurai, N., Scott, L. M., Seki, T., Sekino, K., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Smith, J. D., Sokolsky, P., Stokes, B. T., Stratton, S. R., Stroman, T. A., Suzawa, T., Takagi, Y., Takahashi, Y., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Tsutsumi, K., Uchihori, Y., Udo, S., Urban, F., Wong, T., Yamamoto, M., Yamane, R., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoneda, Y., Yoshida, S., Yoshii, H., Zhezher, Y., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment, High Energy Physics - Phenomenology
Abstract: We present the results of the search for ultra-high-energy photons with nine years of data from the Telescope Array surface detector. A multivariate classifier is built upon 16 reconstructed parameters of the extensive air shower. These parameters are related to the curvature and the width of the shower front, the steepness of the lateral distribution function, and the timing parameters of the waveforms sensitive to the shower muon content. A total number of two photon candidates found in the search is fully compatible with the expected background. The $95\%\,$CL limits on the diffuse flux of the photons with energies greater than $10^{18.0}$, $10^{18.5}$, $10^{19.0}$, $10^{19.5}$ and $10^{20.0}$ eV are set at the level of $0.067$, $0.012$, $0.0036$, $0.0013$, $0.0013~\mbox{km}^{-2}\mbox{yr}^{-1}\mbox{sr}^{-1}$ correspondingly., Comment: 7 pages, 2 figures
Published: 2018
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26. Testing a reported correlation between arrival directions of ultrahigh-energy cosmic rays and a flux pattern from nearby starburst galaxies using Telescope Array data

Author: Telescope Array Collaboration, Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., di Matteo, A., Fujii, T., Fujita, K., Fukushima, M., Furlich, G., Goto, T., Hanlon, W., Hayashi, M., Hayashi, Y., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Jeong, H. M., Jeong, S., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kishigami, S., Kitamura, S., Kitamura, Y., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lee, K. H., Lubsandorzhiev, B., Lundquist, J. P., Machida, K., Martens, K., Matsuyama, T., Matthews, J. N., Mayta, R., Minamino, M., Mukai, K., Myers, I., Nagasawa, K., Nagataki, S., Nakamura, R., Nakamura, T., Nonaka, T., Oda, H., Ogio, S., Ogura, J., Ohnishi, M., Ohoka, H., Okuda, T., Omura, Y., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Remington, J., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sahara, R., Saito, K., Saito, Y., Sakaki, N., Sakurai, N., Scott, L. M., Seki, T., Sekino, K., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Smith, J. D., Sokolsky, P., Stokes, B. T., Stratton, S. R., Stroman, T. A., Suzawa, T., Takagi, Y., Takahashi, Y., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Tsutsumi, K., Uchihori, Y., Udo, S., Urban, F., Wong, T., Yamamoto, M., Yamane, R., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoneda, Y., Yoshida, S., Yoshii, H., Zhezher, Y., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The Pierre Auger Collaboration (Auger) recently reported a correlation between the arrival directions of cosmic rays with energies above 39 EeV and the flux pattern of 23 nearby starburst galaxies (SBGs). In this Letter, we tested the same hypothesis using cosmic rays detected by the Telescope Array experiment (TA) in the 9-year period from May 2008 to May 2017. Unlike the Auger analysis, we did not optimize the parameter values but kept them fixed to the best-fit values found by Auger, namely 9.7% for the anisotropic fraction of cosmic rays assumed to originate from the SBGs in the list and 12.9{\deg} for the angular scale of the correlations. The energy threshold we adopted is 43 EeV, corresponding to 39 EeV in Auger when taking into account the energy-scale difference between two experiments. We find that the TA data is compatible with isotropy to within 1.1{\sigma} and with the Auger result to within 1.4{\sigma}, meaning that it is not capable to discriminate between these two hypotheses., Comment: More accurate title, fixed an inconsistency in the declination range used, with a few figures slightly changing as a result, other minor revisions
Published: 2018
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27. Mass composition of ultra-high-energy cosmic rays with the Telescope Array Surface Detector Data

Author: Telescope Array Collaboration, Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., di Matteo, A., Fujii, T., Fujita, K., Fukushima, M., Furlich, G., Goto, T., Hanlon, W., Hayashi, M., Hayashi, Y., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Jeong, H. M., Jeong, S., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kishigami, S., Kitamura, S., Kitamura, Y., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lee, K. H., Lubsandorzhiev, B., Lundquist, J. P., Machida, K., Martens, K., Matsuyama, T., Matthews, J. N., Mayta, R., Minamino, M., Mukai, K., Myers, I., Nagasawa, K., Nagataki, S., Nakamura, R., Nakamura, T., Nonaka, T., Oda, H., Ogio, S., Ogura, J., Ohnishi, M., Ohoka, H., Okuda, T., Omura, Y., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Piskunov, M. S., Pshirkov, M. S., Remington, J., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sahara, R., Saito, K., Saito, Y., Sakaki, N., Sakurai, N., Scott, L. M., Seki, T., Sekino, K., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Smith, J. D., Sokolsky, P., Stokes, B. T., Stratton, S. R., Stroman, T. A., Suzawa, T., Takagi, Y., Takahashi, Y., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Tsutsumi, K., Uchihori, Y., Udo, S., Urban, F., Wong, T., Yamamoto, M., Yamane, R., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoneda, Y., Yoshida, S., Yoshii, H., Zhezher, Y., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The results on ultra-high-energy cosmic rays (UHECR) mass composition obtained with the Telescope Array surface detector are presented. The analysis employs the boosted decision tree (BDT) multivariate analysis built upon 14 observables related to both the properties of the shower front and the lateral distribution function. The multivariate classifier is trained with Monte-Carlo sets of events induced by the primary protons and iron. An average atomic mass of UHECR is presented for energies $10^{18.0}-10^{20.0}\ \mbox{eV}$. The average atomic mass of primary particles shows no significant energy dependence and corresponds to $\langle \ln A \rangle = 2.0 \pm 0.1 (stat.) \pm 0.44 (syst.)$. The result is compared to the mass composition obtained by the Telescope Array with $\mbox{X}_{\mbox{max}}$ technique along with the results of other experiments. Possible systematic errors of the method are discussed., Comment: 11 pages, 9 figures
Published: 2018
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28. Influence of Earth-Directed Coronal Mass Ejections on the Sun's Shadow Observed by the Tibet-III Air Shower Array

Author: Amenomori, M., Bi, X. J., Chen, D., Chen, T. L., Chen, W. Y., Cui, S. W., Danzengluobu, Ding, L. K., Feng, C. F., Feng, Zhaoyang, Feng, Z. Y., Gou, Q. B., Guo, Y. Q., He, H. H., He, Z. T., 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., Lu, H., Meng, X. R., Miyazaki, T., Munakata, K., Nakajima, T., Nakamura, Y., Nanjo, H., Nishizawa, M., Niwa, T., Ohnishi, M., Ohta, I., Ozawa, S., Qian, X. L., Qu, X. B., Saito, T., Saito, T. Y., Sakata, M., Sako, T. K., Shao, J., Shibata, M., Shiomi, A., Shirai, T., Sugimoto, H., Takita, M., Tan, Y. H., Tateyama, N., Torii, S., Tsuchiya, H., Udo, S., Wang, H., Wu, H. R., Xue, L., Yamamoto, Y., Yamauchi, K., Yang, Z., Yuan, S. A. F., Zhai, L. M., Zhang, H. M., Zhang, J. L., Zhang, X. Y., Zhang, Y., Zhang, Yi, Zhang, Ying, Zhaxisangzhu, and Zho, X. X.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We examine the possible influence of Earth-directed coronal mass ejections (ECMEs) on the Sun's shadow in the 3~TeV cosmic-ray intensity observed by the Tibet-III air shower (AS) array. We confirm a clear solar-cycle variation of the intensity deficit in the Sun's shadow during ten years between 2000 and 2009. This solar-cycle variation is overall reproduced by our Monte Carlo (MC) simulations of the Sun's shadow based on the potential field model of the solar magnetic field averaged over each solar rotation period. We find, however, that the magnitude of the observed intensity deficit in the Sun's shadow is significantly less than that predicted by MC simulations, particularly during the period around solar maximum when a significant number of ECMEs is recorded. The $\chi^2$ tests of the agreement between the observations and the MC simulations show that the difference is larger during the periods when the ECMEs occur, and the difference is reduced if the periods of ECMEs are excluded from the analysis. This suggests the first experimental evidence of the ECMEs affecting the Sun's shadow observed in the 3~TeV cosmic-ray intensity., Comment: 11 pages, 3 figures, accepted for publication in the ApJ
Published: 2018
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29. Study of muons from ultra-high energy cosmic ray air showers measured with the Telescope Array experiment

Author: Telescope Array Collaboration, Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., Di Matteo, A., Fujii, T., Fujita, K., Fukushima, M., Furlich, G., Goto, T., Hanlon, W., Hayashi, M., Hayashi, Y., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Jeong, H. M., Jeong, S. M., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kishigami, S., Kitamura, S., Kitamura, Y., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lee, K. H., Lubsandorzhiev, B., Lundquist, J. P., Machida, K., Martens, K., Matsuyama, T., Matthews, J. N., Mayta, R., Minamino, M., Mukai, K., Myers, I., Nagasawa, K., Nagataki, S., Nakamura, R., Nakamura, T., Nonaka, T., Oda, H., Ogio, S., Ogura, J., Ohnishi, M., Ohoka, H., Okuda, T., Omura, Y., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Remington, J., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sahara, R., Saito, K., Saito, Y., Sakaki, N., Sakurai, N., Scott, L. M., Seki, T., Sekino, K., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Smith, J. D., Sokolsky, P., Stokes, B. T., Stratton, S. R., Stroman, T. A., Suzawa, T., Takagi, Y., Takahashi, Y., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Tsutsumi, K., Uchihori, Y., Udo, S., Urban, F., Wong, T., Yamamoto, M., Yamane, R., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoneda, Y., Yoshida, S., Yoshii, H., Zhezher, Y., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: One of the uncertainties in interpretation of ultra-high energy cosmic ray (UHECR) data comes from the hadronic interaction models used for air shower Monte Carlo (MC) simulations. The number of muons observed at the ground from UHECR-induced air showers is expected to depend upon the hadronic interaction model. One may therefore test the hadronic interaction models by comparing the measured number of muons with the MC prediction. In this paper, we present the results of studies of muon densities in UHE extensive air showers obtained by analyzing the signal of surface detector stations which should have high $\it{muon \, purity}$. The muon purity of a station will depend on both the inclination of the shower and the relative position of the station. In 7 years' data from the Telescope Array experiment, we find that the number of particles observed for signals with an expected muon purity of $\sim$65% at a lateral distance of 2000 m from the shower core is $1.72 \pm 0.10{\rm (stat.)} \pm 0.37 {\rm (syst.)}$ times larger than the MC prediction value using the QGSJET II-03 model for proton-induced showers. A similar effect is also seen in comparisons with other hadronic models such as QGSJET II-04, which shows a $1.67 \pm 0.10 \pm 0.36$ excess. We also studied the dependence of these excesses on lateral distances and found a slower decrease of the lateral distribution of muons in the data as compared to the MC, causing larger discrepancy at larger lateral distances.
Published: 2018
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30. The Cosmic-Ray Energy Spectrum between 2 PeV and 2 EeV Observed with the TALE detector in monocular mode

Author: Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., Di Matteo, A., Fujii, T., Fujita, K., Fukushima, M., Furlich, G., Goto, T., Hanlon, W., Hayashi, M., Hayashi, Y., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Jeong, H. M., Jeong, S. M., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kishigami, S., Kitamura, S., Kitamura, Y., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lee, K. H., Lubsandorzhiev, B., Lundquist, J. P., Machida, K., Martens, K., Matsuyama, T., Matthews, J. N., Mayta, R., Minamino, M., Mukai, K., Myers, I., Nagasawa, K., Nagataki, S., Nakamura, R., Nakamura, T., Nonaka, T., Nozato, A., Oda, H., Ogio, S., Ogura, J., Ohnishi, M., Ohoka, H., Okuda, T., Omura, Y., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sahara, R., Saito, K., Saito, Y., Sakaki, N., Sakurai, N., Scott, L. M., Seki, T., Sekino, K., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Smith, J. D., Sokolsky, P., Stokes, B. T., Stratton, S. R., Stroman, T. A., Suzawa, T., Takagi, Y., Takahashi, Y., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Tsutsumi, K., Uchihori, Y., Udo, S., Urban, F., Wong, T., Yamamoto, M., Yamane, R., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoneda, Y., Yoshida, S., Yoshii, H., Zhezher, Y., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We report on a measurement of the cosmic ray energy spectrum by the Telescope Array Low-Energy Extension (TALE) air fluorescence detector. The TALE air fluorescence detector is also sensitive to the Cherenkov light produced by shower particles. Low energy cosmic rays, in the PeV energy range, are detectable by TALE as "Cherenkov Events". Using these events, we measure the energy spectrum from a low energy of $\sim 2$ PeV to an energy greater than 100 PeV. Above 100 PeV TALE can detect cosmic rays using air fluorescence. This allows for the extension of the measurement to energies greater than a few EeV. In this paper, we will describe the detector, explain the technique, and present results from a measurement of the spectrum using $\sim 1000$ hours of observation. The observed spectrum shows a clear steepening near $10^{17.1}$ eV, along with an ankle-like structure at $10^{16.2}$ eV. These features present important constraints on galactic cosmic rays origin and propagation models. The feature at $10^{17.1}$ eV may also mark the end of the galactic cosmic rays flux and the start of the transition to extra-galactic sources., Comment: 26 pages, 24 figures, submitted to ApJ
Published: 2018
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31. Evidence of Intermediate-Scale Energy Spectrum Anisotropy of Cosmic Rays E$\geq$10$^{19.2}$ eV with the Telescope Array Surface Detector

Author: Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., Di Matteo, A., Fujii, T., Fujita, K., Fukushima, M., Furlich, G., Goto, T., Hanlon, W., Hayashi, M., Hayashi, Y., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Jeong, H. M., Jeong, S. M., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kishigami, S., Kitamura, S., Kitamura, Y., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lee, K. H., Lubsandorzhiev, B., Lundquist, J. P., Machida, K., Martens, K., Matsuyama, T., Matthews, J. N., Mayta, R., Minamino, M., Mukai, K., Myers, I., Nagasawa, K., Nagataki, S., Nakamura, R., Nakamura, T., Nonaka, T., Nozato, A., Oda, H., Ogio, S., Ogura, J., Ohnishi, M., Ohoka, H., Okuda, T., Omura, Y., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sahara, R., Saito, K., Saito, Y., Sakaki, N., Sakurai, N., Scott, L. M., Seki, T., Sekino, K., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Smith, J. D., Sokolsky, P., Stokes, B. T., Stratton, S. R., Stroman, T. A., Suzawa, T., Takagi, Y., Takahashi, Y., Takamura, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Tsutsumi, K., Uchihori, Y., Udo, S., Urban, F., Wong, T., Yamamoto, M., Yamane, R., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoneda, Y., Yoshida, S., Yoshii, H., Zhezher, Y., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: An intermediate-scale energy spectrum anisotropy has been found in the arrival directions of ultra-high energy cosmic rays of energies above $10^{19.2}$ eV in the northern hemisphere, using 7 years of data from the Telescope Array surface detector. A relative energy distribution test is done comparing events inside oversampled spherical caps of equal exposure, to those outside, using the Poisson likelihood ratio. The center of maximum significance is at $9^h$$16^m$, $45^{\circ}$. and has a deficit of events with energies $10^{19.2}$$\leq$$E$$<$$10^{19.75}$ eV and an excess for $E$$\geq$$10^{19.75}$ eV. The post-trial probability of this energy anisotropy, appearing by chance anywhere on an isotropic sky, is found by Monte Carlo simulation to be $9$$\times$$10^{-5}$ ($3.74$$\sigma_{global}$).
Published: 2018
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32. Depth of Ultra High Energy Cosmic Ray Induced Air Shower Maxima Measured by the Telescope Array Black Rock and Long Ridge FADC Fluorescence Detectors and Surface Array in Hybrid Mode

Author: Telescope Array Collaboration, Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., Fujii, T., Fujita, K., Fukushima, M., Furlich, G., Goto, T., Hanlon, W., Hayashi, M., Hayashi, Y., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Jeong, S. M., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kishigami, S., Kitamura, S., Kitamura, Y., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lubsandorzhiev, B., Lundquist, J. P., Machida, M., Martens, K., Matsuyama, T., Matthews, J. N., Mayta, R., Minamino, M., Mukai, K., Myers, I., Nagasawa, K., Nagataki, S., Nakamura, R., Nakamura, T., Nonaka, T., Nozato, A., Oda, H., Ogio, S., Ogura, J., Ohnishi, M., Ohoka, H., Okuda, T., Omura, Y., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sahara, R., Saito, K., Saito, Y., Sakaki, N., Sakurai, N., Scott, L. M., Seki, T., Sekino, K., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Smith, J. D., Sokolsky, P., Stokes, B. T., Stratton, S. R., Stroman, T. A., Suzawa, T., Takagi, Y., Takahashi, Y., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Tsutsumi, K., Uchihori, Y., Udo, S., Urban, F., Wong, T., Yamamoto, M., Yamane, R., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoneda, Y., Yoshida, S., Yoshii, H., Zhezher, Y., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The Telescope Array observatory utilizes fluorescence detectors and surface detectors to observe air showers produced by ultra high energy cosmic rays in the Earth's atmosphere. Cosmic ray events observed in this way are termed hybrid data. The depth of air shower maximum is related to the mass of the primary particle that generates the shower. This paper reports on shower maxima data collected over 8.5 years using the Black Rock Mesa and Long Ridge fluorescence detectors in conjunction with the array of surface detectors. We compare the means and standard deviations of the observed $X_{\mathrm{max}}$ distributions with Monte Carlo $X_{\mathrm{max}}$ distributions of unmixed protons, helium, nitrogen, and iron, all generated using the QGSJet~II-04 hadronic model. We also perform an unbinned maximum likelihood test of the observed data, which is subjected to variable systematic shifting of the data $X_{\mathrm{max}}$ distributions to allow us to test the full distributions, and compare them to the Monte Carlo to see which elements are not compatible with the observed data. For all energy bins, QGSJet~II-04 protons are found to be compatible with Telescope Array hybrid data at the 95% confidence level after some systematic $X_{\mathrm{max}}$ shifting of the data. Three other QGSJet~II-04 elements are found to be compatible using the same test procedure in an energy range limited to the highest energies where data statistics are sparse., Comment: 39 pages, 18 figures, 5 tables, published in The Astrophysical Journal. This is a peer-reviewed, un-copyedited version of an article published in The Astrophysical Journal. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at https://doi.org/10.3847/1538-4357/aabad7
Published: 2018
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33. Evidence for Declination Dependence of the Ultrahigh Energy Cosmic Ray Spectrum in the Northern Hemisphere

Author: Abbasi, R. U., Abu-Zayyad, T., Allen, M., Arai, Y., Arimura, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Buckland, I., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., Fujii, T., Fujisue, K., Fujita, K., Fujiwara, R., Fukushima, M., Fukushima, R., Furlich, G., Globus, N., Gonzalez, R., Hanlon, W., Hayashi, M., Hayashida, N., Hibino, K., Higuchi, R., Honda, K., Ikeda, D., Inadomi, T., Inoue, N., Ishii, T., Ito, H., Ivanov, D., Iwakura, H., Iwasaki, A., Jeong, H. M., Jeong, S., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kasami, S., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kharuk, I., Kido, E., Kim, H. B., Kim, J. H., Kim, M. H., Kim, S. W., Kimura, Y., Kishigami, S., Kubota, Y., Kurisu, S., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lee, K. H., Lubsandorzhiev, B., Lundquist, J. P., Machida, K., Matsumiya, H., Matsuyama, T., Matthews, J. N., Mayta, R., Minamino, M., Mukai, K., Myers, I., Nagataki, S., Nakai, K., Nakamura, R., Nakamura, T., Nakamura, Y., Nakazawa, A., Nishio, E., Nonaka, T., Oda, H., Ogio, S., Ohnishi, M., Ohoka, H., Oku, Y., Okuda, T., Omura, Y., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Potts, M., Pshirkov, M. S., Remington, J., Rodriguez, D. C., Rubtsov, G. I., Ryu, D., Sagawa, H., Sahara, R., Saito, Y., Sakaki, N., Sako, T., Sakurai, N., Sano, K., Sato, K., Seki, T., Sekino, K., Shah, P. D., Shibasaki, Y., Shibata, F., Shibata, N., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Shinto, D., Smith, J. D., Sokolsky, P., Sone, N., Stokes, B. T., Stroman, T. A., Takagi, Y., Takahashi, Y., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Tanoue, Y., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsuda, R., Tsunesada, Y., Uchihori, Y., Udo, S., Uehama, T., Urban, F., Wong, T., Yamamoto, M., Yamazaki, K., Yang, J., Yashiro, K., Yoshida, F., Yoshioka, Y., Zhezher, Y., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Telescope Array (TA) is the largest experiment in the Northern Hemisphere studying ultrahigh energy cosmic rays. TA measurements of the cosmic ray spectrum using the surface detector have the best statistical power in the experiment, and observe the ankle of the spectrum and the high energy cutoff. When the data are divided into two declination bands, above and below 24.8 degrees, the cutoff appears at $10^{19.64 \pm 0.04}$ ($10^{19.84 \pm 0.02}$) eV in the lower (higher) band, an energy difference of 58\%. The global significance of the difference is 4.3 standard deviations. The lack of an instrumental cause of this difference implies it is astrophysical in nature.
Published: 2018

34. Evaluation of the Interplanetary Magnetic Field Strength Using the Cosmic-Ray Shadow of the Sun

Author: Amenomori, M., Bi, X. J., Chen, D., Chen, T. L., Chen, W. Y., Cui, S. W., Danzengluobu, Ding, L. K., Feng, C. F., Feng, Zhaoyang, Feng, Z. Y., Gou, Q. B., Guo, Y. Q., He, H. H., He, Z. T., 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., Lu, H., Meng, X. R., Miyazaki, T., Mizutani, K., Munakata, K., Nakajima, T., Nakamura, Y., Nanjo, H., Nishizawa, M., Niwa, T., Ohnishi, M., Ohta, I., Ozawa, S., Qian, X. L., Qu, X. B., Saito, T., Saito, T. Y., Sakata, M., Sako, T. K., Shao, J., Shibata, M., Shiomi, A., Shirai, T., Sugimoto, H., Takita, M., Tan, Y. H., Tateyama, N., Torii, S., Tsuchiya, H., Udo, S., Wang, H., Wu, H. R., Xue, L., Yamamoto, Y., Yamauchi, K., Yang, Z., Yuan, S. A. F., Yuda, T., Zhai, L. M., Zhang, H. M., Zhang, J. L., Zhang, X. Y., Zhang, Y., Zhang, Yi, Zhang, Ying, Zhaxisangzhu, and Zho, X. X.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Physics - Space Physics
Abstract: We analyze the Sun's shadow observed with the Tibet-III air shower array and find that the shadow's center deviates northward (southward) from the optical solar disc center in the "Away" ("Toward") IMF sector. By comparing with numerical simulations based on the solar magnetic field model, we find that the average IMF strength in the "Away" ("Toward") sector is $1.54 \pm 0.21_{\rm stat} \pm 0.20_{\rm syst}$ ($1.62 \pm 0.15_{\rm stat} \pm 0.22_{\rm syst}$) times larger than the model prediction. These demonstrate that the observed Sun's shadow is a useful tool for the quantitative evaluation of the average solar magnetic field., Comment: 7 pages, 4 figures
Published: 2018
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35. Search for Anisotropy in the Ultra High Energy Cosmic Ray Spectrum using the Telescope Array Surface Detector

Author: Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., Fujii, T., Fukushima, M., Goto, T., Hanlon, W., Hayashi, Y., Hayashi, M., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kishigami, S., Kitamura, S., Kitamura, Y., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lan, J., Lubsandorzhiev, B., Lundquist, J. P., Machida, K., Martens, K., Matsuda, T., Matsuyama, T., Matthews, J. N., Minamino, M., Mukai, K., Myers, I., Nagasawa, K., Nagataki, S., Nakamura, T., Nonaka, T., Nozato, A., Ogio, S., Ogura, J., Ohnishi, M., Ohoka, H., Oki, K., Okuda, T., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Saito, K., Saito, Y., Sakaki, N., Sakurai, N., Scott, L. M., Sekino, K., Shah, P. D., Shibata, T., Shibata, F., Shimodaira, H., Shin, B. K., Shin, H. S., Smith, J. D., Sokolsky, P., Stokes, B. T., Stratton, S. R., Stroman, T. A., Suzawa, T., Takahashi, Y., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, M., Tanaka, K., Tanaka, H., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Tsutsumi, K., Uchihori, Y., Udo, S., Urban, F., Wong, T., Yamane, R., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoneda, Y., Yoshida, S., Yoshii, H., Zhezher, Y., Zollinger, R., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The Telescope Array (TA) experiment is located in the western desert of Utah, USA, and observes ultra high energy cosmic rays (UHECRs) in the Northern hemisphere. At the highest energies, $E>10$~EeV, the shape of cosmic ray energy spectrum may carry an imprint of the source density distribution along the line of sight different in different directions of the sky. In this study, we search for such directional variations in the shape of the energy spectrum using events observed with the Telescope Array's surface detector. We divide the TA field of view into two nearly equal-exposure regions: the "on-source" region which we define as $\pm 30^\circ$ of the supergalactic plane containing mostly nearby structures, and the complementary "off-source" region where the sources are further away on average. We compare the UHECR spectra in these regions by fitting them to the broken power law and comparing the resulting parameters. We find that the off-source spectrum has an earlier break at highest energies. The chance probability to obtain such or larger difference in statistically equivalent distributions is estimated as $6.2\pm1.1\times10^{-4}$ ($3.2\sigma$) by a Monte-Carlo simulation. The observed difference in spectra is in a reasonable quantitative agreement with a simplified model that assumes that the UHECR sources trace the galaxy distribution from the 2MRS catalogue, primary particles are protons and the magnetic deflections can be neglected., Comment: 17 pages 6 figures, submitted to Physical Review Letters, (31.May.2017)
Published: 2017

36. Analysis of solar gamma rays and solar neutrons detected on March 7th and September 25th of 2011 by Ground Level Neutron Telescopes, SEDA-FIB and FERMI-LAT

Author: Muraki, Y., Valdes-Galicia, J. F., Gonzalez, L. X., Kamiya, K., Katayose, Y., Koga, K., Matsumoto, H., Masuda, S., Matsubara, Y., Nagai, Y., Ohnishi, M., Ozawa, S., Sako, T., Shibata, S., Takita, M., Tanaka, Y., Tsuchiya, H., Watanabe, K., and Zhang, J. L.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: At the 33rd ICRC, we reported the possible detection of solar gamma rays by a ground level detector and later re-examined this event. On March 7, 2011, the solar neutron telescope (SNT) located at Mt. Sierra Negra, Mexico (4,600 m) observed enhancements of the counting rate from 19:49 to 20:02 UT and from 20:50 to 21:01 UT. The statistical significance was 9.7sigma and 8.5sigma, respectively. This paper discusses the possibility of using this mountain detector to detect solar gamma rays. In association with this event, the solar neutron detector SEDA-FIB onboard the International Space Station has also detected solar neutrons with a statistical significance of 7.5sigma. The FERMI-LAT detector also observed high-energy gamma rays from this flare with a statistical significance of 6.7sigma. We thus attempted to make a unified model to explain this data. In this paper, we report on another candidate for solar gamma rays detected on September 25th, 2011 by the SNT located in Tibet (4,300 m) from 04:37 to 04:47 UT with a statistical significance of 8.0sigma (by the Li-Ma method)., Comment: 15 pages
Published: 2017

37. Gamma-ray Showers Observed at Ground Level in Coincidence With Downward Lightning Leaders

Author: Abbasi, R. U., Abu-Zayyad, T., Allen, M., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Byrne, M., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., Fujii, T., Fukushima, M., Furlich, G., Goto, T., Hanlon, W., Hayashi, Y., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ito, H., Ivanov, D., Jeong, S., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kishigami, S. S., Krehbiel, P. R., Kuzmin, V., Kwon, Y. J., Lan, J., LeVon, R., Lundquist, J. P., Machida, K., Martens, K., Matuyama, T., Matthews, J. N., Minamino, M., Mukai, K., Myers, I., Nagataki, S., Nakamura, R., Nakamura, T., Nonaka, T., Ogio, S., Ohnishi, M., Ohoka, H., Oki, K., Okuda, T., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Remington, J., Rison, W., Rodeheffer, D., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Saito, K., Sakaki, N., Sakurai, N., Seki, T., Sekino, K., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Smith, J. D., Sokolsky, P., Springer, R. W., Stokes, B. T., Stroman, T. A., Takai, H., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Thomas, R. J., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Uchihori, Y., Udo, S., Urban, F., Vasiloff, G., Wong, T., Yamamoto, M., Yamane, R., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoneda, Y., Yoshida, S., Yoshii, H., and Zundel, Z.
Subjects: Physics - Atmospheric and Oceanic Physics, Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract: Bursts of gamma ray showers have been observed in coincidence with downward propagating negative leaders in lightning flashes by the Telescope Array Surface Detector (TASD). The TASD is a 700~square kilometer cosmic ray observatory located in southwestern Utah, U.S.A. In data collected between 2014 and 2016, correlated observations showing the structure and temporal development of three shower-producing flashes were obtained with a 3D lightning mapping array, and electric field change measurements were obtained for an additional seven flashes, in both cases co-located with the TASD. National Lightning Detection Network (NLDN) information was also used throughout. The showers arrived in a sequence of 2--5 short-duration ($\le$10~$\mu$s) bursts over time intervals of several hundred microseconds, and originated at an altitude of $\simeq$3--5 kilometers above ground level during the first 1--2 ms of downward negative leader breakdown at the beginning of cloud-to-ground lightning flashes. The shower footprints, associated waveforms and the effect of atmospheric propagation indicate that the showers consist primarily of downward-beamed gamma radiation. This has been supported by GEANT simulation studies, which indicate primary source fluxes of $\simeq$$10^{12}$--$10^{14}$ photons for $16^{\circ}$ half-angle beams. We conclude that the showers are terrestrial gamma-ray flashes (TGFs), similar to those observed by satellites, but that the ground-based observations are more representative of the temporal source activity and are also more sensitive than satellite observations, which detect only the most powerful TGFs.
Published: 2017
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38. Significant Improvement of Prognosis After the Advent of Immune Checkpoint Inhibitors in Patients with Advanced, Unresectable, or Metastatic Urothelial Carcinoma: A Propensity Score Matching and Inverse Probability of Treatment Weighting Analysis on Real-World Data

Author: Miyake M, Nishimura N, Shimizu T, Ohnishi M, Kuwada M, Itami Y, Inoue T, Ohnishi K, Matsumoto Y, Yoshida T, Tatsumi Y, Shinohara M, Hori S, Morizawa Y, Gotoh D, Nakai Y, Anai S, Torimoto K, Aoki K, Fujii T, Tanaka N, and Fujimoto K
Subjects: urinary bladder neoplasms, immunotherapy, chemotherapy, survival, propensity score, Neoplasms. Tumors. Oncology. Including cancer and carcinogens, RC254-282
Abstract: Makito Miyake,1 Nobutaka Nishimura,1,2 Takuto Shimizu,1,3 Mikiko Ohnishi,4 Masaomi Kuwada,4 Yoshitaka Itami,5 Takeshi Inoue,5 Kenta Ohnishi,6 Yoshihiro Matsumoto,6 Takanori Yoshida,7 Yoshihiro Tatsumi,8 Masatake Shinohara,9 Shunta Hori,1 Yosuke Morizawa,1 Daisuke Gotoh,1 Yasushi Nakai,1 Satoshi Anai,1 Kazumasa Torimoto,1 Katsuya Aoki,1 Tomomi Fujii,10 Nobumichi Tanaka,1,11 Kiyohide Fujimoto1 1Department of Urology, Nara Medical University, Kashihara, Nara, 634-8522, Japan; 2Department of Urology, Okanami General Hospital, Iga, Mie, Japan; 3Department of Urology, Saiseikai Chuwa Hospital, Nara, Japan; 4Department of Urology, Matsusaka Chuo General Hospital, Matsusaka, Mie, Japan; 5Department of Urology, Nara Prefecture General Medical Center, Nara, Japan; 6Department of Urology, Hoshigaoka Medical Center, Hirakata, Osaka, Japan; 7Department of Urology, Tane General Hospital, Osaka, Japan; 8Department of Urology, JCHO Yamato Koriyama Hospital, Koriyama, Nara, Japan; 9Department of Urology, Osaka Gyoumeikan Hospital, Osaka, Japan; 10Department of Diagnostic Pathology, Nara Medical University, Kashihara, Nara, 634-8522, Japan; 11Department of Prostate Brachytherapy, Nara Medical University, Kashihara, Nara, 634-8522, JapanCorrespondence: Makito Miyake, Department of Urology, Nara Medical University, 840 Shijo-cho, Nara, 634-8522, Japan, Tel +81-744-22-3051 (ext 2338), Fax +81-744-22-9282, Email makitomiyake@yahoo.co.jpPurpose: The treatment landscape for advanced, unresectable, or metastatic urothelial carcinoma (aUC) has shifted substantially since the advent of immune checkpoint inhibitors (ICIs). We investigated the extent to which pembrolizumab therapy is superior to conventional chemotherapy as a second-line treatment.Patients and Methods: A multicenter-derived database registered 454 patients diagnosed with aUC between 2008 and 2020. Of these, 94 patients (21%) who received second-line pembrolizumab and 75 (17%) who received second-line chemotherapy but never received third-line or later ICI therapy were included. We compared overall survival (OS) from the initial date of first-line chemotherapy between two groups by adjusting for prognostic factors through propensity score matching (PSM) and inverse probability of treatment weighting (IPTW). The IPTW-adjusted hazard ratio and 95% confidence interval were estimated using a multivariate Cox regression analysis. To identify patients who were more likely to benefit from second-line pembrolizumab than from chemotherapy, we performed a subgroup analysis for OS with an IPTW-adjusted model.Results: The PSM-adjusted comparison showed a significant improvement in the prognosis with second-line pembrolizumab use (P = 0.01). The OS benefit with the advent of pembrolizumab was 8 months (18 months vs 26 months). Multivariable analyses using IPTW adjustment demonstrated that lymph node metastasis (P = 0.001), lung metastasis (P = 0.013), and bone metastasis (P = 0.003) were poor independent prognostic factors, and pembrolizumab use (P = 0.021) was a favorable independent prognostic factor. Subgroup analyses revealed that pembrolizumab was associated with survival benefits over chemotherapy in all subgroups, including young patients (age < 70 years), those who received radical surgery, and those without visceral metastasis.Conclusion: We demonstrated a significant improvement in prognosis after the advent of pembrolizumab for patients with aUC. ICIs should not be restricted based on patient characteristics.Keywords: urinary bladder neoplasms, immunotherapy, chemotherapy, survival, propensity score
Published: 2022

39. Search for EeV Protons of Galactic Origin

Author: Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., Fujii, T., Fukushima, M., Goto, T., Hanlon, W., Hayashi, Y., Hayashi, M., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kishigami, S., Kitamura, S., Kitamura, Y., Kuzmin, V., Kwon, Y. J., Lan, J., Lubsandorzhiev, B., Lundquist, J. P., Machida, K., Martens, K., Matsuda, T., Matsuyama, T., Matthews, J. N., Minamino, M., Mukai, K., Myers, I., Nagasawa, K., Nagataki, S., Nakamura, T., Nonaka, T., Nozato, A., Ogio, S., Ogura, J., Ohnishi, M., Ohoka, H., Oki, K., Okuda, T., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Saito, K., Saito, Y., Sakaki, N., Sakurai, N., Scott, L. M., Sekino, K., Shah, P. D., Shibata, T., Shibata, F., Shimodaira, H., Shin, B. K., Shin, H. S., Smith, J. D., Sokolsky, P., Stokes, B. T., Stratton, S. R., Stroman, T. A., Suzawa, T., Takahashi, Y., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, M., Tanaka, K., Tanaka, H., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tirone, A. H., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Tsutsumi, K., Uchihori, Y., Udo, S., Urban, F., Wong, T., Yamane, R., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoneda, Y., Yoshida, S., Yoshii, H., Zollinger, R., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Cosmic rays in the energy range $10^{18.0}$ - $10^{18.5}$ eV are thought to have a light, probably protonic, composition. To study their origin one can search for anisotropy in their arrival directions. Extragalactic cosmic rays should be isotropic, but galactic cosmic rays of this type should be seen mostly along the galactic plane, and there should be a shortage of events coming from directions near the galactic anticenter. This is due to the fact that, under the influence of the galactic magnetic field, the transition from ballistic to diffusive behavior is well advanced, and this qualitative picture persists over the whole energy range. Guided by models of the galactic magnetic field that indicate that the enhancement along the galactic plane should have a standard deviation of about 20$^\circ$ in galactic latitude, and the deficit in the galactic anticenter direction should have a standard deviation of about 50$^\circ$ in galactic longitude, we use the data of the Telescope Array surface detector in $10^{18.0}$ to $10^{18.5}$ eV energy range to search for these effects. The data are isotropic. Neither an enhancement along the galactic plane nor a deficit in the galactic anticenter direction is found. Using these data we place an upper limit on the fraction of EeV cosmic rays of galactic origin at 1.3% at 95% confidence level.
Published: 2016
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40. First Upper Limits on the Radar Cross Section of Cosmic-Ray Induced Extensive Air Showers

Author: Abbasi, R. U., Abe, M., Othman, M. Abou Bakr, Abu-Zayyad, T., Allen, M., Anderson, R., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Besson, D., Blake, S. A., Byrne, M., Cady, R., Chae, M. J., Cheon, B. G., Chiba, J., Chikawa, M., Cho, W. R., Farhang-Boroujeny, B., Fujii, T., Fukushima, M., Gillman, W. H., Goto, T., Hanlon, W., Hanson, J. C., Hayashi, Y., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Jayanthmurthy, C., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kitamura, S., Kitamura, Y., Kunwar, S., Kuzmin, V., Kwon, Y. J., Lan, J., Lim, S. I., Lundquist, J. P., Machida, K., Martens, K., Matsuda, T., Matsuyama, T., Matthews, J. N., Minamino, M., Mukai, K., Myers, I., Nagasawa, K., Nagataki, S., Nakamura, T., Nonaka, T., Nozato, A., Ogio, S., Ogura, J., Ohnishi, M., Ohoka, H., Oki, K., Okuda, T., Ono, M., Oshima, A., Ozawa, S., Park, I. H., Prohira, S., Pshirkov, M. S., Rezazadeh-Reyhani, A., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sakurai, N., Sampson, A. L., Scott, L. M., Schurig, D., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Smith, J. D., Sokolsky, P., Springer, R. W., Stokes, B. T., Stratton, S. R., Stroman, T. A., Suzawa, T., Takai, H., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Tsutsumi, K., Uchihori, Y., Udo, S., Urban, F., Vasiloff, G., Venkatesh, S., Wong, T., Yamane, R., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoneda, Y., Yoshida, S., Yoshii, H., Zollinger, R., and Zundel, Z.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: TARA (Telescope Array Radar) is a cosmic ray radar detection experiment colocated with Telescope Array, the conventional surface scintillation detector (SD) and fluorescence telescope detector (FD) near Delta, Utah, U.S.A. The TARA detector combines a 40 kW, 54.1 MHz VHF transmitter and high-gain transmitting antenna which broadcasts the radar carrier over the SD array and within the FD field of view, towards a 250 MS/s DAQ receiver. TARA has been collecting data since 2013 with the primary goal of observing the radar signatures of extensive air showers (EAS). Simulations indicate that echoes are expected to be short in duration (~10 microseconds) and exhibit rapidly changing frequency, with rates on the order of 1 MHz/microsecond. The EAS radar cross-section (RCS) is currently unknown although it is the subject of over 70 years of speculation. A novel signal search technique is described in which the expected radar echo of a particular air shower is used as a matched filter template and compared to waveforms obtained by triggering the radar DAQ using the Telescope Array fluorescence detector. No evidence for the scattering of radio frequency radiation by EAS is obtained to date. We report the first quantitative RCS upper limits using EAS that triggered the Telescope Array Fluorescence Detector., Comment: 21 pages, 30 figures
Published: 2016
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41. Ultimate impedance of coherent heat conduction in van der Waals graphene-MoS2 heterostructures

Author: Hu, S., Ju, S., Shao, C., Guo, J., Xu, B., Ohnishi, M., and Shiomi, J.
Published: 2021
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42. Search for correlations between the arrival directions of IceCube neutrino events and ultrahigh-energy cosmic rays detected by the Pierre Auger Observatory and the Telescope Array

Author: The IceCube Collaboration, Aartsen, M. G., Abraham, K., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Altmann, D., Anderson, T., Ansseau, I., Archinger, M., Arguelles, C., Arlen, T. C., Auffenberg, J., Bai, X., Barwick, S. W., Baum, V., Bay, R., Beatty, J. J., Tjus, J. Becker, Becker, K. -H., Beiser, E., Berghaus, P., Berley, D., Bernardini, E., Bernhard, A., Besson, D. Z., Binder, G., Bindig, D., Bissok, M., Blaufuss, E., Blumenthal, J., Boersma, D. J., Bohm, C., Börner, M., Bos, F., Bose, D., Böser, S., Botner, O., Braun, J., Brayeur, L., Bretz, H. -P., Buzinsky, N., Casey, J., Casier, M., Cheung, E., Chirkin, D., Christov, A., Clark, K., Classen, L., Coenders, S., Cowen, D. F., Silva, A. H. Cruz, Daughhetee, J., Davis, J. C., Day, M., de André, J. P. A. M., De Clercq, C., Rosendo, E. del Pino, Dembinski, H., De Ridder, S., Desiati, P., de Vries, K. D., de Wasseige, G., de With, M., DeYoung, T., Díaz-Vélez, J. C., di Lorenzo, V., Dumm, J. P., Dunkman, M., Eberhardt, B., Ehrhardt, T., Eichmann, B., Euler, S., Evenson, P. A., Fahey, S., Fazely, A. R., Feintzeig, J., Felde, J., Filimonov, K., Finley, C., Fischer-Wasels, T., Flis, S., Fösig, C. -C., Fuchs, T., Gaisser, T. K., Gaior, R., Gallagher, J., Gerhardt, L., Ghorbani, K., Gier, D., Gladstone, L., Glagla, M., Glüsenkamp, T., Goldschmidt, A., Golup, G., Gonzalez, J. G., Góra, D., Grant, D., Griffith, Z., Groß, A., Ha, C., Haack, C., Ismail, A. Haj, Hallgren, A., Halzen, F., Hansen, E., Hansmann, B., Hanson, K., Hebecker, D., Heereman, D., Helbing, K., Hellauer, R., Hickford, S., Hignight, J., Hill, G. C., Hoffman, K. D., Hoffmann, R., Holzapfel, K., Homeier, A., Hoshina, K., Huang, F., Huber, M., Huelsnitz, W., Hulth, P. O., Hultqvist, K., In, S., Ishihara, A., Jacobi, E., Japaridze, G. S., Jeong, M., Jero, K., Jurkovic, M., Kappes, A., Karg, T., Karle, A., Kauer, M., Keivani, A., Kelley, J. L., Kemp, J., Kheirandish, A., Kiryluk, J., Kläs, J., Klein, S. R., Kohnen, G., Koirala, R., Kolanoski, H., Konietz, R., Köpke, L., Kopper, C., Kopper, S., Koskinen, D. J., Kowalski, M., Krings, K., Kroll, G., Kroll, M., Krückl, G., Kunnen, J., Kurahashi, N., Kuwabara, T., Labare, M., Lanfranchi, J. L., Larson, M. J., Lesiak-Bzdak, M., Leuermann, M., Leuner, J., Lu, L., Lünemann, J., Madsen, J., Maggi, G., Mahn, K. B. M., Mandelartz, M., Maruyama, R., Mase, K., Matis, H. S., Maunu, R., McNally, F., Meagher, K., Medici, M., Meli, A., Menne, T., Merino, G., Meures, T., Miarecki, S., Middell, E., Mohrmann, L., Montaruli, T., Morse, R., Nahnhauer, R., Naumann, U., Neer, G., Niederhausen, H., Nowicki, S. C., Nygren, D. R., Pollmann, A. Obertacke, Olivas, A., Omairat, A., O'Murchadha, A., Palczewski, T., Pandya, H., Pankova, D. V., Paul, L., Pepper, J. A., Heros, C. Pérez de los, Pfendner, C., Pieloth, D., Pinat, E., Posselt, J., Price, P. B., Przybylski, G. T., Quinnan, M., Raab, C., Rädel, L., Rameez, M., Rawlins, K., Reimann, R., Relich, M., Resconi, E., Rhode, W., Richman, M., Richter, S., Riedel, B., Robertson, S., Rongen, M., Rott, C., Ruhe, T., Ryckbosch, D., Sabbatini, L., Sander, H. -G., Sandrock, A., Sandroos, J., Sarkar, S., Schatto, K., Schimp, M., Schmidt, T., Schoenen, S., Schöneberg, S., Schönwald, A., Schulte, L., Schumacher, L., Seckel, D., Seunarine, S., Soldin, D., Song, M., Spiczak, G. M., Spiering, C., Stahlberg, M., Stamatikos, M., Stanev, T., Stasik, A., Steuer, A., Stezelberger, T., Stokstad, R. G., Stößl, A., Ström, R., Strotjohann, N. L., Sullivan, G. W., Sutherland, M., Taavola, H., Taboada, I., Tatar, J., Ter-Antonyan, S., Terliuk, A., Tešić, G., Tilav, S., Toale, P. A., Tobin, M. N., Toscano, S., Tosi, D., Tselengidou, M., Turcati, A., Unger, E., Usner, M., Vallecorsa, S., Vandenbroucke, J., van Eijndhoven, N., Vanheule, S., van Santen, J., Veenkamp, J., Vehring, M., Voge, M., Vraeghe, M., Walck, C., Wallace, A., Wallraff, M., Wandkowsky, N., Weaver, Ch., Wendt, C., Westerhoff, S., Whelan, B. J., Wiebe, K., Wiebusch, C. H., Wille, L., Williams, D. R., Wissing, H., Wolf, M., Wood, T. R., Woschnagg, K., Xu, D. L., Xu, X. W., Xu, Y., Yanez, J. P., Yodh, G., Yoshida, S., Collaboration, M. Zoll. The Pierre Auger, Aab, A., Abreu, P., Aglietta, M., Ahn, E. J., Samarai, I. Al, Albuquerque, I. F. M., Allekotte, I., Allison, P., Almela, A., Castillo, J. Alvarez, Alvarez-Muñiz, J., Batista, R. Alves, Ambrosio, M., Aminaei, A., Anchordoqui, L., Andrada, B., Andringa, S., Aramo, C., Arqueros, F., Arsene, N., Asorey, H., Assis, P., Aublin, J., Avila, G., Awal, N., Badescu, A. M., Baus, C., Becker, K. H., Bellido, J. A., Berat, C., Bertaina, M. E., Bertou, X., Biermann, P. L., Billoir, P., Blaess, S. G., Blanco, A., Blanco, M., Blazek, J., Bleve, C., Blümer, H., Boháčová, M., Boncioli, D., Bonifazi, C., Borodai, N., Botti, A. M., Brack, J., Brancus, I., Bretz, T., Bridgeman, A., Briechle, F. L., Buchholz, P., Bueno, A., Buitink, S., Buscemi, M., Caballero-Mora, K. S., Caccianiga, B., Caccianiga, L., Candusso, M., Caramete, L., Caruso, R., Castellina, A., Cataldi, G., Cazon, L., Cester, R., Chavez, A. G., Chiavassa, A., Chinellato, J. A., Diaz, J. C. Chirinos, Chudoba, J., Clay, R. W., Colalillo, R., Coleman, A., Collica, L., Coluccia, M. R., Conceição, R., Contreras, F., Cooper, M. J., Cordier, A., Coutu, S., Covault, C. E., Dallier, R., D'Amico, S., Daniel, B., Dasso, S., Daumiller, K., Dawson, B. R., de Almeida, R. M., de Jong, S. J., De Mauro, G., Neto, J. R. T. de Mello, De Mitri, I., de Oliveira, J., de Souza, V., Debatin, J., del Peral, L., Deligny, O., Dhital, N., Di Giulio, C., Di Matteo, A., Castro, M. L. Díaz, Diogo, F., Dobrigkeit, C., Docters, W., D'Olivo, J. C., Dorofeev, A., Anjos, R. C. dos, Dova, M. T., Dundovic, A., Ebr, J., Engel, R., Erdmann, M., Erfani, M., Escobar, C. O., Espadanal, J., Etchegoyen, A., Falcke, H., Fang, K., Farrar, G., Fauth, A. C., Fazzini, N., Ferguson, A. P., Fick, B., Figueira, J. M., Filevich, A., Filipčič, A., Fratu, O., Freire, M. M., Fujii, T., Fuster, A., Gallo, F., García, B., Garcia-Gamez, D., Garcia-Pinto, D., Gate, F., Gemmeke, H., Gherghel-Lascu, A., Ghia, P. L., Giaccari, U., Giammarchi, M., Giller, M., Głas, D., Glaser, C., Glass, H., Berisso, M. Gómez, Vitale, P. F. Gómez, González, N., Gookin, B., Gordon, J., Gorgi, A., Gorham, P., Gouffon, P., Griffith, N., Grillo, A. F., Grubb, T. D., Guarino, F., Guedes, G. P., Hampel, M. R., Hansen, P., Harari, D., Harrison, T. A., Harton, J. L., Hasankiadeh, Q., Haungs, A., Hebbeker, T., Heck, D., Heimann, P., Herve, A. E., Hojvat, C., Hollon, N., Holt, E., Homola, P., Hörandel, J. 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Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: This paper presents the results of different searches for correlations between very high-energy neutrino candidates detected by IceCube and the highest-energy cosmic rays measured by the Pierre Auger Observatory and the Telescope Array. We first consider samples of cascade neutrino events and of high-energy neutrino-induced muon tracks, which provided evidence for a neutrino flux of astrophysical origin, and study their cross-correlation with the ultrahigh-energy cosmic ray (UHECR) samples as a function of angular separation. We also study their possible directional correlations using a likelihood method stacking the neutrino arrival directions and adopting different assumptions on the size of the UHECR magnetic deflections. Finally, we perform another likelihood analysis stacking the UHECR directions and using a sample of through-going muon tracks optimized for neutrino point-source searches with sub-degree angular resolution. No indications of correlations at discovery level are obtained for any of the searches performed. The smallest of the p-values comes from the search for correlation between UHECRs with IceCube high-energy cascades, a result that should continue to be monitored., Comment: Replaced with published version. Added journal reference and DOI
Published: 2015
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43. The IceCube Neutrino Observatory, the Pierre Auger Observatory and the Telescope Array: Joint Contribution to the 34th International Cosmic Ray Conference (ICRC 2015)

Author: IceCube Collaboration, Aartsen, M. G., Abraham, K., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Altmann, D., Anderson, T., Ansseau, I., Archinger, M., Arguelles, C., Arlen, T. C., Auffenberg, J., Bai, X., Barwick, S. W., Baum, V., Bay, R., Beatty, J. J., Tjus, J. Becker, Becker, K. -H., Beiser, E., BenZvi, S., Berghaus, P., Berley, D., Bernardini, E., Bernhard, A., Besson, D. Z., Binder, G., Bindig, D., Bissok, M., Blaufuss, E., Blumenthal, J., Boersma, D. J., Bohm, C., Börner, M., Bos, F., Bose, D., Böser, S., Botner, O., Braun, J., Brayeur, L., Bretz, H. -P., Buzinsky, N., Casey, J., Casier, M., Cheung, E., Chirkin, D., Christov, A., Clark, K., Classen, L., Coenders, S., Cowen, D. F., Silva, A. H. Cruz, Daughhetee, J., Davis, J. C., Day, M., de André, J. P. A. M., De Clercq, C., Rosendo, E. del Pino, Dembinski, H., De Ridder, S., Desiati, P., de Vries, K. D., de Wasseige, G., de With, M., DeYoung, T., Díaz-Vélez, J. C., di Lorenzo, V., Dumm, J. P., Dunkman, M., Eagan, R., Eberhardt, B., Ehrhardt, T., Eichmann, B., Euler, S., Evenson, P. A., Fadiran, O., Fahey, S., Fazely, A. R., Fedynitch, A., Feintzeig, J., Felde, J., Filimonov, K., Finley, C., Fischer-Wasels, T., Flis, S., Fösig, C. -C., Fuchs, T., Gaisser, T. K., Gaior, R., Gallagher, J., Gerhardt, L., Ghorbani, K., Gier, D., Gladstone, L., Glagla, M., Glüsenkamp, T., Goldschmidt, A., Golup, G., Gonzalez, J. G., Góra, D., Grant, D., Groh, J. C., Groß, A., Ha, C., Haack, C., Ismail, A. Haj, Hallgren, A., Halzen, F., Hansmann, B., Hanson, K., Hebecker, D., Heereman, D., Helbing, K., Hellauer, R., Hellwig, D., Hickford, S., Hignight, J., Hill, G. C., Hoffman, K. D., Hoffmann, R., Holzapfel, K., Homeier, A., Hoshina, K., Huang, F., Huber, M., Huelsnitz, W., Hulth, P. O., Hultqvist, K., In, S., Ishihara, A., Jacobi, E., Japaridze, G. S., Jero, K., Jurkovic, M., Kaminsky, B., Kappes, A., Karg, T., Karle, A., Kauer, M., Keivani, A., Kelley, J. 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J., Querchfeld, S., Quinn, S., Rautenberg, J., Ravel, O., Ravignani, D., Reinert, D., Revenu, B., Ridky, J., Risse, M., Ristori, P., Rizi, V., de Carvalho, W. Rodrigues, Rojo, J. Rodriguez, Rodríguez-Frías, M. D., Rogozin, D., Rosado, J., Roth, M., Roulet, E., Rovero, A. C., Saffi, S. J., Saftoiu, A., Salamida, F., Salazar, H., Saleh, A., Greus, F. Salesa, Salina, G., Gomez, J. D. Sanabria, Sánchez, F., Sanchez-Lucas, P., Santos, E. M., Santos, E., Sarazin, F., Sarkar, B., Sarmento, R., Sarmiento-Cano, C., Sato, R., Scarso, C., Schauer, M., Scherini, V., Schieler, H., Schmidt, D., Scholten, O., Schoorlemmer, H., Schovánek, P., Schröder, F. G., Schulz, A., Schulz, J., Schumacher, J., Sciutto, S. J., Segreto, A., Settimo, M., Shadkam, A., Shellard, R. C., Sigl, G., Sima, O., Śmiałkowski, A., Šmída, R., Snow, G. R., Sommers, P., Sonntag, S., Sorokin, J., Squartini, R., Srivastava, Y. N., Stanca, D., Stanič, S., Stapleton, J., Stasielak, J., Stephan, M., Stutz, A., Suarez, F., Durán, M. Suarez, Suomijärvi, T., Supanitsky, A. D., Sutherland, M. S., Swain, J., Szadkowski, Z., Taborda, O. A., Tapia, A., Tepe, A., Theodoro, V. M., Tibolla, O., Timmermans, C., Peixoto, C. J. Todero, Toma, G., Tomankova, L., Tomé, B., Tonachini, A., Elipe, G. Torralba, Machado, D. Torres, Travnicek, P., Trini, M., Ulrich, R., Unger, M., Urban, M., Galicia, J. F. Valdés, Valiño, I., Valore, L., van Aar, G., van Bodegom, P., Berg, A. M. van den, van Velzen, S., van Vliet, A., Varela, E., Cárdenas, B. Vargas, Varner, G., Vasquez, R., Vázquez, J. R., Vázquez, R. A., Veberič, D., Verzi, V., Vicha, J., Videla, M., Villaseñor, L., Vlcek, B., Vorobiov, S., Wahlberg, H., Wainberg, O., Walz, D., Watson, A. A., Weber, M., Weidenhaupt, K., Weindl, A., Welling, C., Werner, F., Widom, A., Wiencke, L., Wilczyński, H., Winchen, T., Wittkowski, D., Wundheiler, B., Wykes, S., Yang, L., Yapici, T., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zepeda, A., Zimmermann, B., Ziolkowski, M., Zuccarello, F., Collaboration, Telescope Array, Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Chae, M. J., Cheon, B. G., Chiba, J., Chikawa, M., Cho, W. R., Fukushima, M., Goto, T., Hanlon, W., Hayashi, Y., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kitamura, S., Kitamura, Y., Kuzmin, V., Kwon, Y. J., Lan, J., Lim, S. I., Lundquist, J. P., Machida, K., Martens, K., Matsuda, T., Matsuyama, T., Matthews, J. N., Minamino, M., Mukai, Y., Myers, I., Nagasawa, K., Nagataki, S., Nakamura, T., Nonaka, T., Nozato, A., Ogio, S., Ogura, J., Ohnishi, M., Ohoka, H., Oki, K., Okuda, T., Ono, M., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sakurai, N., Scott, L. M., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Smith, J. D., Sokolsky, P., Springer, R. W., Stokes, B. T., Stratton, S. R., Stroman, T. A., Suzawa, T., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Tsutsumi, K., Uchihori, Y., Udo, S., Urban, F., Vasiloff, G., Wong, T., Yamane, R., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoneda, Y., Yoshii, H., Zollinger, R., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, High Energy Physics - Experiment
Abstract: We have conducted three searches for correlations between ultra-high energy cosmic rays detected by the Telescope Array and the Pierre Auger Observatory, and high-energy neutrino candidate events from IceCube. Two cross-correlation analyses with UHECRs are done: one with 39 cascades from the IceCube `high-energy starting events' sample and the other with 16 high-energy `track events'. The angular separation between the arrival directions of neutrinos and UHECRs is scanned over. The same events are also used in a separate search using a maximum likelihood approach, after the neutrino arrival directions are stacked. To estimate the significance we assume UHECR magnetic deflections to be inversely proportional to their energy, with values $3^\circ$, $6^\circ$ and $9^\circ$ at 100 EeV to allow for the uncertainties on the magnetic field strength and UHECR charge. A similar analysis is performed on stacked UHECR arrival directions and the IceCube sample of through-going muon track events which were optimized for neutrino point-source searches., Comment: one proceeding, the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The Netherlands; will appear in PoS(ICRC2015)
Published: 2015

44. Pierre Auger Observatory and Telescope Array: Joint Contributions to the 34th International Cosmic Ray Conference (ICRC 2015)

Author: Telescope Array Collaboration, Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Chae, M. J., Cheon, B. G., Chiba, J., Chikawa, M., Cho, W. R., Fujii, T., Fukushima, M., Goto, T., Hanlon, W., Hayashi, Y., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kitamura, S., Kitamura, Y., Kuzmin, V., Kwon, Y. J., Lan, J., Lim, S. I., Lundquist, J. P., Machida, K., Martens, K., Matsuda, T., Matsuyama, T., Matthews, J. N., Minamino, M., Mukai, Y., Myers, I., Nagasawa, K., Nagataki, S., Nakamura, T., Nonaka, T., Nozato, A., Ogio, S., Ogura, J., Ohnishi, M., Ohoka, H., Oki, K., Okuda, T., Ono, M., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sakurai, N., Scott, L. M., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Smith, J. D., Sokolsky, P., Springer, R. W., Stokes, B. T., Stratton, S. R., Stroman, T. A., Suzawa, T., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Tsutsumi, K., Uchihori, Y., Udo, S., Urban, F., Vasiloff, G., Wong, T., Yamane, R., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoneda, Y., Yoshida, S., Yoshii, H., Zollinger, R., Zundel, Z., Collaboration, Pierre Auger, Aab, A., Abreu, P., Aglietta, M., Ahn, E. J., Samarai, I. Al, Albuquerque, I. F. M., Allekotte, I., Allison, P., Almela, A., Castillo, J. Alvarez, Alvarez-Muñiz, J., Batista, R. Alves, Ambrosio, M., Aminaei, A., Anastasi, G. A., Anchordoqui, L., Andringa, S., Aramo, C., Arqueros, F., Arsene, N., Asorey, H., Assis, P., Aublin, J., Avila, G., Awal, N., Badescu, A. M., Baus, C., Beatty, J. J., Becker, K. H., Bellido, J. A., Berat, C., Bertaina, M. E., Bertou, X., Biermann, P. L., Billoir, P., Blaess, S. G., Blanco, A., Blanco, M., Blazek, J., Bleve, C., Blümer, H., Boháčová, M., Boncioli, D., Bonifazi, C., Borodai, N., Brack, J., Brancus, I., Bretz, T., Bridgeman, A., Brogueira, P., Buchholz, P., Bueno, A., Buitink, S., Buscemi, M., Caballero-Mora, K. S., Caccianiga, B., Caccianiga, L., Candusso, M., Caramete, L., Caruso, R., Castellina, A., Cataldi, G., Cazon, L., Cester, R., Chavez, A. G., Chiavassa, A., Chinellato, J. A., Chudoba, J., Cilmo, M., Clay, R. W., Cocciolo, G., Colalillo, R., Coleman, A., Collica, L., Coluccia, M. R., Conceição, R., Contreras, F., Cooper, M. J., Cordier, A., Coutu, S., Covault, C. E., Dallier, R., Daniel, B., Dasso, S., Daumiller, K., Dawson, B. R., de Almeida, R. M., de Jong, S. J., De Mauro, G., Neto, J. R. T. de Mello, De Mitri, I., de Oliveira, J., de Souza, V., del Peral, L., Deligny, O., Dhital, N., Di Giulio, C., Di Matteo, A., Diaz, J. C., Castro, M. L. Díaz, Diogo, F., Dobrigkeit, C., Docters, W., D'Olivo, J. C., Dorofeev, A., Hasankiadeh, Q. Dorosti, Anjos, R. C. dos, Dova, M. T., Ebr, J., Engel, R., Erdmann, M., Erfani, M., Escobar, C. O., Espadanal, J., Etchegoyen, A., Falcke, H., Fang, K., Farrar, G., Fauth, A. C., Fazzini, N., Ferguson, A. P., Fick, B., Figueira, J. M., Filevich, A., Filipčič, A., Fratu, O., Freire, M. M., García, B., García-Gámez, D., Garcia-Pinto, D., Gate, F., Gemmeke, H., Gherghel-Lascu, A., Ghia, P. L., Giaccari, U., Giammarchi, M., Giller, M., Głas, D., Glaser, C., Glass, H., Golup, G., Berisso, M. Gómez, Vitale, P. F. Gómez, González, N., Gookin, B., Gordon, J., Gorgi, A., Gorham, P., Gouffon, P., Griffith, N., Grillo, A. F., Grubb, T. D., Guarino, F., Guedes, G. P., Hampel, M. R., Hansen, P., Harari, D., Harrison, T. A., Hartmann, S., Harton, J. L., Haungs, A., Hebbeker, T., Heck, D., Heimann, P., Hervé, A. E., Hill, G. C., Hojvat, C., Hollon, N., Holt, E., Homola, P., Hörandel, J. R., Horvath, P., Hrabovský, M., Huber, D., Huege, T., Insolia, A., Isar, P. G., Jandt, I., Jansen, S., Jarne, C., Johnsen, J. A., Josebachuili, M., Kääpä, A., Kambeitz, O., Kampert, K. H., Kasper, P., Katkov, I., Keilhauer, B., Kemp, E., Kieckhafer, R. M., Klages, H. O., Kleifges, M., Kleinfeller, J., Krause, R., Krohm, N., Kuempel, D., Mezek, G. Kukec, Kunka, N., Awad, A. W. Kuotb, LaHurd, D., Latronico, L., Lauer, R., Lauscher, M., Lautridou, P., Coz, S. Le, Lebrun, D., Lebrun, P., de Oliveira, M. A. Leigui, Letessier-Selvon, A., Lhenry-Yvon, I., Link, K., Lopes, L., López, R., Casado, A. López, Louedec, K., Lucero, A., Malacari, M., Mallamaci, M., Maller, J., Mandat, D., Mantsch, P., Mariazzi, A. G., Marin, V., Mariş, I. C., Marsella, G., Martello, D., Martinez, H., Bravo, O. Martínez, Martraire, D., Meza, J. J. Masías, Mathes, H. J., Mathys, S., Matthews, J., Matthews, J. A. J., Matthiae, G., Maurizio, D., Mayotte, E., Mazur, P. O., Medina, C., Medina-Tanco, G., Meissner, R., Mello, V. B. B., Melo, D., Menshikov, A., Messina, S., Micheletti, M. I., Middendorf, L., Minaya, I. A., Miramonti, L., Mitrica, B., Molina-Bueno, L., Mollerach, S., Montanet, F., Morello, C., Mostafá, M., Moura, C. A., Müller, G., Muller, M. A., Müller, S., Navas, S., Necesal, P., Nellen, L., Nelles, A., Neuser, J., Nguyen, P. H., Niculescu-Oglinzanu, M., Niechciol, M., Niemietz, L., Niggemann, T., Nitz, D., Nosek, D., Novotny, V., Nožka, L., Núñez, L. A., Ochilo, L., Oikonomou, F., Olinto, A., Pacheco, N., Selmi-Dei, D. Pakk, Palatka, M., Pallotta, J., Papenbreer, P., Parente, G., Parra, A., Paul, T., Pech, M., Pȩkala, J., Pelayo, R., Pepe, I. M., Perrone, L., Petermann, E., Peters, C., Petrera, S., Petrov, Y., Phuntsok, J., Piegaia, R., Pierog, T., Pieroni, P., Pimenta, M., Pirronello, V., Platino, M., Plum, M., Porcelli, A., Porowski, C., Prado, R. R., Privitera, P., Prouza, M., Quel, E. J., Querchfeld, S., Quinn, S., Rautenberg, J., Ravel, O., Ravignani, D., Reinert, D., Revenu, B., Ridky, J., Risse, M., Ristori, P., Rizi, V., de Carvalho, W. Rodrigues, Rojo, J. Rodriguez, Rodríguez-Frías, M. D., Rogozin, D., Rosado, J., Roth, M., Roulet, E., Rovero, A. C., Saffi, S. J., Saftoiu, A., Salamida, F., Salazar, H., Saleh, A., Greus, F. Salesa, Salina, G., Gomez, J. D. Sanabria, Sánchez, F., Sanchez-Lucas, P., Santos, E. M., Santos, E., Sarazin, F., Sarkar, B., Sarmento, R., Sarmiento-Cano, C., Sato, R., Scarso, C., Schauer, M., Scherini, V., Schieler, H., Schmidt, D., Scholten, O., Schoorlemmer, H., Schovánek, P., Schröder, F. G., Schulz, A., Schulz, J., Schumacher, J., Sciutto, S. J., Segreto, A., Settimo, M., Shadkam, A., Shellard, R. C., Sigl, G., Sima, O., Śmiałkowski, A., Šmída, R., Snow, G. R., Sommers, P., Sonntag, S., Sorokin, J., Squartini, R., Srivastava, Y. N., Stanca, D., Stanič, S., Stapleton, J., Stasielak, J., Stephan, M., Stutz, A., Suarez, F., Durán, M. Suarez, Suomijärvi, T., Supanitsky, A. D., Sutherland, M. S., Swain, J., Szadkowski, Z., Taborda, O. A., Tapia, A., Tepe, A., Theodoro, V. M., Tibolla, O., Timmermans, C., Peixoto, C. J. Todero, Toma, G., Tomankova, L., Tomé, B., Tonachini, A., Elipe, G. Torralba, Machado, D. Torres, Travnicek, P., Trini, M., Ulrich, R., Unger, M., Urban, M., Galicia, J. F. Valdés, Valiño, I., Valore, L., van Aar, G., van Bodegom, P., Berg, A. M. van den, van Velzen, S., van Vliet, A., Varela, E., Cárdenas, B. Vargas, Varner, G., Vasquez, R., Vázquez, J. R., Vázquez, R. A., Veberič, D., Verzi, V., Vicha, J., Videla, M., Villaseñor, L., Vlcek, B., Vorobiov, S., Wahlberg, H., Wainberg, O., Walz, D., Watson, A. A., Weber, M., Weidenhaupt, K., Weindl, A., Welling, C., Werner, F., Widom, A., Wiencke, L., Wilczyński, H., Winchen, T., Wittkowski, D., Wundheiler, B., Wykes, S., Yang, L., Yapici, T., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zepeda, A., Zimmermann, B., Ziolkowski, M., and Zuccarello, F.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Joint contributions of the Pierre Auger Collaboration and the Telescope Array Collaboration to the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The Netherlands., Comment: 3 proceedings, the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The Netherlands; will appear in PoS(ICRC2015)
Published: 2015

45. Measurement of the Proton-Air Cross Section with Telescope Array's Middle Drum Detector and Surface Array in Hybrid Mode

Author: Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Anderson, R., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Chae, M. J., Cheon, B. G., Chiba, J., Chikawa, M., Cho, W. R., Fujii, T., Fukushima, M., Goto, T., Hanlon, W., Hayashi, Y., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kitamura, S., Kitamura, Y., Kuzmin, V., Kwon, Y. J., Lan, J., Lim, S. I., Lundquist, J. P., Machida, K., Martens, K., Matsuda, T., Matsuyama, T., Matthews, J. N., Minamino, M., Mukai, K., Myers, I., Nagasawa, K., Nagataki, S., Nakamura, T., Nonaka, T., Nozato, A., Ogio, S., Ogura, J., Ohnishi, M., Ohoka, H., Oki, K., Okuda, T., Ono, M., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sakurai, N., Sampson, A. L., Scott, L. M., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Smith, J. D., Sokolsky, P., Springer, R. W., Stokes, B. T., Stratton, S. R., Stroman, T. A., Suzawa, T., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Tsutsumi, K., Uchihori, Y., Udo, S., Urban, F., Vasiloff, G., Wong, T., Yamane, R., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoneda, Y., Yoshida, S., Yoshii, H., Zollinger, R., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, High Energy Physics - Experiment
Abstract: In this work we are reporting on the measurement of the proton-air inelastic cross section $\sigma^{\rm inel}_{\rm p-air}$ using the Telescope Array (TA) detector. Based on the measurement of the $\sigma^{\rm inel}_{\rm p-air}$ the proton-proton cross section $\sigma_{\rm p-p}$ value is also determined at $\sqrt{s} = 95_{-8}^{+5}$ TeV. Detecting cosmic ray events at ultra high energies with Telescope Array enables us to study this fundamental parameter that we are otherwise unable to access with particle accelerators. The data used in this report is the hybrid events observed by the Middle Drum fluorescence detector together with the surface array detector collected over five years. The value of the $\sigma^{\rm inel}_{\rm p-air}$ is found to be equal to $567.0 \pm 70.5 [{\rm Stat.}] ^{+29}_{-25} [{\rm Sys.}]$ mb. The total proton-proton cross section is subsequently inferred from Glauber Formalism and Block, Halzen and Stanev QCD inspired fit and is found to be equal to $170_{-44}^{+48} [{\rm Stat.}] _{-17}^{+19} [{\rm Sys.}] $mb.
Published: 2015
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46. Searches for Large-Scale Anisotropy in the Arrival Directions of Cosmic Rays Detected above Energy of $10^{19}$ eV at the Pierre Auger Observatory and the Telescope Array

Author: Auger, The Pierre, Collaborations, Telescope Array, Aab, A., Abreu, P., Aglietta, M., Ahn, E. J., Samarai, I. Al, Albuquerque, I. F. M., Allekotte, I., Allen, J., Allison, P., Almela, A., Castillo, J. Alvarez, Alvarez-Muñiz, J., Batista, R. Alves, Ambrosio, M., Aminaei, A., Anchordoqui, L., Andringa, S., Aramo, C., Arqueros, F., Asorey, H., Assis, P., Aublin, J., Ave, M., Avenier, M., Avila, G., Badescu, A. M., Barber, K. B., Bäuml, J., Baus, C., Beatty, J. J., Becker, K. H., Bellido, J. A., Berat, C., Bertou, X., Biermann, P. L., Billoir, P., Blanco, M., Bleve, C., Blümer, H., Boháčová, M., Boncioli, D., Bonifazi, C., Bonino, R., Borodai, N., Brack, J., Brancus, I., Brogueira, P., Brown, W. C., Buchholz, P., Bueno, A., Buitink, S., Buscemi, M., Caballero-Mora, K. S., Caccianiga, B., Caccianiga, L., Candusso, M., Caramete, L., Caruso, R., Castellina, A., Cataldi, G., Cazon, L., Cester, R., Chavez, A. G., Chiavassa, A., Chinellato, J. A., Chudoba, J., Cilmo, M., Clay, R. W., Cocciolo, G., Colalillo, R., Coleman, A., Collica, L., Coluccia, M. R., Conceição, R., Contreras, F., Cooper, M. J., Cordier, A., Coutu, S., Covault, C. E., Cronin, J., Curutiu, A., Dallier, R., Daniel, B., Dasso, S., Daumiller, K., Dawson, B. R., de Almeida, R. M., De Domenico, M., de Jong, S. J., Neto, J. R. T. de Mello, De Mitri, I., de Oliveira, J., de Souza, V., del Peral, L., Deligny, O., Dembinski, H., Dhital, N., Di Giulio, C., Di Matteo, A., Diaz, J. C., Castro, M. L. Díaz, Diogo, F., Dobrigkeit, C., Docters, W., D'Olivo, J. C., Dorofeev, A., Hasankiadeh, Q. Dorosti, Dova, M. T., Ebr, J., Engel, R., Erdmann, M., Erfani, M., Escobar, C. O., Espadanal, J., Etchegoyen, A., Luis, P. Facal San, Falcke, H., Fang, K., Farrar, G., Fauth, A. C., Fazzini, N., Ferguson, A. P., Fernandes, M., Fick, B., Figueira, J. M., Filevich, A., Filipčič, A., Fox, B. D., Fratu, O., Fröhlich, U., Fuchs, B., Fuji, T., Gaior, R., García, B., Roca, S. T. Garcia, Garcia-Gamez, D., Garcia-Pinto, D., Garilli, G., Bravo, A. Gascon, Gate, F., Gemmeke, H., Ghia, P. L., Giaccari, U., Giammarchi, M., Giller, M., Glaser, C., Glass, H., Berisso, M. Gómez, Vitale, P. F. Gómez, Gonçalves, P., Gonzalez, J. G., González, N., Gookin, B., Gorgi, A., Gorham, P., Gouffon, P., Grebe, S., Griffith, N., Grillo, A. F., Grubb, T. D., Guardincerri, Y., Guarino, F., Guedes, G. P., Hampel, M. R., Hansen, P., Harari, D., Harrison, T. A., Hartmann, S., Harton, J. L., Haungs, A., Hebbeker, T., Heck, D., Heimann, P., Herve, A. E., Hill, G. C., Hojvat, C., Hollon, N., Holt, E., Homola, P., Hörandel, J. R., Horvath, P., Hrabovský, M., Huber, D., Huege, T., Insolia, A., Isar, P. G., Islo, K., Jandt, I., Jansen, S., Jarne, C., Josebachuili, M., Kääpä, A., Kambeitz, O., Kampert, K. H., Kasper, P., Katkov, I., Kégl, B., Keilhauer, B., Keivani, A., Kemp, E., Kieckhafer, R. M., Klages, H. O., Kleifges, M., Kleinfeller, J., Krause, R., Krohm, N., Krömer, O., Kruppke-Hansen, D., Kuempel, D., Kunka, N., La Rosa, G., LaHurd, D., Latronico, L., Lauer, R., Lauscher, M., Lautridou, P., Coz, S. Le, Leão, M. S. A. B., Lebrun, D., Lebrun, P., de Oliveira, M. A. Leigui, Letessier-Selvon, A., Lhenry-Yvon, I., Link, K., López, R., Agüera, A. Lopez, Louedec, K., Bahilo, J. Lozano, Lu, L., Lucero, A., Ludwig, M., Maccarone, M. C., Malacari, M., Maldera, S., Mallamaci, M., Maller, J., Mandat, D., Mantsch, P., Mariazzi, A. G., Marin, V., Mariş, I. C., Marsella, G., Martello, D., Martin, L., Martinez, H., Bravo, O. Martínez, Martraire, D., Meza, J. J. Masías, Mathes, H. J., Mathys, S., Matthews, J. A. J., Matthews, J., Matthiae, G., Maurel, D., Maurizio, D., Mayotte, E., Mazur, P. O., Medina, C., Medina-Tanco, G., Melissas, M., Melo, D., Menichetti, E., Menshikov, A., Messina, S., Meyhandan, R., Mićanović, S., Micheletti, M. I., Middendorf, L., Minaya, I. A., Miramonti, L., Mitrica, B., Molina-Bueno, L., Mollerach, S., Monasor, M., Ragaigne, D. Monnier, Montanet, F., Morello, C., Mostafá, M., Moura, C. A., Muller, M. A., Müller, G., Münchmeyer, M., Mussa, R., Navarra, G., Navas, S., Necesal, P., Nellen, L., Nelles, A., Neuser, J., Niechciol, M., Niemietz, L., Niggemann, T., Nitz, D., Nosek, D., Novotny, V., Nožka, L., Ochilo, L., Olinto, A., Oliveira, M., Pacheco, N., Selmi-Dei, D. Pakk, Palatka, M., Pallotta, J., Palmieri, N., Papenbreer, P., Parente, G., Parra, A., Paul, T., Pech, M., Pekala, J., Pelayo, R., Pepe, I. M., Perrone, L., Pesce, R., Petermann, E., Peters, C., Petrera, S., Petrolini, A., Petrov, Y., Phuntsok, J., Piegaia, R., Pierog, T., Pieroni, P., Pimenta, M., Pirronello, V., Platino, M., Plum, M., Porcelli, A., Porowski, C., Prado, R. R., Privitera, P., Prouza, M., Purrello, V., Quel, E. J., Querchfeld, S., Quinn, S., Rautenberg, J., Ravel, O., Ravignani, D., Revenu, B., Ridky, J., Riggi, S., Risse, M., Ristori, P., Rizi, V., Roberts, J., de Carvalho, W. Rodrigues, Cabo, I. Rodriguez, Fernandez, G. Rodriguez, Rojo, J. Rodriguez, Rodríguez-Frías, M. D., Ros, G., Rosado, J., Rossler, T., Roth, M., Roulet, E., Rovero, A. C., Saffi, S. J., Saftoiu, A., Salamida, F., Salazar, H., Saleh, A., Greus, F. Salesa, Salina, G., Sánchez, F., Sanchez-Lucas, P., Santo, C. E., Santos, E., Santos, E. M., Sarazin, F., Sarkar, B., Sarmento, R., Sato, R., Scharf, N., Scherini, V., Schieler, H., Schiffer, P., Scholten, O., Schoorlemmer, H., Schovánek, P., Schulz, A., Schulz, J., Schumacher, J., Sciutto, S. J., Segreto, A., Settimo, M., Shadkam, A., Shellard, R. C., Sidelnik, I., Sigl, G., Sima, O., Śmiał, A., Šmída, R., Snow, G. R., Sommers, P., Sorokin, J., Squartini, R., Srivastava, Y. N., Stanič, S., Stapleton, J., Stasielak, J., Stephan, M., Stutz, A., Suarez, F., Suomijärvi, T., Supanitsky, A. D., Sutherland, M. S., Swain, J., Szadkowski, Z., Szuba, M., Taborda, O. A., Tapia, A., Tartare, M., Theodoro, V. M., Timmermans, C., Peixoto, C. J. Todero, Toma, G., Tomankova, L., Tomé, B., Tonachini, A., Elipe, G. Torralba, Machado, D. Torres, Travnicek, P., Trovato, E., Tueros, M., Ulrich, R., Unger, M., Urban, M., Galicia, J. F. Valdés, Valiño, I., Valore, L., van Aar, G., Berg, A. M. van den, van Velzen, S., van Vliet, A., Varela, E., Cárdenas, B. Vargas, Varner, G., Vázquez, J. R., Vázquez, R. A., Veberič, D., Verzi, V., Vicha, J., Videla, M., Villaseñor, L., Vlcek, B., Vorobiov, S., Wahlberg, H., Wainberg, O., Walz, D., Watson, A. A., Weber, M., Weidenhaupt, K., Weindl, A., Werner, F., Widom, A., Wiencke, L., Wilczyńska, B., Wilczyński, H., Will, M., Williams, C., Winchen, T., Wittkowski, D., Wundheiler, B., Wykes, S., Yamamoto, T., Yapici, T., Younk, P., Yuan, G., Yushkov, A., Zamorano, B., Zas, E., Zavrtanik, D., Zavrtanik, M., Zaw, I., Zepeda, A., Zhou, J., Zhu, Y., Silva, M. Zimbres, Ziolkowski, M., Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Anderson, R., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Chae, M. J., Cheon, B. G., Chiba, J., Chikawa, M., Cho, W. R., Fujii, T., Fukushima, M., Goto, T., Hanlon, W., Hayashi, Y., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kitamura, S., Kitamura, Y., Kuzmin, V., Kwon, Y. J., Lan, J., Lim, S. I., Lundquist, J. P., Machida, K., Martens, K., Matsuda, T., Matsuyama, T., Matthews, J. N., Minamino, M., Mukai, K., Myers, I., Nagasawa, K., Nagataki, S., Nakamura, T., Nonaka, T., Nozato, A., Ogio, S., Ogura, J., Ohnishi, M., Ohoka, H., Oki, K., Okuda, T., Ono, M., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sakurai, N., Sampson, A. L., Scott, L. M., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Smith, J. D., Sokolsky, P., Springer, R. W., Stokes, B. T., Stratton, S. R., Stroman, T. A., Suzawa, T., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Tsutsumi, K., Uchihori, Y., Udo, S., Urban, F., Vasiloff, G., Wong, T., Yamane, R., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoneda, Y., Yoshida, S., Yoshii, H., Zollinger, R., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Spherical harmonic moments are well-suited for capturing anisotropy at any scale in the flux of cosmic rays. An unambiguous measurement of the full set of spherical harmonic coefficients requires full-sky coverage. This can be achieved by combining data from observatories located in both the northern and southern hemispheres. To this end, a joint analysis using data recorded at the Telescope Array and the Pierre Auger Observatory above $10^{19}$ eV is presented in this work. The resulting multipolar expansion of the flux of cosmic rays allows us to perform a series of anisotropy searches, and in particular to report on the angular power spectrum of cosmic rays above $10^{19}$ eV. No significant deviation from isotropic expectations is found throughout the analyses performed. Upper limits on the amplitudes of the dipole and quadrupole moments are derived as a function of the direction in the sky, varying between 7% and 13% for the dipole and between 7% and 10% for a symmetric quadrupole., Comment: 33 pages, 13 figures, to appear in The Astrophysical Journal
Published: 2014
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47. Study of Ultra-High Energy Cosmic Ray Composition Using Telescope Array's Middle Drum Detector and Surface Array in Hybrid Mode

Author: Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Anderson, R., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Chae, M. J., Cheon, B. G., Chiba, J., Chikawa, M., Cho, W. R., Fujii, T., Fukushima, M., Goto, T., Hanlon, W., Hayashi, Y., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kitamura, S., Kitamura, Y., Kuzmin, V., Kwon, Y. J., Lan, J., Lim, S. I., Lundquist, J. P., Machida, K., Martens, K., Matsuda, T., Matsuyama, T., Matthews, J. N., Minamino, M., Mukai, Y., Myers, I., Nagasawa, K., Nagataki, S., Nakamura, T., Nonaka, T., Nozato, A., Ogio, S., Ogura, J., Ohnishi, M., Ohoka, H., Oki, K., Okuda, T., Ono, M., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sakurai, N., Sampson, A. L., Scott, L. M., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Smith, J. D., Sokolsky, P., Springer, R. W., Stokes, B. T., Stratton, S. R., Stroman, T., Suzawa, T., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Tsutsumi, K., Uchihori, Y., Udo, S., Urban, F., Vasiloff, G., Wong, T., Yamane, R., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoneda, Y., Yoshida, S., Yoshiia, H., Zollinger, R., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Previous measurements of the composition of Ultra-High Energy Cosmic Rays(UHECRs) made by the High Resolution Fly's Eye(HiRes) and Pierre Auger Observatory(PAO) are seemingly contradictory, but utilize different detection methods, as HiRes was a stereo detector and PAO is a hybrid detector. The five year Telescope Array(TA) Middle Drum hybrid composition measurement is similar in some, but not all, respects in methodology to PAO, and good agreement is evident between data and a light, largely protonic, composition when comparing the measurements to predictions obtained with the QGSJetII-03 and QGSJet-01c models. These models are also in agreement with previous HiRes stereo measurements, confirming the equivalence of the stereo and hybrid methods. The data is incompatible with a pure iron composition, for all models examined, over the available range of energies. The elongation rate and mean values of Xmax are in good agreement with Pierre Auger Observatory data. This analysis is presented using two methods: data cuts using simple geometrical variables and a new pattern recognition technique., Comment: 23 pages, 30 figures
Published: 2014
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48. A Northern Sky Survey for Point-Like Sources of EeV Neutral Particles with the Telescope Array Experiment

Author: Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Anderson, R., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Chae, M. J., Cheon, B. G., Chiba, J., Chikawa, M., Cho, W. R., Fujii, T., Fukushima, M., Goto, T., Hanlon, W., Hayashi, Y., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kitamura, S., Kitamura, Y., Kuzmin, V., Kwon, Y. J., Lan, J., Lim, S. I., Lundquist, J. P., Machida, K., Martens, K., Matsuda, T., Matsuyama, T., Matthews, J. N., Minamino, M., Mukai, K., Myers, I., Nagasawa, K., Nagataki, S., Nakamura, T., Nonaka, T., Nozato, A., Ogio, S., Ogura, J., Ohnishi, M., Ohoka, H., Oki, K., Okuda, T., Ono, M., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sakurai, N., Sampson, A. L., Scott, L. M., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Smith, J. D., Sokolsky, P., Springer, R. W., Stokes, B. T., Stratton, S. R., Stroman, T. A., Suzawa, T., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Tsutsumi, K., Uchihori, Y., Udo, S., Urban, F., Vasiloff, G., Wong, T., Yamane, R., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoneda, Y., Yoshida, S., Yoshii, H., Zollinger, R., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report on the search for steady point-like sources of neutral particles around 10$^{18}$ eV between 2008 May and 2013 May with the scintillator surface detector of the Telescope Array experiment. We found overall no significant point-like excess above 0.5 EeV in the northern sky. Subsequently, we also searched for coincidence with the Fermi bright Galactic sources. No significant coincidence was found within the statistical uncertainty. Hence, we set an upper limit on the neutron flux that corresponds to an averaged flux of 0.07 km$^{-2}$ yr$^{-1}$ for $E>1$ EeV in the northern sky at the 95% confidence level. This is the most stringent flux upper limit in a northern sky survey assuming point-like sources. The upper limit at the 95% confidence level on the neutron flux from Cygnus X-3 is also set to 0.2 km$^{-2}$ yr$^{-1}$ for $E>0.5$ EeV. This is an order of magnitude lower than previous flux measurements., Comment: 27 pages, 10 figures, 3 tables, accepted for publication in the Astrophysical Journal
Published: 2014
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49. Indications of Intermediate-Scale Anisotropy of Cosmic Rays with Energy Greater Than 57 EeV in the Northern Sky Measured with the Surface Detector of the Telescope Array Experiment

Author: The Telescope Array Collaboration, Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Anderson, R., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Chae, M. J., Cheon, B. G., Chiba, J., Chikawa, M., Cho, W. R., Fujii, T., Fukushima, M., Goto, T., Hanlon, W., Hayashi, Y., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kitamura, S., Kitamura, Y., Kuzmin, V., Kwon, Y. J., Lan, J., Lim, S. I., Lundquist, J. P., Machida, K., Martens, K., Matsuda, T., Matsuyama, T., Matthews, J. N., Minamino, M., Mukai, K., Myers, I., Nagasawa, K., Nagataki, S., Nakamura, T., Nonaka, T., Nozato, A., Ogio, S., Ogura, J., Ohnishi, M., Ohoka, H., Oki, K., Okuda, T., Ono, M., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sakurai, N., Sampson, A. L., Scott, L. M., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Smith, J. D., Sokolsky, P., Springer, R. W., Stokes, B. T., Stratton, S. R., Stroman, T. A., Suzawa, T., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Tsutsumi, K., Uchihori, Y., Udo, S., Urban, F., Vasiloff, G., Wong, T., Yamane, R., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoneda, Y., Yoshida, S., Yoshii, H., Zollinger, R., and Zundel, Z.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We have searched for intermediate-scale anisotropy in the arrival directions of ultrahigh-energy cosmic rays with energies above 57~EeV in the northern sky using data collected over a 5 year period by the surface detector of the Telescope Array experiment. We report on a cluster of events that we call the hotspot, found by oversampling using 20$^\circ$-radius circles. The hotspot has a Li-Ma statistical significance of 5.1$\sigma$, and is centered at R.A.=146.7$^{\circ}$, Dec.=43.2$^{\circ}$. The position of the hotspot is about 19$^{\circ}$ off of the supergalactic plane. The probability of a cluster of events of 5.1$\sigma$ significance, appearing by chance in an isotropic cosmic-ray sky, is estimated to be 3.7$\times$10$^{-4}$ (3.4$\sigma$)., Comment: 16 pages, 3 figures, accepted for publication in the ApJ Letters
Published: 2014
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50. Search for Ultra-High-Energy Neutrinos with the Telescope Array Surface Detector

Author: Abbasi, R. U., Abe, M., Abu-Zayyad, T., Allen, M., Azuma, R., Barcikowski, E., Belz, J. W., Bergman, D. R., Blake, S. A., Cady, R., Cheon, B. G., Chiba, J., Chikawa, M., di Matteo, A., Fujii, T., Fujita, K., Fujiwara, R., Fukushima, M., Furlich, G., Hanlon, W., Hayashi, M., Hayashi, Y., Hayashida, N., Hibino, K., Honda, K., Ikeda, D., Inoue, N., Ishii, T., Ishimori, R., Ito, H., Ivanov, D., Jeong, H. M., Jeong, S., Jui, C. C. H., Kadota, K., Kakimoto, F., Kalashev, O., Kasahara, K., Kawai, H., Kawakami, S., Kawana, S., Kawata, K., Kido, E., Kim, H. B., Kim, J. H., Kim, J. H., Kishigami, S., Kitamura, S., Kitamura, Y., Kuzmin, V., Kuznetsov, M., Kwon, Y. J., Lee, K. H., Lubsandorzhiev, B., Lundquist, J. P., Machida, K., Martens, K., Matsuyama, T., Matthews, J. N., Mayta, R., Minamino, M., Mukai, K., Myers, I., Nagasawa, K., Nagataki, S., Nakai, K., Nakamura, R., Nakamura, T., Nonaka, T., Oda, H., Ogio, S., Ogura, J., Ohnishi, M., Ohoka, H., Okuda, T., Omura, Y., Ono, M., Onogi, R., Oshima, A., Ozawa, S., Park, I. H., Pshirkov, M. S., Remington, J., Rodriguez, D. C., Rubtsov, G., Ryu, D., Sagawa, H., Sahara, R., Saito, K., Saito, Y., Sakaki, N., Sako, T., Sakurai, N., Scott, L. M., Seki, T., Sekino, K., Shah, P. D., Shibata, F., Shibata, T., Shimodaira, H., Shin, B. K., Shin, H. S., Smith, J. D., Sokolsky, P., Stokes, B. T., Stratton, S. R., Stroman, T. A., Suzawa, T., Takagi, Y., Takahashi, Y., Takamura, M., Takeda, M., Takeishi, R., Taketa, A., Takita, M., Tameda, Y., Tanaka, H., Tanaka, K., Tanaka, M., Tanoue, Y., Thomas, S. B., Thomson, G. B., Tinyakov, P., Tkachev, I., Tokuno, H., Tomida, T., Troitsky, S., Tsunesada, Y., Tsutsumi, K., Uchihori, Y., Udo, S., Urban, F., Wong, T., Yada, K., Yamamoto, M., Yamaoka, H., Yamazaki, K., Yang, J., Yashiro, K., Yoshii, H., Zhezher, Y., and Zundel, Z.
Published: 2020
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