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19 results on '"He, H H"'

1. An Updated Search of Steady TeV $\gamma-$Ray Point Sources in Northern Hemisphere Using the Tibet Air Shower Array

Author

Wang, Y., Bi, X. J., Cui, S. W., Ding, L. K., Danzengluobu, Ding, X. H., Fan, C., Feng, C. F., Feng, Zhaoyang, Feng, Z. Y., Gao, X. Y., Geng, Q. X., Guo, H. W., He, H. H., He, M., Hu, Haibing, Hu, H. B., Huang, Q., Jia, H. Y., Labaciren, Le, G. M., Li, A. F., Li, J. Y., Lou, Y. -Q., Lu, H., Lu, S. L., Meng, X. R., Mu, J., Ren, J. R., Tan, Y. H., Wang, B., Wang, H., Wang, Y. G., Wu, H. R., Xue, L., Yang, X. C., Ye, Z. H., Yu, G. C., Yuan, A. F., Zhang, H. M., Zhang, J. L., Zhang, N. J., Zhang, X. Y., Zhang, Y., Zhang, Yi, Zhaxisangzhu, Zhou, X. X., and Yuan, Q.

Subjects
Astrophysics
Abstract

Using the data taken from Tibet II High Density (HD) Array (1997 February-1999 September) and Tibet-III array (1999 November-2005 November), our previous northern sky survey for TeV $\gamma-$ray point sources has now been updated by a factor of 2.8 improved statistics. From $0.0^{\circ}$ to $60.0^{\circ}$ in declination (Dec) range, no new TeV $\gamma-$ray point sources with sufficiently high significance were identified while the well-known Crab Nebula and Mrk421 remain to be the brightest TeV $\gamma-$ray sources within the field of view of the Tibet air shower array. Based on the currently available data and at the 90% confidence level (C.L.), the flux upper limits for different power law index assumption are re-derived, which are approximately improved by 1.7 times as compared with our previous reported limits., Comment: This paper has been accepted by hepnp

Published
2008
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2. New estimation of the spectral index of high-energy cosmic rays as determined by the Compton-Getting anisotropy

Author

Amenomori, M., Bi, X. J., Chen, D., Cui, S. W., Danzengluobu, Ding, L. K., Ding, X. H., Fan, C., Feng, C. F., Feng, Zhaoyang, Feng, Z. Y., Gao, X. Y., Geng, Q. X., Guo, H. W., He, H. H., He, M., Hibino, K., Hotta, N., Hu, Haibing, Hu, H. B., Huang, J., Huang, Q., Jia, H. Y., Kajino, F., Kasahara, K., Katayose, Y., Kato, C., Kawata, K., Labaciren, Le, G. M., Li, A. F., Li, J. Y., Lou, Y. -Q., Lu, H., Lu, S. L., Meng, X. R., Mizutani, K., Mu, J., Munakata, K., Nagai, A., Nanjo, H., Nishizawa, M., Ohnishi, M., Ohta, I., Onuma, H., Ouchi, T., Ozawa, S., Ren, J. R., Saito, T., Saito, T. Y., Sakata, M., Sako, T. K., Shibata, M., Shiomi, A., Shirai, T., Sugimoto, H., Takita, M., Tan, Y. H., Tateyama, N., Torii, S., Tsuchiya, H., Udo, S., Wang, B., Wang, H., Wang, X., Wang, Y., Wang, Y. G., Wu, H. R., Xue, L., Yamamoto, Y., Yan, C. T., Yang, X. C., Yasue, S., Ye, Z. H., Yu, G. C., Yuan, A. F., Yuda, T., Zhang, H. M., Zhang, J. L., Zhang, N. J., Zhang, X. Y., Zhang, Y., Zhang, Yi, Zhaxisangzhu, and Zhou, X. X.

Subjects
Astrophysics
Abstract

The amplitude of the Compton-Getting (CG) anisotropy contains the power-law index of the cosmic-ray energy spectrum. Based on this relation and using the Tibet air-shower array data, we measure the cosmic-ray spectral index to be $-3.03 \pm 0.55_{stat} \pm < 0.62_{syst}$ between 6 TeV and 40 TeV, consistent with $-$2.7 from direct energy spectrum measurements. Potentially, this CG anisotropy analysis can be utilized to confirm the astrophysical origin of the ``knee'' against models for non-standard hadronic interactions in the atmosphere., Comment: accepted to ApJL

Published
2007
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3. Future plan for observation of cosmic gamma rays in the 100 TeV energy region with the Tibet air shower array : simulation and sensitivity

Author

Amenomori, M., Bi, X. J., Chen, D., Cui, S. W., Danzengluobu, Ding, L. K., Ding, X. H., Fan, C., Feng, C. F., Feng, Zhaoyang, Feng, Z. Y., Gao, X. Y., Geng, Q. X., Guo, H. W., He, H. H., He, M., Hibino, K., Hotta, N., Hu, Haibing, Hu, H. B., Huang, J., Huang, Q., Jia, H. Y., Kajino, F., Kasahara, K., Katayose, Y., Kato, C., Kawata, K., Labaciren, Le, G. M., Li, A. F., Li, J. Y., Lou, Y. -Q., Lu, H., Lu, S. L., Meng, X. R., Mizutani, K., Mu, J., Munakata, K., Nagai, A., Nanjo, H., Nishizawa, M., Ohnishi, M., Ohta, I., Onuma, H., Ouchi, T., Ozawa, S., Ren, J. R., Saito, T., Saito, T. Y., Sakata, M., Sako, T. K., Shibata, M., Shiomi, A., Shirai, T., Sugimoto, H., Takita, M., Tan, Y. H., Tateyama, N., Torii, S., Tsuchiya, H., Udo, S., Wang, B., Wang, H., Wang, X., Wang, Y., Wang, Y. G., Wu, H. R., Xue, L., Yamamoto, Y., Yan, C. T., Yang, X. C., Yasue, S., Ye, Z. H., Yu, G. C., Yuan, A. F., Yuda, T., Zhang, H. M., Zhang, J. L., Zhang, N. J., Zhang, X. Y., Zhang, Y., Zhang, Yi, Zhaxisangzhu, and Zhou, X. X.

Subjects
Astrophysics
Abstract

The Tibet air shower array, which has an effective area of 37,000 square meters and is located at 4300 m in altitude, has been observing air showers induced by cosmic rays with energies above a few TeV. We have a plan to add a large muon detector array to it for the purpose of increasing its sensitivity to cosmic gamma rays in the 100 TeV energy region by discriminating them from cosmic-ray hadrons. We have deduced the attainable sensitivity of the muon detector array using our Monte Carlo simulation. We report here on the detailed procedure of our Monte Carlo simulation., Comment: 4 pages, 5 figures, 30th International Cosmic Ray Conference

Published
2007

4. Future plan for observation of cosmic gamma rays in the 100 TeV energy region with the Tibet air shower array : physics goal and overview

Author

Amenomori, M., Bi, X. J., Chen, D., Cui, S. W., Danzengluobu, Ding, L. K., Ding, X. H., Fan, C., Feng, C. F., Feng, Zhaoyang, Feng, Z. Y., Gao, X. Y., Geng, Q. X., Guo, H. W., He, H. H., He, M., Hibino, K., Hotta, N., Hu, Haibing, Hu, H. B., Huang, J., Huang, Q., Jia, H. Y., Kajino, F., Kasahara, K., Katayose, Y., Kato, C., Kawata, K., Labaciren, Le, G. M., Li, A. F., Li, J. Y., Lou, Y. -Q., Lu, H., Lu, S. L., Meng, X. R., Mizutani, K., Mu, J., Munakata, K., Nagai, A., Nanjo, H., Nishizawa, M., Ohnishi, M., Ohta, I., Onuma, H., Ouchi, T., Ozawa, S., Ren, J. R., Saito, T., Saito, T. Y., Sakata, M., Sako, T. K., Shibata, M., Shiomi, A., Shirai, T., Sugimoto, H., Takita, M., Tan, Y. H., Tateyama, N., Torii, S., Tsuchiya, H., Udo, S., Wang, B., Wang, H., Wang, X., Wang, Y., Wang, Y. G., Wu, H. R., Xue, L., Yamamoto, Y., Yan, C. T., Yang, X. C., Yasue, S., Ye, Z. H., Yu, G. C., Yuan, A. F., Yuda, T., Zhang, H. M., Zhang, J. L., Zhang, N. J., Zhang, X. Y., Zhang, Y., Zhang, Yi, Zhaxisangzhu, and Zhou, X. X.

Subjects
Astrophysics
Abstract

The Tibet air shower array, which has an effective area of 37,000 square meters and is located at 4300 m in altitude, has been observing air showers induced by cosmic rays with energies above a few TeV. We are planning to add a large muon detector array to it for the purpose of increasing its sensitivity to cosmic gamma rays in the 100 TeV (10 - 1000 TeV) energy region by discriminating them from cosmic-ray hadrons. We report on the possibility of detection of gamma rays in the 100 TeV energy region in our field of view, based on the improved sensitivity of our air shower array deduced from the full Monte Carlo simulation., Comment: 4 pages, 3 figures, 30th International Cosmic Ray Conference

Published
2007

5. Peta-electron volt gamma-ray emission from the Crab Nebula

Author

The LHAASO Collaboration, Cao, Zhen, Aharonian, F., An, Q., Axikegu, Bai, L. X., Bai, Y. X., Bao, Y. W., Bastieri, D., Bi, X. J., Bi, Y. J., Cai, H., Cai, J. T., Cao, Zhe, Chang, J., Chang, J. F., Chen, B. M., Chen, E. S., Chen, J., Chen, Liang, Chen, Long, Chen, M. J., Chen, M. L., Chen, Q. H., Chen, S. H., Chen, S. Z., Chen, T. L., Chen, X. L., Chen, Y., Cheng, N., Cheng, Y. D., Cui, S. W., Cui, X. H., Cui, Y. D., Piazzoli, B. D'Ettorre, Dai, B. Z., Dai, H. L., Dai, Z. G., Danzengluobu, della Volpe, D., Dong, X. J., Duan, K. K., Fan, J. H., Fan, Y. Z., Fan, Z. X., Fang, J., Fang, K., Feng, C. F., Feng, L., Feng, S. H., Feng, Y. L., Gao, B., Gao, C. D., Gao, L. Q., Gao, Q., Gao, W., Ge, M. M., Geng, L. S., Gong, G. H., Gou, Q. B., Gu, M. H., Guo, F. L., Guo, J. G., Guo, X. L., Guo, Y. Q., Guo, Y. Y., Han, Y. A., He, H. H., He, H. N., He, J. C., He, S. L., He, X. B., He, Y., Heller, M., Hor, Y. K., Hou, C., Hou, X., Hu, H. B., Hu, S., Hu, S. C., Hu, X. J., Huang, D. H., Huang, Q. L., Huang, W. H., Huang, X. T., Huang, X. Y., Huang, Z. C., Ji, F., Ji, X. L., Jia, H. Y., Jiang, K., Jiang, Z. J., Jin, C., Ke, T., Kuleshov, D., Levochkin, K., Li, B. B., Li, Cheng, Li, Cong, Li, F., Li, H. B., Li, H. C., Li, H. Y., Li, Jie, Li, Jian, Li, K., Li, W. L., Li, X. R., Li, Xin, Li, Y., Li, Y. Z., Li, Zhe, Li, Zhuo, Liang, E. W., Liang, Y. F., Lin, S. J., Liu, B., Liu, C., Liu, D., Liu, H., Liu, H. D., Liu, J., Liu, J. L., Liu, J. S., Liu, J. Y., Liu, M. Y., Liu, R. Y., Liu, S. M., Liu, W., Liu, Y., Liu, Y. N., Liu, Z. X., Long, W. J., Lu, R., Lv, H. K., Ma, B. Q., Ma, L. L., Ma, X. H., Mao, J. R., Masood, A., Min, Z., Mitthumsiri, W., Montaruli, T., Nan, Y. C., Pang, B. Y., Pattarakijwanich, P., Pei, Z. Y., Qi, M. Y., Qi, Y. Q., Qiao, B. Q., Qin, J. J., Ruffolo, D., Rulev, V., S��iz, A., Shao, L., Shchegolev, O., Sheng, X. D., Shi, J. Y., Song, H. C., Stenkin, Yu. V., Stepanov, V., Su, Y., Sun, Q. N., Sun, X. N., Sun, Z. B., Tam, P. H. T., Tang, Z. B., Tian, W. W., Wang, B. D., Wang, C., Wang, H., Wang, H. G., Wang, J. C., Wang, J. S., Wang, L. P., Wang, L. Y., Wang, R. N., Wang, Wei, Wang, X. G., Wang, X. J., Wang, X. Y., Wang, Y., Wang, Y. D., Wang, Y. J., Wang, Y. P., Wang, Z. H., Wang, Z. X., Wang, Zhen, Wang, Zheng, Wei, D. M., Wei, J. J., Wei, Y. J., Wen, T., Wu, C. Y., Wu, H. R., Wu, S., Wu, W. X., Wu, X. F., Xi, S. Q., Xia, J., Xia, J. J., Xiang, G. M., Xiao, D. X., Xiao, G., Xiao, H. B., Xin, G. G., Xin, Y. L., Xing, Y., Xu, D. L., Xu, R. X., Xue, L., Yan, D. H., Yan, J. Z., Yang, C. W., Yang, F. F., Yang, J. Y., Yang, L. L., Yang, M. J., Yang, R. Z., Yang, S. B., Yao, Y. H., Yao, Z. G., Ye, Y. M., Yin, L. Q., Yin, N., You, X. H., You, Z. Y., Yu, Y. H., Yuan, Q., Zeng, H. D., Zeng, T. X., Zeng, W., Zeng, Z. K., Zha, M., Zhai, X. X., Zhang, B. B., Zhang, H. M., Zhang, H. Y., Zhang, J. L., Zhang, J. W., Zhang, L. X., Zhang, Li, Zhang, Lu, Zhang, P. F., Zhang, P. P., Zhang, R., Zhang, S. R., Zhang, S. S., Zhang, X., Zhang, X. P., Zhang, Y. F., Zhang, Y. L., Zhang, Yi, Zhang, Yong, Zhao, B., Zhao, J., Zhao, L., Zhao, L. Z., Zhao, S. P., Zheng, F., Zheng, Y., Zhou, B., Zhou, H., Zhou, J. N., Zhou, P., Zhou, R., Zhou, X. X., Zhu, C. G., Zhu, F. R., Zhu, H., Zhu, K. J., and Zuo, X.

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Nebula, Multidisciplinary, 010308 nuclear & particles physics, Crab Pulsar, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Electron, Astrophysics, 01 natural sciences, Luminosity, Rotational energy, Crab Nebula, Pulsar, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract

The Crab pulsar and the surrounding nebula powered by the pulsar's rotational energy through the formation and termination of a relativistic electron-positron wind is a bright source of gamma-rays carrying crucial information about this complex conglomerate. We report the detection of $\gamma$-rays with a spectrum showing gradual steepening over three energy decades, from $5\times 10^{-4}$ to $1.1$ petaelectronvolt (PeV). The ultra-high-energy photons exhibit the presence of a PeV electron accelerator (a pevatron) with an acceleration rate exceeding 15% of the absolute theoretical limit. Assuming that unpulsed $\gamma$-rays are produced at the termination of the pulsar's wind, we constrain the pevatron's size, between $0.025$ and $0.1$ pc, and the magnetic field $\approx 110 \mu$G. The production rate of PeV electrons, $2.5 \times 10^{36}$ erg $\rm s^{-1}$, constitutes 0.5% of the pulsar's spin-down luminosity, although we do not exclude a non-negligible contribution of PeV protons to the production of the highest energy $\gamma$-rays., Comment: 43 pages, 13 figures, 2 tables; Published in Science

Published
2021

6. Knee of the cosmic hydrogen and helium spectrum below 1 PeV measured by ARGO-YBJ and a Cherenkov telescope of LHAASO

Author

Bartoli, B., Bernardini, P., Bi, X. J., Branchini, P., Budano, A., Camarri, P., Cao, Z., Cardarelli, R., Catalanotti, S., Chen, S. Z., Chen, T. L., Creti, P., Cui, S. W., Dai, B. Z., D Amone, A., Danzengluobu, Mitri, I., D Ettorre Piazzoli, B., Di Girolamo, T., Di Sciascio, G., Feng, C. F., Feng, Zhaoyang, Feng, Zhenyong, Gou, Q. B., Guo, Y. Q., He, H. H., Hu, Haibing, Hu, Hongbo, Iacovacci, M., Iuppa, R., Jia, H. Y., Labaciren, Li, H. J., Liguori, G., Liu, C., Liu, J., Liu, M. Y., Lu, H., Ma, L. L., Ma, X. H., Mancarella, G., Mari, S. M., Marsella, G., Martello, D., Mastroianni, S., Montini, P., Ning, C. C., Panareo, M., Perrone, L., Pistilli, P., Ruggieri, F., Salvini, P., Santonico, R., Shen, P. R., Sheng, X. D., Shi, F., Surdo, A., Tan, Y. H., Piero Vallania, Vernetto, S., Vigorito, C., Wang, H., Wu, C. Y., Wu, H. R., Xue, L., Yang, Q. Y., Yang, X. C., Yao, Z. G., Yuan, A. F., Zha, M., Zhang, H. M., Zhang, L., Zhang, X. Y., Zhang, Y., Zhao, J., Zhaxiciren, Zhaxisangzhu, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., Zizzi, G., Bai, Y. X., Chen, M. J., Chen, Y., Feng, S. H., Gao, B., Gu, M. H., Hou, C., Li, X. X., Liu, J. L., Wang, X., Xiao, G., Zhang, B. K., Zhang, S. S., Zhou, B., Zuo, X., Bartoli, B., Bernardini, P., Bi, X. J., Cao, Z., Catalanotti, S., Chen, S. Z., Chen, T. L., Cui, S. W., Dai, B. Z., D'Amone, A., Danzengluobu, Null, De Mitri, I., D'Ettorre Piazzoli, B., Di Girolamo, T., Di Sciascio, G., Feng, C. F., Feng, Zhaoyang, Feng, Zhenyong, Guo, Q. B., Guo, Y. Q., He, H. H., Hu, Haibing, Hu, Hongbo, Iacovacci, M., Iuppa, R., Jia, H. Y., Labaciren, Null, Li, H. J., Liu, C., Liu, J., Liu, M. Y., Lu, H., Ma, L. L., Ma, X. H., Mancarella, G., Mari, S. M., Marsella, G., Mastroianni, S., Montini, P., Ning, C. C., Perrone, L., Pistilli, P., Salvini, P., Santonico, R., Shen, P. R., Sheng, X. D., Shi, F., Surdo, A., Tan, Y. H., Vallania, P., Vernetto, S., Vigorito, C., Wang, H., Wu, C. Y., Wu, H. R., Xue, L., Yang, Q. Y., Yang, X. C., Yao, Z. G., Yuan, A. F., Zha, M., Zhang, H. M., Zhang, L., Zhang, X. Y., Zhang, Y., Zhao, J., Zhaxiciren, Null, Zhaxisangzhu, Null, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., Bai, Y. X., Chen, M. J., Feng, S. H., Gao, B., Gu, M. H., Hou, C., Liu, J. L., Wang, X., Xiao, G., Zhang, B. K., Zhang, S. S., Zhou, B., Zuo, X., ITA, Bartoli, Bruno, Bi, X. . j., Catalanotti, Sergio, Chen, S. . z., Chen, T. . l., Cui, S. . w., Dai, B. z, D’Amone, A., D'ETTORRE PIAZZOLI, Benedetto, DI GIROLAMO, Tristano, Feng, C. . f., Guo, Q. . b., Guo, Y. . q., He, H. . h., Iacovacci, Michele, Jia, H. . y., Li, H. . j., Liu, M. . y., Ma, L. . l., Ma, X. . h., Mari, S. . m., Ning, C. . c., Shen, P. . r., Sheng, X. . d., Tan, Y. . h., Wu, C. . y., Wu, H. . r., Yang, Q. . y., Yang, X. . c., Yao, Z. . g., Yuan, A. . f., Zhang, H. . m., Zhang, X. . y., Zhou, X. . x., Zhu, F. . r., Zhu, Q. . q., Bai, Y. . x., Chen, M. . j., Feng, S. . h., Gu, M. . h., Liu, J. . l., Zhang, B. . k., Zhang, S. . s., B., Bartoli, P., Bernardini, X. J., Bi, Z., Cao, S., Catalanotti, S. Z., Chen, T. L., Chen, S. W., Cui, B. Z., Dai, D, A., ’, Amone, Danzengluobu, I. De, Mitri, D, B., Ettorre, Piazzoli, T. Di, Girolamo, G. Di, Sciascio, C. F., Feng, Zhaoyang, Feng, Zhenyong, Feng, Q. B., Guo, Y. Q., Guo, H. H., He, Haibing, Hu, Hongbo, Hu, M., Iacovacci, R., Iuppa, H. Y., Jia, Labaciren, H. J., Li, C., Liu, J., Liu, M. Y., Liu, H., Lu, L. L., Ma, X. H., Ma, G., Mancarella, Mari, Stefano Maria, G., Marsella, S., Mastroianni, Montini, Paolo, C. C., Ning, L., Perrone, P., Pistilli, P., Salvini, R., Santonico, P. R., Shen, X. D., Sheng, F., Shi, A., Surdo, Y. H., Tan, P., Vallania, S., Vernetto, C., Vigorito, H., Wang, C. Y., Wu, H. R., Wu, L., Xue, Q. Y., Yang, X. C., Yang, Z. G., Yao, A. F., Yuan, M., Zha, H. M., Zhang, L., Zhang, X. Y., Zhang, Y., Zhang, J., Zhao, Zhaxiciren, Zhaxisangzhu, X. X., Zhou, F. R., Zhu, Q. Q., Zhu, Y. X., Bai, M. J., Chen, S. H., Feng, B., Gao, M. H., Gu, C., Hou, J. L., Liu, X., Wang, G., Xiao, B. K., Zhang, S. S., Zhang, B., Zhou, and Collaboratio, (LHAASO

Subjects
Nuclear and High Energy Physics, Proton, Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, FOS: Physical sciences, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmic Ray, Helium, Spectral line, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), 0103 physical sciences, 010303 astronomy & astrophysics, Cherenkov radiation, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectral index, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, 13. Climate action, Production (computer science), Astrophysics - High Energy Astrophysical Phenomena, Energy (signal processing), proton
Abstract

The measurement of the cosmic ray energy spectrum, in particular for individual species of nuclei, is an important tool to investigate cosmic ray production and propagation mechanisms. The determination of the ``knees'' in the spectra of different species remains one of the main challenges in cosmic ray physics. In fact, experimental results are still conflicting. In this paper we report a measurement of the mixed proton and helium energy spectrum, obtained with the combined data of the ARGO-YBJ experiment and a wide field of view Cherenkov telescope, a prototype of the future LHAASO experiment. By means of a multiparameter technique, we have selected a high-purity proton plus helium sample. The reconstructed energy resolution is found to be about 25% throughout the investigated energy range from 100 TeV to 3 PeV, with a systematic uncertainty in the absolute energy scale of 9.7%. The found energy spectrum can be fitted with a broken power-law function, with a break at the energy ${\mathrm{E}}_{k}=700\ifmmode\pm\else\textpm\fi{}230(\mathrm{stat})\ifmmode\pm\else\textpm\fi{}70(\mathrm{sys})\text{ }\text{ }\mathrm{TeV}$, where the spectral index changes from $\ensuremath{-}2.56\ifmmode\pm\else\textpm\fi{}0.05$ to $\ensuremath{-}3.24\ifmmode\pm\else\textpm\fi{}0.36$. The statistical significance of the observed spectral break is 4.2 standard deviations.

Published
2015

7. Search for Gamma-Ray Bursts with the ARGO-YBJ Detector in Shower Mode

Author

Bartoli, B., Bernardini, P., Bi, X. J., Cao, Z., Catalanotti, S., Chen, S. Z., Chen, T. L., Cui, S. W., Dai, B. Z., D'Amone, A., Danzengluobu, De Mitri, I., D'Ettorre Piazzoli, B., Di Girolamo, T., Di Sciascio, G., Feng, C. F., Feng, Zhaoyang, Feng, Zhenyong, Gao, W., Gou, Q. B., Guo, Y. Q., He, H. H., Hu, Haibing, Hu, Hongbo, Iacovacci, M., Iuppa, R., Jia, H. Y., Labaciren, Li, H. J., Liu, C., Liu, J., Liu, M. Y., Lu, H., Ma, L. L., Ma, X. H., Mancarella, G., Mari, S. M., Marsella, G., Mastroianni, S., Montini, P., Ning, C. C., Perrone, L., Pistilli, P., Salvini, P., Santonico, R., Shen, P. R., Sheng, X. D., Shi, F., Surdo, A., Tan, Y. H., VALLANIA, PIERO, VERNETTO, Silvia Teresa, Vigorito, C., Wang, H., Wu, C. Y., Wu, H. R., Xue, L., Yang, Q. Y., Yang, X. C., Yao, Z. G., Yuan, A. F., Zha, M., Zhang, H. M., Zhang, L., Zhang, X. Y., Zhang, Y., Zhao, J., Zhaxiciren, Zhaxisangzhu, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., ARGO-YBJ Collaboration, Bartoli, B., Bernardini, P., Bi, X. J., Cao, Z., Catalanotti, S., Chen, S. Z., Chen, T. L., Cui, S. W., Dai, B. Z., D'Amone, A., Danzengluobu, Null, Mitri, I. De, Piazzoli, B. D'Ettorre, Di Girolamo, T., Sciascio, G. Di, Feng, C. F., Feng, Zhaoyang, Feng, Zhenyong, Gao, W., Gou, Q. B., Guo, Y. Q., He, H. H., Hu, Haibing, Hu, Hongbo, Iacovacci, M., Iuppa, R., Jia, H. Y., Labaciren, Null, Li, H. J., Liu, C., Liu, J., Liu, M. Y., Lu, H., Ma, L. L., Ma, X. H., Mancarella, G., Mari, S. M., Marsella, G., Mastroianni, S., Montini, P., Ning, C. C., Perrone, L., Pistilli, P., Salvini, P., Santonico, R., Shen, P. R., Sheng, X. D., Shi, F., Surdo, A., Tan, Y. H., Vallania, P., Vernetto, S., Vigorito, C., Wang, H., Wu, C. Y., Wu, H. R., Xue, L., Yang, Q. Y., Yang, X. C., Yao, Z. G., Yuan, A. F., Zha, M., Zhang, H. M., Zhang, L., Zhang, X. Y., Zhang, Y., Zhao, J., Zhaxiciren, Null, Zhaxisangzhu, Null, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., and Girolamo, T. Di

Subjects
Astrophysics and Astronomy, gamma-ray burst: general, FOS: Physical sciences, Field of view, Cosmic ray, Astrophysics, general [gamma-ray burst], 7. Clean energy, 01 natural sciences, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010303 astronomy & astrophysics, Particle Physics - Phenomenology, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Physics, 010308 nuclear & particles physics, Detector, Gamma ray, hep-ph, Astronomy and Astrophysics, Gamma-ray astronomy, Astronomy and Astrophysic, Redshift, High Energy Physics - Phenomenology, Air shower, 13. Climate action, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst
Abstract

The ARGO-YBJ detector, located at the Yangbajing Cosmic Ray Laboratory (4300 m a. s. l., Tibet, China), was a full coverage air shower array dedicated to gamma ray astronomy and cosmic ray studies. The wide field of view (~ 2 sr) and high duty cycle (> 86%), made ARGO-YBJ suitable to search for short and unexpected gamma ray emissions like gamma ray bursts (GRBs). Between 2007 November 6 and 2013 February 7, 156 satellite-triggered GRBs (24 of them with known redshift) occurred within the ARGO-YBJ field of view. A search for possible emission associated to these GRBs has been made in the two energy ranges 10-100 GeV and 10-1000 GeV. No significant excess has been found in time coincidence with the satellite detections nor in a time window of one hour after the bursts. Taking into account the EBL absorption, upper limits to the energy fluence at 99% of confidence level have been evaluated,with values ranging from ~ 10-5 erg cm-2 to ~10-1 erg cm-2., 24pages and 12 figures

Published
2017
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8. Long-term monitoring of the TeV emission from Mrk 421 with the ARGO-YBJ experiment

Author

Collaboration, The ARGO-YBJ, Bartoli, B., Bernardini, P., Bi, X. J., Bleve, C., Bolognino, I., Branchini, P., Budano, A., Melcarne, A. K. Calabrese, Camarri, P., Cao, Z., Cappa, A., Cardarelli, R., Catalanotti, S., Cattaneo, C., Celio, P., Chen, S. Z., Chen, T. L., Chen, Y., Creti, P., Cui, S. W., Dai, B. Z., Staiti, G. D'Alí, Danzengluobu, Dattoli, M., De Mitri, I., Piazzoli, B. D'Ettorre, Di Girolamo, T., Ding, X. H., Di Sciascio, G., Feng, C. F., Feng, Zhaoyang, Feng, Zhenyong, Galeazzi, F., Galeotti, P., Giroletti, E., Gou, Q. B., Guo, Y. Q., He, H. H., Hu, Haibing, Hu, Hongbo, Huang, Q., Iacovacci, M., Iuppa, R., James, I., Jia, H. Y., Labaciren, Li, H. J., Li, J. Y., Li, X. X., Liguori, G., Liu, C., Liu, C. Q., Liu, J., Liu, M. Y., Lu, H., Ma, X. H., Mancarella, G., Mari, S. M., Marsella, G., Martello, D., Mastroianni, S., Montini, P., Ning, C. C., Pagliaro, A., Panareo, M., Panico, B., Perrone, L., Pistilli, P., Qu, X. B., Rossi, E., Ruggieri, F., Salvini, P., Santonico, R., Shen, P. R., Sheng, X. D., Shi, F., Stanescu, C., Surdo, A., Tan, Y. H., Vallania, P., Vernetto, S., Vigorito, C., Wang, B., Wang, H., Wu, C. Y., Wu, H. R., Xu, B., Xue, L., Yan, Y. X., Yang, Q. Y., Yang, X. C., Yao, Z. G., Yuan, A. F., Zha, M., Zhang, H. M., Zhang, Jilong, Zhang, Jianli, Zhang, L., Zhang, P., Zhang, X. Y., Zhang, Y., Zhaxiciren, Zhaxisangzhu, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., Zizzi, G., Bartoli, Bruno, Catalanotti, Sergio, D'ETTORRE PIAZZOLI, Benedetto, DI GIROLAMO, Tristano, Iacovacci, Michele, Bartoli, B, Bernardini, P, Bi, XJ, Bleve, C, Bolognino, I, Branchini, P, Budano, A, Calabrese Melcarne, AK, Camarri, P, Cao, Z, Cappa, A, Cardarelli, R, Catalanotti, S, Cattaneo, C, Celio, P, Chen, SZ, Chen, TL, Chen, Y, Creti, P, Cui SW, Dai, BZ, D'Alí Staiti, G, Danzengluobu, Dattoli, M, De Mitri, I, D'Ettorre Piazzoli, B, Di Girolamo, T, Ding, XH, Di Sciascio, G, Feng CF, Feng, XYa, Feng, ZYo, Galeazzi, F, Galeotti, P, Giroletti, E, Gou, QB, Guo, YQ, He, HH, Hu, HBi, Hu, HBo, Huang, Q, Iacovacci, M, Iuppa, R, James, I, Jia, HY, Labaciren, Li, HJ, Li, JY, Li, XX, Liguori, G, Liu, C, Liu, CQ, Liu, J, Liu, MY, Lu, H, Ma, XH, Mancarella, G, Mari, SM, Marsella, G, Martello, D, Mastroianni, S, Montini, P, Ning, CC, Pagliaro, A, Panareo, M, Panico, B, Perrone, L, Pistilli, P, Qu, XB, Rossi, E, Ruggieri, F, Salvini, P, Santonico, R, Shen, PR, Sheng, XD, Shi, F, Stanescu, C, Surdo, A, Tan, YH, Vallania, P, Vernetto, S, Vigorito, C, Wang, B, Wang, H, Wu, CY, Wu, HR, Xu, B, Xue, L, Yan, YX, Yang, QY, Yang, XC, Yao, ZG, Yuan, AF, Zha, M, Zhang, HM, Zhang, JLo, Zhang,JLi, Zhang,L, Zhang, P, Zhang, XY, Zhang, Y, Zhaxiciren, Zhaxisangzhu, Zhou, XX, Zhu, FR, Zhu, QQ, Zizzi, G, Bi, Xj, Melcarne, Akc, Chen, Sz, Chen, Tl, Cui, Sw, Dai, Bz, Staiti, Gd, Piazzoli, Bd, Ding, Xh, Feng, Cf, Feng, Zy, Gou, Qb, Guo, Yq, He, Hh, Hu, Hb, Jia, Hy, Li, Hj, Li, Jy, Li, Xx, Liu, Cq, Liu, My, Ma, Xh, Mari, Stefano Maria, Ning, Cc, Qu, Xb, Shen, Pr, Sheng, Xd, Tan, Yh, Wu, Cy, Wu, Hr, Yan, Yx, Yang, Qy, Yang, Xc, Yao, Zg, Yuan, Af, Zhang, Hm, Zhang, Jl, Zhang, L, Zhang, Xy, Zhaxiciren, Zhaxisangzhu, Zhou, Xx, Zhu, Fr, Zhu, Qq, and Zizzi, G.

Subjects
media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Oggetti di tipo BL Lacertae, FOS: Physical sciences, Flux, Astrophysics, 01 natural sciences, 7. Clean energy, individual (Markarian 421) [BL Lacertae objects], Spectral line, Gamma-rays, Markarian 421, BL Lacertae, Resistive Plate Chambers, law.invention, law, 0103 physical sciences, Radiative transfer, 010303 astronomy & astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Markarian 421, Settore FIS/01 - Fisica Sperimentale, Astronomy and Astrophysics, general [gamma ray], Synchrotron, 3. Good health, Air shower, 13. Climate action, Space and Planetary Science, Duty cycle, Sky, Raggi gamma, Spectral energy distribution, Astrophysics - High Energy Astrophysical Phenomena
Abstract

ARGO-YBJ is an air shower detector array with a fully covered layer of resistive plate chambers. It is operated with a high duty cycle and a large field of view. It continuously monitors the northern sky at energies above 0.3 TeV. In this paper, we report a long-term monitoring of Mrk 421 over the period from 2007 November to 2010 February. This source was observed by the satellite-borne experiments Rossi X-ray Timing Explorer and Swift in the X-ray band. Mrk 421 was especially active in the first half of 2008. Many flares are observed in both X-ray and gamma-ray bands simultaneously. The gamma-ray flux observed by ARGO-YBJ has a clear correlation with the X-ray flux. No lag between the X-ray and gamma-ray photons longer than 1 day is found. The evolution of the spectral energy distribution is investigated by measuring spectral indices at four different flux levels. Hardening of the spectra is observed in both X-ray and gamma-ray bands. The gamma-ray flux increases quadratically with the simultaneously measured X-ray flux. All these observational results strongly favor the synchrotron self-Compton process as the underlying radiative mechanism., 30 pages, 8 figures

Published
2011

9. Search for GeV Gamma-Ray Bursts with the ARGO-YBJ Detector in Scaler Mode.

Author

Li, X. X., He, H. H., Zhu, F. R., and Chen, S. Z.

Subjects
*GAMMA ray bursts, *DETECTORS, *TELESCOPES, *ASTROPHYSICS, *ARTIFICIAL satellites
Abstract

The ARGO-YBJ experiment is a full coverage array made of Resistive Plate Chambers (RPCs) operated in streamer mode to detect the extensive array showers (EASs). With large field of view (>2sr) and high duty cycle (>90%), the ARGO-YBJ detector is the right ground-based apparatus to detect VHE GRBs, while the high altitude (4300 m a.s.l) and scaler working mode enable it to detect GRBs in the GeV region as high energy follow-up observation of satellites such as SWIFT. If a GRB signal is detected, the four scaler channels, which correspond to different energy thresholds, can provide further information on the energy spectrum and its cut-off. More than 40 SWIFT GRBs were in ARGO-YBJ field of view, no significant excess was detected till now. [ABSTRACT FROM AUTHOR]

Published
2008
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10. Underground water Cherenkov muon detector array with the Tibet air shower array for gamma-ray astronomy in the 100 TeV region.

Author

Paredes, Josep M., Reimer, Olaf, Torres, Diego F., Amenomori, M., Ayabe, S., Bi, X. J., Chen, D., Cui, S. W., Danzengluobu, Ding, L. K., Ding, X. H., Feng, C. F., Zhaoyang Feng, Feng, Z. Y., Gao, X. Y., Geng, Q. X., Guo, H. W., He, H. H., He, M., and Hibino, K.

Abstract

We propose to build a large water-Cherenkov-type muon-detector array (Tibet MD array) around the 37 000 m2 Tibet air shower array (Tibet AS array) already constructed at 4300 m above sea level in Tibet, China. Each muon detector is a waterproof concrete pool, 6 m wide × 6 m long × 1.5 m deep in size, equipped with a 20 inch-in-diameter PMT. The Tibet MD array consists of 240 muon detectors set up 2.5 m underground. Its total effective area will be 8640 m2 for muon detection. The Tibet MD array will significantly improve gamma-ray sensitivity of the Tibet AS array in the 100 TeV region (10-1000 TeV) by means of gamma/hadron separation based on counting the number of muons accompanying an air shower. The Tibet AS+MD array will have the sensitivity to gamma rays in the 100 TeV region by an order of magnitude better than any other previous existing detectors in the world. [ABSTRACT FROM AUTHOR]

Published
2007
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11. The cosmic ray proton plus helium energy spectrum measured by the ARGO-YBJ experiment in the energy range 3-300 TeV

Author

Argo-Ybj, The Collaboration, Bartoli, B., Bernardini, P., Bi, X. J., Cao, Z., Catalanotti, S., Chen, S. Z., Chen, T. L., Cui, S. W., Dai, B. Z., D Amone, A., Danzengluobu, Mitri, I., D Ettorre Piazzoli, B., Di Girolamo, T., Di Sciascio, G., Feng, C. F., Feng, Zhaoyang, Feng, Zhenyong, Gou, Q. B., Guo, Y. Q., He, H. H., Hu, Haibing, Hu, Hongbo, Iacovacci, M., Iuppa, R., Jia, H. Y., Labaciren, Li, H. J., Liu, C., Liu, J., Liu, M. Y., Lu, H., Ma, L. L., Ma, X. H., Mancarella, G., Mari, S. M., Marsella, G., Mastroianni, S., Montini, P., Ning, C. C., Perrone, L., Pistilli, P., Salvini, P., Santonico, R., Settanta, G., Shen, P. R., Sheng, X. D., Shi, F., Surdo, A., Tan, Y. H., Piero Vallania, Vernetto, S., Vigorito, C., Wang, H., Wu, C. Y., Wu, H. R., Xue, L., Yang, Q. Y., Yang, X. C., Yao, Z. G., Yuan, A. F., Zha, M., Zhang, H. M., Zhang, L., Zhang, X. Y., Zhang, Y., Zhao, J., Zhaxiciren, Zhaxisangzhu, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., Bartoli, B., Bernardini, P., Bi, X. J., Cao, Z., Catalanotti, S., Chen, S. Z., Chen, T. L., Cui, S. W., Dai, B. Z., D'Amone, A., Danzengluobu, De Mitri, I., D'Ettorre Piazzoli, B., Di Girolamo, T., Di Sciascio, G., Feng, C. F., Feng, Z., Gou, Q. B., Guo, Y. Q., He, H. H., Hu, H., Iacovacci, M., Iuppa, R., Jia, H. Y., Labaciren, Li, H. J., Liu, C., Liu, J., Liu, M. Y., Lu, H., Ma, L. L., Ma, X. H., Mancarella, G., Mari, S. M., Marsella, G., Mastroianni, S., Montini, P., Ning, C. C., Perrone, L., Pistilli, P., Salvini, P., Santonico, R., Settanta, G., Shen, P. R., Sheng, X. D., Shi, F., Surdo, A., Tan, Y. H., Vallania, P., Vernetto, S., Vigorito, C., Wang, H., Wu, C. Y., Wu, H. R., Xue, L., Yang, Q. Y., Yang, X. C., Yao, Z. G., Yuan, A. F., Zha, M., Zhang, H. M., Zhang, L., Zhang, X. Y., Zhang, Y., Zhao, J., Zhaxiciren, Zhaxisangzhu, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., B., Bartoli, Bernardini, Paolo, X. . J., Bi, Z., Cao, S., Catalanotti, Chen, S. . Z., Chen, T. . L., Cui, S. . W., Dai, B. . Z., A., D’Amone, DE MITRI, Ivan, B., D’Ettorre Piazzoli, T., Di Girolamo, G., Di Sciascio, Feng, C. . F., Zhaoyang, Feng, Zhenyong, Feng, Gou, Q. . B., Guo, Y. . Q., H. . H., He, Haibing, Hu, Hongbo, Hu, M., Iacovacci, R., Iuppa, Jia, H. . Y., H. . J., Li, C., Liu, J., Liu, Liu, M. . Y., H., Lu, L. . L., Ma, X. . H., Ma, Mancarella, Giovanni, Mari, S. . M., Marsella, Giovanni, S., Mastroianni, P., Montini, Ning, C. . C., Perrone, Lorenzo, P., Pistilli, P., Salvini, R., Santonico, G., Settanta, Shen, P. . R., Sheng, X. . D., F., Shi, A., Surdo, Tan, Y. . H., P., Vallania, S., Vernetto, C., Vigorito, H., Wang, C. . Y., Wu, H. . R., Wu, L., Xue, Yang, Q. . Y., Yang, X. . C., Yao, Z. . G., Yuan, A. . F., M., Zha, Zhang, H. . M., L., Zhang, Zhang, X. . Y., Y., Zhang, J., Zhao, Zhou, X. . X., Zhu, F. . R., Zhu, Q. . Q., B. Bartoli, BERNARDINI, Paolo, X. .J. Bi, Z. Cao, S. Catalanotti, S. .Z. Chen, T. .L. Chen, S. .W. Cui, B. .Z. Dai, A. D’Amone, B. D’Ettorre Piazzoli, T. Di Girolamo, G. Di Sciascio, C. .F. Feng, Zhaoyang Feng, Zhenyong Feng, Q. .B. Gou, Y. .Q. Guo, H. .H. He, Haibing Hu, Hongbo Hu, M. Iacovacci, R. Iuppa, H. .Y. Jia, H. .J. Li, C. Liu, J. Liu, M. .Y. Liu, H. Lu, L. .L. Ma, X. .H. Ma, MANCARELLA, Giovanni, S. .M. Mari, MARSELLA, GIOVANNI, S. Mastroianni, P. Montini, C. .C. Ning, PERRONE, Lorenzo, P. Pistilli, P. Salvini, R. Santonico, G. Settanta, P. .R. Shen, X. .D. Sheng, F. Shi, A. Surdo, Y. .H. Tan, P. Vallania, S. Vernetto, C. Vigorito, H. Wang, C. .Y. Wu, H. .R. Wu, L. Xue, Q. .Y. Yang, X. .C. Yang, Z. .G. Yao, A. .F. Yuan, M. Zha, H. .M. Zhang, L. Zhang, X. .Y. Zhang, Y. Zhang, J. Zhao, X. .X. Zhou, F. .R. Zhu, Q. .Q. Zhu, Bartoli, Bruno, Bi, X. . j., Catalanotti, Sergio, Chen, S. . z., Chen, T. . l., Cui, S. . w., Dai, B. . z., D’Amone, A., Danzengluobu, Null, D'ETTORRE PIAZZOLI, Benedetto, DI GIROLAMO, Tristano, Feng, C. . f., Feng, Zhaoyang, Feng, Zhenyong, Gou, Q. . b., Guo, Y. . q., He, H. . h., Hu, Haibing, Hu, Hongbo, Iacovacci, Michele, Jia, H. . y., Labaciren, Null, Li, H. . j., Liu, M. . y., Ma, L. . l., Ma, X. . h., Mari, S. . m., Ning, C. . c., Shen, P. . r., Sheng, X. . d., Tan, Y. . h., Wu, C. . y., Wu, H. . r., Yang, Q. . y., Yang, X. . c., Yao, Z. . g., Yuan, A. . f., Zhang, H. . m., Zhang, X. . y., Zhaxiciren, Null, Zhaxisangzhu, Null, Zhou, X. . x., Zhu, F. . r., Zhu, Q. . q., Mari, Stefano Maria, The ARGO YBJ, Collaboration, and ITA

Subjects
Nuclear and High Energy Physics, PARTICLE-ACCELERATION, Physics and Astronomy (miscellaneous), Proton, Astrophysics::High Energy Astrophysical Phenomena, SHELL, FOS: Physical sciences, Cosmic ray, Astrophysics, 01 natural sciences, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), Observatory, 0103 physical sciences, Ultra-high-energy cosmic ray, 010306 general physics, Cosmic-ray observatory, DETECTOR, Nuclear and High Energy Physic, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), AIR-SHOWERS, Spectral index, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, Air shower, 13. Climate action, SUPERNOVA REMNANT, High Energy Physics::Experiment, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The ARGO-YBJ experiment is a full-coverage air shower detector located at the Yangbajing Cosmic Ray Observatory (Tibet, People's Republic of China, 4300 m a.s.l.). The high altitude, combined with the full-coverage technique, allows the detection of extensive air showers in a wide energy range and offer the possibility of measuring the cosmic ray proton plus helium spectrum down to the TeV region, where direct balloon/space-borne measurements are available. The detector has been in stable data taking in its full configuration from November 2007 to February 2013. In this paper the measurement of the cosmic ray proton plus helium energy spectrum is presented in the region 3-300 TeV by analyzing the full collected data sample. The resulting spectral index is $\gamma = -2.64 \pm 0.01$. These results demonstrate the possibility of performing an accurate measurement of the spectrum of light elements with a ground based air shower detector., Comment: 18 pages, 8 figures, preprint submitted to Phys. Rev. D

12. TeV gamma-ray survey of the Northern sky using the ARGO-YBJ detector

Author

Argo-Ybj, The Collaboration, Bartoli, B., Bernardini, P., Bi, X. J., Bolognino, I., Branchini, P., Budano, A., Calabrese Melcarne, A. K., Camarri, P., Cao, Z., Cardarelli, R., Catalanotti, S., Chen, S. Z., Chen, T. L., Chen, Y., Creti, P., Cui, S. W., Dai, B. Z., Damone, A., Danzengluobu, Mitri, I., Dettorre Piazzoli, B., Di Girolamo, T., Ding, X. H., Di Sciascio, G., Feng, C. F., Feng, Zhaoyang, Feng, Zhenyong, Gou, Q. B., Guo, Y. Q., He, H. H., Hu, Haibing, Hu, Hongbo, Huang, Q., Iacovacci, M., Iuppa, R., Jia, H. Y., Labaciren, Li, H. J., Li, J. Y., Li, X. X., Liguori, G., Liu, C., Liu, C. Q., Liu, J., Liu, M. Y., Lu, H., Ma, L. L., Ma, X. H., Mancarella, G., Mari, S. M., Marsella, G., Martello, D., Mastroianni, S., Montini, P., Ning, C. C., Panareo, M., Panico, B., Perrone, L., Pistilli, P., Ruggieri, F., Salvini, P., Santonico, R., Sbano, S. N., Shen, P. R., Sheng, X. D., Shi, F., Surdo, A., Tan, Y. H., Piero Vallania, Vernetto, S., Vigorito, C., Wang, B., Wang, H., Wu, C. Y., Wu, H. R., Xu, B., Xue, L., Yang, Q. Y., Yang, X. C., Yao, Z. G., Yuan, A. F., Zha, M., Zhang, H. M., Zhang, Jilong, Zhang, Jianli, Zhang, L., Zhang, P., Zhang, X. Y., Zhang, Y., Zhao, J., Zhaxiciren, Zhaxisangzhu, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., Zizzi, G., Bartoli, Bruno, Bernardini, P., X. J., Bi, Bolognino, I., Branchini, P., Budano, A., Calabrese Melcarne, A. K., Camarri, P., Cao, Z., Cardarelli, R., Catalanotti, Sergio, Chen, S. Z., Chen, T. L., Chen, Y., Creti, P., Cui, S. W., Dai, B. Z., D'Amone, A., Danzengluobu, De Mitri, I., D'ETTORRE PIAZZOLI, Benedetto, DI GIROLAMO, Tristano, Ding, X. H., Di Sciascio, G., Feng, C. F., Zhaoyang, Feng, Zhenyong, Feng, Gou, Q. B., Guo, Y. Q., H. H., He, Haibing, Hu, Hongbo, Hu, Huang, Q., Iacovacci, Michele, Iuppa, R., Jia, H. Y., Labaciren, H. J., Li, J. Y., Li, X. X., Li, Liguori, G., Liu, C., Liu, C. Q., Liu, J., Liu, M. Y., Lu, H., L. L., Ma, X. H., Ma, Mancarella, G., Mari, S. M., Marsella, G., Martello, D., Mastroianni, S., Montini, P., Ning, C. C., Panareo, M., Panico, B., Perrone, L., Pistilli, P., Ruggieri, F., Salvini, P., Santonico, R., Sbano, S. N., Shen, P. R., Sheng, X. D., Shi, F., Surdo, A., Tan, Y. H., Vallania, P., Vernetto, S., Vigorito, C., Wang, B., Wang, H., C. Y., Wu, H. R., Wu, Xu, B., Xue, L., Yang, Q. Y., Yang, X. C., Yao, Z. G., Yuan, A. F., Zha, M., Zhang, H. M., Jilong, Zhang, Jianli, Zhang, Zhang, L., Zhang, P., Zhang, X. Y., Zhang, Y., Zhao, J., Zhaxiciren, Zhaxisangzhu, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., Zizzi, and G., B. Bartoli, BERNARDINI, Paolo, X. J. Bi, I. Bolognino, P. Branchini, A. Budano, A. K. Calabrese Melcarne, P. Camarri, Z. Cao, R. Cardarelli, S. Catalanotti, S. Z. Chen, T. L. Chen, Y. Chen, P. Creti, S. W. Cui, B. Z. Dai, D'AMONE, ANTONIO, DE MITRI, Ivan, B. D'Ettorre Piazzoli, T. Di Girolamo, X. H. Ding, G. Di Sciascio, C. F. Feng, Zhaoyang Feng, Zhenyong Feng, Q. B. Gou, Y. Q. Guo, H. H. He, Haibing Hu, Hongbo Hu, Q. Huang, M. Iacovacci, R. Iuppa, H. Y. Jia, H. J. Li, J. Y. Li, X. X. Li, G. Liguori, C. Liu, C. Q. Liu, J. Liu, M. Y. Liu, H. Lu, L. L. Ma, X. H. Ma, MANCARELLA, Giovanni, S. M. Mari, MARSELLA, GIOVANNI, MARTELLO, Daniele, S. Mastroianni, P. Montini, C. C. Ning, PANAREO, Marco, B. Panico, PERRONE, Lorenzo, P. Pistilli, F. Ruggieri, P. Salvini, R. Santonico, S. N. Sbano, P. R. Shen, X. D. Sheng, F. Shi, A. Surdo, Y. H. Tan, P. Vallania, S. Vernetto, C. Vigorito, B. Wang, H. Wang, C. Y. Wu, H. R. Wu, B. Xu, L. Xue, Q. Y. Yang, X. C. Yang, Z. G. Yao, A. F. Yuan, M. Zha, H. M. Zhang, Jilong Zhang, Jianli Zhang, L. Zhang, P. Zhang, X. Y. Zhang, Y. Zhang, J. Zhao, X. X. Zhou, F. R. Zhu, Q. Q. Zhu, G. Zizzi, B., Bartoli, Bernardini, Paolo, I., Bolognino, P., Branchini, A., Budano, A. K., Calabrese Melcarne, P., Camarri, Z., Cao, R., Cardarelli, S., Catalanotti, S. Z., Chen, T. L., Chen, Y., Chen, P., Creti, S. W., Cui, B. Z., Dai, D'Amone, Antonio, B., D'Ettorre Piazzoli, T., Di Girolamo, X. H., Ding, G., Di Sciascio, C. F., Feng, Q. B., Gou, Y. Q., Guo, Q., Huang, M., Iacovacci, R., Iuppa, H. Y., Jia, G., Liguori, C., Liu, C. Q., Liu, J., Liu, M. Y., Liu, H., Lu, Mancarella, Giovanni, S. M., Mari, Marsella, Giovanni, Martello, Daniele, S., Mastroianni, P., Montini, C. C., Ning, Panareo, Marco, B., Panico, Perrone, Lorenzo, P., Pistilli, F., Ruggieri, P., Salvini, R., Santonico, S. N., Sbano, P. R., Shen, X. D., Sheng, F., Shi, A., Surdo, Y. H., Tan, P., Vallania, S., Vernetto, C., Vigorito, B., Wang, H., Wang, B., Xu, L., Xue, Q. Y., Yang, X. C., Yang, Z. G., Yao, A. F., Yuan, M., Zha, H. M., Zhang, L., Zhang, P., Zhang, X. Y., Zhang, Y., Zhang, J., Zhao, X. X., Zhou, F. R., Zhu, Q. Q., Zhu, G., Zizzi, Mari, Stefano Maria, and The ARGO YBJ, Collaboration

Subjects
Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, FOS: Physical sciences, Flux, Field of view, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Gamma rays: general – surveys, 01 natural sciences, Declination, 0103 physical sciences, Absorption (logic), 010303 astronomy & astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Settore FIS/01 - Fisica Sperimentale, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, Astronomy and Astrophysics, general – su [gamma rays], Air shower, Extragalactic background light, 13. Climate action, Space and Planetary Science, Sky, general – surveys [Gamma rays], Astrophysics - High Energy Astrophysical Phenomena
Abstract

The ARGO-YBJ detector is an extensive air shower array that has been used to monitor the northern $\gamma$-ray sky at energies above 0.3 TeV from 2007 November to 2013 January. In this paper, we present the results of a sky survey in the declination band from $-10^{\circ}$ to $70^{\circ}$, using data recorded over the past five years. With an integrated sensitivity ranging from 0.24 to $\sim$1 Crab units depending on the declination, six sources have been detected with a statistical significance greater than 5 standard deviations. Several excesses are also reported as potential $\gamma$-ray emitters. The features of each source are presented and discussed. Additionally, $95\%$ confidence level upper limits of the flux from the investigated sky region are shown. Specific upper limits for 663 GeV $\gamma$-ray AGNs inside the ARGO-YBJ field of view are reported. The effect of the absorption of $\gamma$-rays due to the interaction with extragalactic background light is estimated., Comment: 30 pages, 13 figures, Accepted for publication by ApJ

13. Absolute-energy-scale calibration of ARGO-YBJ for light primaries in multi-TeV region with the Moon shadow observation

Author

X. C. Yang, H. H. He, T. Di Girolamo, Zhenyong Feng, H. Y. Jia, B. D'Ettorre Piazzoli, L. Xue, Hong-peng Lu, P. Pistilli, H. M. Zhang, X. X. Zhou, M. Iacovacci, M. Zha, Labaciren, X. D. Sheng, S. M. Mari, J. K. K. Liu, A. Surdo, Paolo Bernardini, L. L. Ma, Haibing Hu, Longzhou Zhang, H. W. Wang, J. B. Zhao, P. Salvini, Chang-Chun Ning, C. X. Liu, H. J. Li, H. R. Wu, Zhaoyang Feng, G. Marsella, X. J. Bi, Y. Zhang, Z. G. Yao, G. Mancarella, Zhaxisangzhu, C. Y. Wu, B. Bartoli, S. Z. Chen, L. Perrone, R. Santonico, G. Di Sciascio, Y. H. Tan, Fudong Shi, B. Z. Dai, S. Mastroianni, Carlo Vigorito, Zhaxiciren, F. R. Zhu, Danzengluobu, Y. Q. Guo, Q. Q. Zhu, I. De Mitri, Q. B. Gou, Zihuang Cao, Piero Vallania, T. L. Chen, A. F. Yuan, Pengnian Shen, S. Catalanotti, S. W. Cui, Hongbo Hu, C. F. Feng, P. Montini, X. H. Ma, X. Y. Zhang, Minghui Liu, R. Iuppa, S. Vernetto, A. D'Amone, Q. Y. Yang, Bartoli, B., Bernardini, P., Bi, X. J., Cao, Z., Catalanotti, S., Chen, S. Z., Chen, T. L., Cui, S. W., Dai, B. Z., D'Amone, A., Danzengluobu, Null, De Mitri, I., D'Ettorre Piazzoli, B., Di Girolamo, T., Di Sciascio, G., Feng, C. F., Feng, Zhaoyang, Feng, Zhenyong, Gou, Q. B., Guo, Y. Q., He, H. H., Hu, Haibing, Hu, Hongbo, Iacovacci, M., Iuppa, R., Jia, H. Y., Labaciren, Null, Li, H. J., Liu, C., Liu, J., Liu, M. Y., Lu, H., Ma, L. L., Ma, X. H., Mancarella, G., Mari, Stefano Maria, Marsella, G., Mastroianni, S., Montini, Paolo, Ning, C. C., Perrone, L., Pistilli, Pio, Salvini, P., Santonico, R., Shen, P. R., Sheng, X. D., Shi, F., Surdo, A., Tan, Y. H., Vallania, P., Vernetto, S., Vigorito, C., Wang, H., Wu, C. Y., Wu, H. R., Xue, L., Yang, Q. Y., Yang, X. C., Yao, Z. G., Yuan, A. F., Zha, M, Zhang, H. M., Zhang, L., Zhang, X. Y., Zhang, Y., Zhao, J., Zhaxiciren, Null, Zhaxisangzhu, Null, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., Bernardini, Paolo, D'Amone, Antonio, DE MITRI, Ivan, D’Ettorre Piazzoli, B., Mancarella, Giovanni, Mari, S. M., Marsella, Giovanni, Montini, P., Perrone, Lorenzo, Pistilli, P., Zha, M., and collaboration), (The ARGO YBJ

Subjects
Cosmic ray, Energy calibration, Energy spectrum, Moon shadow, Physics, Large Hadron Collider, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Hadron, Moon shadow, Astronomy, Astronomy and Astrophysics, Cosmic ray, Interaction model, Astrophysics, 01 natural sciences, Scale error, Energy calibration, Energy spectrum, Rigidity (electromagnetism), 0103 physical sciences, Ultra-high-energy cosmic ray, 010303 astronomy & astrophysics, Argo
Abstract

In 2011 ARGO-YBJ experiment has reported a work to study the absolute rigidity scale of the primary cosmic ray particles based on the Moon's shadow observation. Given the progress in high energy hadronic interaction models with LHC data, in cosmic ray chemical composition measurement and in experimental data accumulation, more updates can be researched. This paper aims to further disentangle the composition dependence in absolute-energy-scale calibration by using specific moon-shadow data which mainly is comprised of light component cosmic rays. Results show that, 17% energy scale error is estimated from 3 TeV to 50 TeV. To validate the performance of this technique, the light component cosmic ray spectrum in the same energy region is shown. (C) 2017 Elsevier B.V. All rights reserved.

Published
2017
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14. STUDY OF THE DIFFUSE GAMMA-RAY EMISSION FROM THE GALACTIC PLANE WITH ARGO-YBJ

Author

Q. Q. Zhu, Labaciren, Zhengguo Cao, P. Bernardini, J. K. K. Liu, X. X. Zhou, C. Y. Wu, J. Zhao, Y. J. Zhang, R. Santonico, H. H. He, Zhenyong Feng, P. R. Shen, F. Shi, C. Q. Liu, Q. B. Gou, F. R. Zhu, P. Creti, C. C. Ning, X. C. Yang, Haifeng Li, H. Lu, I. De Mitri, A. D'Amone, P. Vallania, S. M. Mari, T. Di Girolamo, Danzengluobu, R. Cardarelli, A. F. Yuan, M. Panareo, Minghui Liu, B. D'Ettorre Piazzoli, Y. H. Tan, M. Zha, Lanqing Ma, X. J. Bi, L. Xue, L. Zhang, T. L. Chen, S. Vernetto, Zhaxiciren, A. Surdo, R. Iuppa, G. Zizzi, C. Vigorito, Zhaxisangzhu, P. Salvini, Q. Y. Yang, S. Z. Chen, G. Marsella, B. Bartoli, G. Liguori, M. Iacovacci, S. Catalanotti, B. Z. Dai, Zhaoyang Feng, Paolo Camarri, P. Montini, X. H. Ma, L. Perrone, G. Di Sciascio, X. Y. Zhang, A. Budano, Z. G. Yao, Haibing Hu, Xiangdong Sheng, S. Mastroianni, D. Martello, P. Pistilli, H. M. Zhang, H. R. Wu, Hongbo Hu, Yicheng Guo, H. Wang, Cunfeng Feng, F. Ruggieri, H. Y. Jia, S. W. Cui, G. Mancarella, P. Branchini, Mari, Stefano Maria, The ARGO YBJ, Collaboration, ITA, Bartoli, Bruno, Bernardini, P., Bi, X. J., Branchini, P., Budano, A., Camarri, P., Cao, Z., Cardarelli, R., Catalanotti, Sergio, Chen, S. Z., Chen, T. L., Creti, P., Cui, S. W., Dai, B. Z., D’Amone, A., Danzengluobu, Null, De Mitri, I., D'ETTORRE PIAZZOLI, Benedetto, DI GIROLAMO, Tristano, Sciascio, G. Di, Feng, C. F., Feng, Zhaoyang, Feng, Zhenyong, Gou, Q. B., Guo, Y. Q., He, H. H., Hu, Haibing, Hu, Hongbo, Iacovacci, Michele, Iuppa, R., Jia, H. Y., Labaciren, Null, Li, H. J., Liguori, G., Liu, C., Liu, J., Liu, M. Y., Lu, H., Ma, L. L., Ma, X. H., Mancarella, G., Mari, S. M., Marsella, G., Martello, D., Mastroianni, S., Montini, P., Ning, C. C., Panareo, M., Perrone, L., Pistilli, P., Ruggieri, F., Salvini, P., Santonico, R., Shen, P. R., Sheng, X. D., Shi, F., Surdo, A., Tan, Y. H., Vallania, P., Vernetto, S., Vigorito, C., Wang, H., Wu, C. Y., Wu, H. R., Xue, L., Yang, Q. Y., Yang, X. C., Yao, Z. G., Yuan, A. F., Zha, M., Zhang, H. M., Zhang, L., Zhang, X. Y., Zhang, Y., Zhao, J., Zhaxiciren, Null, Zhaxisangzhu, Null, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., Zizzi, G., B., Bartoli, Bernardini, Paolo, X. J., Bi, P., Branchini, A., Budano, P., Camarri, Z., Cao, R., Cardarelli, S., Catalanotti, S. Z., Chen, T. L., Chen, P., Creti, S. W., Cui, B. Z., Dai, D'Amone, Antonio, Danzengluobu, DE MITRI, Ivan, B., D’Ettorre Piazzoli, T., Di Girolamo, G., Di Sciascio, C. F., Feng, Zhaoyang, Feng, Zhenyong, Feng, Q. B., Gou, Y. Q., Guo, H. H., He, Haibing, Hu, Hongbo, Hu, M., Iacovacci, R., Iuppa, H. Y., Jia, Labaciren, H. J., Li, G., Liguori, C., Liu, J., Liu, M. Y., Liu, H., Lu, L. L., Ma, X. H., Ma, Mancarella, Giovanni, S. M., Mari, Marsella, Giovanni, Martello, Daniele, S., Mastroianni, P., Montini, C. C., Ning, Panareo, Marco, Perrone, Lorenzo, P., Pistilli, F., Ruggieri, P., Salvini, R., Santonico, P. R., Shen, X. D., Sheng, F., Shi, A., Surdo, Y. H., Tan, P., Vallania, S., Vernetto, C., Vigorito, H., Wang, C. Y., Wu, H. R., Wu, L., Xue, Q. Y., Yang, X. C., Yang, Z. G., Yao, A. F., Yuan, M., Zha, H. M., Zhang, L., Zhang, X. Y., Zhang, Y., Zhang, J., Zhao, Zhaxiciren, Zhaxisangzhu, X. X., Zhou, F. R., Zhu, Q. Q., Zhu, and G., Zizzi

Subjects
Astrophysics::High Energy Astrophysical Phenomena, observational [methods], Flux, FOS: Physical sciences, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, disk, methods: observational [cosmic rays, diffuse radiation, Galaxy], Galaxy: disk, High Energy Physics - Phenomenology (hep-ph), cosmic rays, Disc, Instrumentation and Methods for Astrophysics (astro-ph.IM), cosmic ray, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Settore FIS/01 - Fisica Sperimentale, Gamma ray, Astronomy and Astrophysics, Galactic plane, Galaxy, diffuse radiation, High Energy Physics - Phenomenology, Space and Planetary Science, Milagro, methods: observational, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, disk [Galaxy], Fermi Gamma-ray Space Telescope
Abstract

The events recorded by ARGO-YBJ in more than five years of data collection have been analyzed to determine the diffuse gamma-ray emission in the Galactic plane at Galactic longitudes 25{\deg} < l < 100{\deg} and Galactic latitudes . The energy range covered by this analysis, from ~350 GeV to ~2 TeV, allows the connection of the region explored by Fermi with the multi-TeV measurements carried out by Milagro. Our analysis has been focused on two selected regions of the Galactic plane, i.e., 40{\deg} < l < 100{\deg} and 65{\deg} < l < 85{\deg} (the Cygnus region), where Milagro observed an excess with respect to the predictions of current models. Great care has been taken in order to mask the most intense gamma-ray sources, including the TeV counterpart of the Cygnus cocoon recently identified by ARGO-YBJ, and to remove residual contributions. The ARGO-YBJ results do not show any excess at sub-TeV energies corresponding to the excess found by Milagro, and are consistent with the predictions of the Fermi model for the diffuse Galactic emission. From the measured energy distribution we derive spectral indices and the differential flux at 1 TeV of the diffuse gamma-ray emission in the sky regions investigated., Comment: 11 pages, 6 figures, published in APJ

Published
2015

15. 4.5 YEARS OF MULTI-WAVELENGTH OBSERVATIONS OF MRK 421 DURING THE ARGO-YBJ AND FERMI COMMON OPERATION TIME

Author

B. Bartoli, A. F. Yuan, Huihai He, Xiangdong Sheng, L. Perrone, A. D'Amone, S. W. Cui, Haibing Hu, Longzhou Zhang, Y. Zhang, B. D'Ettorre Piazzoli, Labaciren, Zhaxiciren, Q. Y. Yang, Q. Q. Zhu, X. C. Yang, C. Y. Wu, Y. Q. Guo, R. Santonico, L. Xue, F. R. Zhu, S. M. Mari, Zihuang Cao, J. K. K. Liu, Q. B. Gou, X. Y. Zhang, Minghui Liu, Hong-peng Lu, I. De Mitri, G. Mancarella, Carlo Vigorito, C. X. Liu, P. Pistilli, H. M. Zhang, X. X. Zhou, J. B. Zhao, T. L. Chen, P. Salvini, A. Surdo, M. Iacovacci, M. Zha, Y. H. Tan, Z. G. Yao, H. J. Li, H. R. Wu, B. Z. Dai, X. J. Bi, Danzengluobu, Fudong Shi, Paolo Bernardini, S. Mastroianni, L. L. Ma, H. W. Wang, G. Marsella, Zhenyong Feng, S. Z. Chen, G. Di Sciascio, P. Montini, X. H. Ma, Hongbo Hu, C. F. Feng, Piero Vallania, H. Y. Jia, Pengnian Shen, S. Catalanotti, T. Di Girolamo, R. Iuppa, S. Vernetto, Zhaxisangzhu, Chang-Chun Ning, Zhaoyang Feng, Bartoli, B., Bernardini, P., Bi, X. J., Cao, Z., Catalanotti, S., Chen, S. Z., Chen, T. L., Cui, S. W., Dai, B. Z., D'Amone, A., Danzengluobu, Null, De Mitri, I., Piazzoli, B. D'Ettorre, Di Girolamo, T., Di Sciascio, G., Feng, C. F., Feng, Zhaoyang, Feng, Zhenyong, Gou, Q. B., Guo, Y. Q., He, H. H., Hu, Haibing, Hu, Hongbo, Iacovacci, M., Iuppa, R., Jia, H. Y., Labaciren, Null, Li, H. J., Liu, C., Liu, J., Liu, M. Y., Lu, H., Ma, L. L., Ma, X. H., Mancarella, G., Mari, Stefano Maria, Marsella, G., Mastroianni, S., Montini, Paolo, Ning, C. C., Perrone, L., Pistilli, Pio, Salvini, P., Santonico, R., Shen, P. R., Sheng, X. D., Shi, F., Surdo, A., Tan, Y. H., Vallania, P., Vernetto, S., Vigorito, C., Wang, H., Wu, C. Y., Wu, H. R., Xue, L., Yang, Q. Y., Yang, X. C., Yao, Z. G., Yuan, A. F., Zha, M., Zhang, H. M., Zhang, L., Zhang, X. Y., Zhang, Y., Zhao, J., Zhaxiciren, Null, Zhaxisangzhu, Null, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., Bartoli, Bruno, Catalanotti, Sergio, D’Amone, A., Mitri, I. De, D'ETTORRE PIAZZOLI, Benedetto, DI GIROLAMO, Tristano, Iacovacci, Michele, Mari, S. M., Montini, P., Pistilli, P., Bernardini, Paolo, Xje, X. J. E, Cao, Z. E, D'Amone, Antonio, Danzengluobu, DE MITRI, Ivan, Piazzoli, B. D., Feng, Z., Hu, H., Labaciren, Mancarella, Giovanni, Marsella, Giovanni, Perrone, Lorenzo, Yao, Z. G. E, Yuan, A., F., Zhaxiciren, and Zhaxisangzhu

Subjects
Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Cosmic ray, Astrophysics, Electron, BL Lacertae objects: individual (Markarian 421), 01 natural sciences, 7. Clean energy, law.invention, Acceleration, law, 0103 physical sciences, Emission spectrum, Blazar, 010303 astronomy & astrophysics, cosmic ray, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, gamma-rays: general, radiation mechanisms: non-thermal, Astronomy and Astrophysics, Space and Planetary Science, 010308 nuclear & particles physics, Spectral density, Astronomy and Astrophysic, Synchrotron, gamma-ray Anstronomy, LARGE-AREA TELESCOPE, GAMMA-RAY EMISSION, BL-LAC OBJECTS, ENERGY-DISTRIBUTIONS, PHYSICAL-PROPERTIES, 13. Climate action, Astrophysics - High Energy Astrophysical Phenomena, SPECTRAL EVOLUTION, SHOCK ACCELERATION, FEBRUARY 2010, TEV BLAZARS, GIANT FLARE, Fermi Gamma-ray Space Telescope
Abstract

We report on the extensive multi-wavelength observations of the blazar Markarian 421 (Mrk 421) covering radio to gamma-rays, during the 4.5 year period of ARGO-YBJ and Fermi common operation time, from August 2008 to February 2013. In particular, thanks to the ARGO-YBJ and Fermi data, the whole energy range from 100 MeV to 10 TeV is covered without any gap. In the observation period, Mrk 421 showed both low and high activity states at all wavebands. The correlations among flux variations in different wavebands were analyzed. Seven large flares, including five X-ray flares and two GeV gamma-ray flares with variable durations (3-58 days), and one X-ray outburst phase were identified and used to investigate the variation of the spectral energy distribution with respect to a relative quiescent phase. During the outburst phase and the seven flaring episodes, the peak energy in X-rays is observed to increase from sub-keV to few keV. The TeV gamma-ray flux increases up to 0.9-7.2 times the flux of the Crab Nebula. The behavior of GeV gamma-rays is found to vary depending on the flare, a feature that leads us to classify flares into three groups according to the GeV flux variation. Finally, the one-zone synchrotron self-Compton model was adopted to describe the emission spectra. Two out of three groups can be satisfactorily described using injected electrons with a power-law spectral index around 2.2, as expected from relativistic diffuse shock acceleration, whereas the remaining group requires a harder injected spectrum. The underlying physical mechanisms responsible for different groups may be related to the acceleration process or to the environment properties., 17 pages, 9 figures, 5 tables, Accepted for publication in ApJS

Published
2016
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16. Observation of TeV gamma rays from the Cygnus region with the ARGO-YBJ experiment

Author

Carla Bleve, Q. Q. Zhu, B. S. Wang, Zhaxisangzhu, Hongbo Hu, C. F. Feng, B. Bartoli, Carlo Vigorito, S. M. Mari, A. F. Yuan, X. D. Sheng, Zhengguo Cao, Paolo Montini, T. Di Girolamo, G. Liguori, B. D'Ettorre Piazzoli, R. Iuppa, L. L. Ma, Haibing Hu, Jilong Zhang, Y. Q. Guo, E. Giroletti, Y. B. Chen, H. J. Li, Chang-Chun Ning, Zhaoyang Feng, H. R. Wu, F. Ruggieri, Y. Zhang, P. Bernardini, S. W. Cui, D. Martello, B. Panico, Labaciren, Jianli Zhang, L. Xue, M. Iacovacci, M. Zha, M. Y. Liu, P. R. Shen, X. Y. Zhang, B. Z. Dai, J. K. K. Liu, Antonio Budano, P. Pistilli, H. M. Zhang, X. X. Zhou, C. Cattaneo, H. Y. Jia, X. H. Ding, Hong-peng Lu, Q. Y. Yang, Zhaxiciren, P. Creti, A. K. Calabrese Melcarne, P. F. Zhang, Cristian Stanescu, P. Branchini, A. Surdo, Roberto Cardarelli, Danzengluobu, G. Zizzi, Q. Huang, X. J. Bi, G. Marsella, Zhenyong Feng, F. R. Zhu, S. Vernetto, C. Liu, Bingwei Xu, X. X. Li, S. Catalanotti, Paolo Camarri, Z. G. Yao, H.H. He, M. Dattoli, M. Panareo, Huaguang Wang, Y. H. Tan, X. H. Ma, Q. B. Gou, I. De Mitri, J. B. Zhao, P. Salvini, Fudong Shi, A. Pagliaro, S. Mastroianni, J. Y. Li, T. L. Chen, I. Bolognino, S. Z. Chen, Giovanni Mancarella, G. Di Sciascio, X. C. Yang, R. Santonico, Irina James, L. Perrone, F. Galeazzi, Longzhou Zhang, C. Y. Wu, C. Q. Liu, G. D'Alí Staiti, P. Vallania, B., Bartoli, Bernardini, Paolo, X. J., Bi, C., Bleve, I., Bolognino, P., Branchini, A., Budano, A. K., Calabrese Melcarne, P., Camarri, Z., Cao, R., Cardarelli, S., Catalanotti, C., Cattaneo, S. Z., Chen, T. L., Chen, Y., Chen, P., Creti, S. W., Cui, B. Z., Dai, G., D'Alí Staiti, Danzengluobu, M., Dattoli, DE MITRI, Ivan, B., D'Ettorre Piazzoli, T., Di Girolamo, X. H., Ding, G., Di Sciascio, C. F., Feng, Zhaoyang, Feng, Zhenyong, Feng, F., Galeazzi, E., Giroletti, Q. B., Gou, Y. Q., Guo, H. H., He, Haibing, Hu, Hongbo, Hu, Q., Huang, M., Iacovacci, R., Iuppa, I., Jame, H. Y., Jia, Labaciren, H. J., Li, J. Y., Li, X. X., Li, G., Liguori, C., Liu, C. Q., Liu, J., Liu, M. Y., Liu, H., Lu, L. L., Ma, X. H., Ma, Mancarella, Giovanni, S. M., Mari, Marsella, Giovanni, Martello, Daniele, S., Mastroianni, P., Montini, C. C., Ning, A., Pagliaro, Panareo, Marco, B., Panico, Perrone, Lorenzo, P., Pistilli, F., Ruggieri, P., Salvini, R., Santonico, P. R., Shen, X. D., Sheng, F., Shi, C., Stanescu, A., Surdo, Y. H., Tan, P., Vallania, S., Vernetto, C., Vigorito, B., Wang, H., Wang, C. Y., Wu, H. R., Wu, B., Xu, L., Xue, Q. Y., Yang, X. C., Yang, Z. G., Yao, A. F., Yuan, M., Zha, H. M., Zhang, Jilong, Zhang, Jianli, Zhang, L., Zhang, P., Zhang, X. Y., Zhang, Y., Zhang, J., Zhao, Zhaxiciren, Zhaxisangzhu, X. X., Zhou, F. R., Zhu, Q. Q., Zhu, G., Zizzi, Bartoli, Bruno, Bernardini, P., Bleve, C., Bolognino, I., Branchini, P., Budano, A., A. K. C., Camarri, P., Cao, Z., Cardarelli, R., Catalanotti, Sergio, Cattaneo, C., Chen, S. Z., Chen, T. L., Chen, Y., Creti, P., Cui, S. W., Dai, B. Z., Staiti, G. D., Dattoli, M., Mitri, I. D., D'ETTORRE PIAZZOLI, Benedetto, DI GIROLAMO, Tristano, Ding, X. H., Sciascio, G. D., Feng, C. F., Feng, Z. Y., Galeazzi, F., Giroletti, E., Gou, Q. B., Guo, Y. Q., H. B., Hu, Huang, Q., Iacovacci, Michele, Iuppa, R., James, I., Jia, H. Y., Liguori, G., Liu, C., Liu, C. Q., Liu, J., Liu, M. Y., Lu, H., Mancarella, G., Mari, S. M., Marsella, G., Martello, D., Mastroianni, S., Montini, P., Ning, C. C., Pagliaro, A., Panareo, M., Panico, B., Perrone, L., Pistilli, P., Ruggieri, F., Salvini, P., Santonico, R., Shen, P. R., Sheng, X. D., Shi, F., Stanescu, C., Surdo, A., Tan, Y. H., Vallania, P., Vernetto, S., Vigorito, C., Wang, B., Wang, H., Xu, B., Xue, L., Yang, Q. Y., Yang, X. C., Yao, Z. G., Yuan, A. F., Zha, M., Zhang, H. M., Zhang, J. L., Zhang, L., Zhang, P., Zhang, X. Y., Zhang, Y., Zhao, J., Zhou, X. X., Zhu, F. R., Zhu, Q. Q., Zizzi, G., Bartoli, B, Bernardini, P, Bi, XJ, Bleve, C, Bolognino, I, Branchini, P, Budano, A, Calabrese Melcarne, AK, Camarri, P, Cao, Z, Cardarelli, R, Catalanotti, S, Cattaneo, C, Chen, SZ, Chen, TL, Chen, Y, Creti, P, Cui, SW, Dai, BZ, D’Ali Staiti, G, Dattoli, M, De Mitri, I, D’Ettorre Piazzoli, B, Di Girolamo, T, Ding, XH, Di Sciascio, G, Feng, CF, Feng, ZYa, Feng, ZYo, Galeazzi, F, Giroletti, E, Gou, QB, Guo, YQ, He, HH, Hu, HBi, Hu, HBo, Huang, Q, Iacovacci, M, Iuppa, R, James, I, Jia, HY, Li, HJ, Li, JY, Li, XX, Liguori, G, Liu, C, Liu, CQ, Liu, J, Liu, MY, Lu, H, Ma, LL, Ma, XH, Mancarella, G, Mari, SM, Marsella, G, Martello, D, Mastroianni, S, Montini, P, Ning, CC, Pagliaro, A, Panareo, M, Panico, B, Perrone, L, Pistilli, P, Ruggieri, F, Salvini, P, Santonico, R, Shen, PR, Sheng, XD, Shi, F, Stanescu, C, Surdo, A, Tan, YH, Vallania, P, Vernetto, S, Vigorito, C, Wang, B, Wang, H, Wu, CY, Wu, HR, Xu, B, Xue, L, Yang, QY, Yang, XC, Yao, ZG, Yuan, AF, M. Zha, M, Zhang, HM, Zhang, JLi, Zhang, JLo, Zhang, L, Zhang, P, Zhang, XY, Zhang, Y, Zhao, J, Zhaxiciren, Zhaxisangzhu, Zhou, XX, Zhu, FR, Zhu, QQ, Zizzi, G, Bartoli, B., Bi, X. J., Melcarne A. K., Calabrese, Catalanotti, S., Staiti G., D'Ali, De Mitri, I., Piazzoli B., D'Ettorre, Di Girolamo, T., Di Sciascio, G., Feng, Zhaoyang, Feng, Zhenyong, He, H. H., Hu, Haibing, Hu, Hongbo, Iacovacci, M., Li, H. J., Li, J. Y., Li, X. X., Ma, L. L., Ma, X. H., Mari, Stefano Maria, Wu, C. Y., Wu, H. R., Zhang, Jilong, and Zhang, Jianli

Subjects
Astrophysics::High Energy Astrophysical Phenomena, general – pulsars: individual (MGRO J2019+37 [Gamma rays], Flux, FOS: Physical sciences, Astrophysics, 01 natural sciences, Pulsar wind nebula, general – pulsar, 0103 physical sciences, MILAGRO, 010303 astronomy & astrophysics, DETECTOR, Argo, Physics, CALIBRATION, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, MGRO J2031+41), Settore FIS/01 - Fisica Sperimentale, Gamma ray, Astronomy and Astrophysics, individual (MGRO J2019+37, MGRO J2031+41), PLANE, 3. Good health, Medium energy, Crab Nebula, gamma ray, 13. Climate action, Space and Planetary Science, GALACTIC SOURCES, J2032+4130, Milagro, gamma rays, general – pulsars, EMISSION, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We report the observation of TeV gamma-rays from the Cygnus region using the ARGO-YBJ data collected from 2007 November to 2011 August. Several TeV sources are located in this region including the two bright extended MGRO J2019+37 and MGRO J2031+41. According to the Milagro data set, at 20 TeV MGRO J2019+37 is the most significant source apart from the Crab Nebula. No signal from MGRO J2019+37 is detected by the ARGO-YBJ experiment, and the derived flux upper limits at 90% confidence level for all the events above 600 GeV with medium energy of 3 TeV are lower than the Milagro flux, implying that the source might be variable and hard to be identified as a pulsar wind nebula. The only statistically significant (6.4 standard deviations) gamma-ray signal is found from MGRO J2031+41, with a flux consistent with the measurement by Milagro., 14 pages, 4 figures

Published
2012

17. Light-component spectrum of the primary cosmic rays in the multi-TeV region measured by the ARGO-YBJ experiment

Author

X. C. Yang, B. Bartoli, Zhenyong Feng, B. Panico, C. Liu, P. R. Shen, Irina James, X. H. Ma, J. K. K. Liu, P. Salvini, G. D'Alí Staiti, P. Vallania, Q. Q. Zhu, P. Pistilli, H. M. Zhang, X. X. Zhou, Giovanni Mancarella, G. Di Sciascio, B. D'Ettorre Piazzoli, P. Creti, R. Santonico, X. X. Li, Y. B. Chen, H. J. Li, Carla Bleve, H. R. Wu, Hongbo Hu, H. Y. Jia, L. Xue, C. F. Feng, Bingwei Xu, C. Y. Wu, A. Surdo, L. Perrone, Hong-peng Lu, C. Q. Liu, Chang-Chun Ning, Zhaoyang Feng, Q. Huang, I. De Mitri, Q. B. Gou, X. Y. Zhang, T. Di Girolamo, Paolo Camarri, T. L. Chen, M. Iacovacci, B. Z. Dai, X. X. Yan, F. R. Zhu, P. F. Zhang, X. J. Bi, Y. Q. Guo, S. Catalanotti, S. W. Cui, S. Z. Chen, Jianli Zhang, P. Bernardini, F. Ruggieri, Cristian Stanescu, P. Branchini, M. Panareo, Zihuang Cao, A. F. Yuan, Carlo Vigorito, B. S. Wang, Longzhou Zhang, Zhaxisangzhu, Haibing Hu, E. Giroletti, Z. G. Yao, S. M. Mari, Antonio Budano, Y. Zhang, Labaciren, D. Martello, M. Zha, C. Cattaneo, A. K. Calabrese Melcarne, Paolo Montini, G. Marsella, R. Iuppa, S. Vernetto, Danzengluobu, X. D. Sheng, J. Y. Li, H.H. He, M. Dattoli, I. Bolognino, M. Y. Liu, Q. Y. Yang, G. Zizzi, X. B. Qu, X. H. Ding, Roberto Cardarelli, Y. H. Tan, A. Pagliaro, G. Liguori, Huaguang Wang, Fudong Shi, S. Mastroianni, Zhaxiciren, Jilong Zhang, Bartoli, B., Bernardini, P., Bi, X. J., Bleve, C., Bolognino, I., Branchini, P., Budano, A., Calabrese Melcarne, A. K., Camarri, P., Cao, Z., Cardarelli, R., Catalanotti, S., Cattaneo, C., Chen, S. Z., Chen, T. L., Chen, Y., Creti, P., Cui, S. W., Dai, B. Z., D'Ali Staiti, G., Danzengluobu, Dattoli, M., De Mitri, I., D'Ettorre Piazzoli, B., Di Girolamo, T., Ding, X. H., Di Sciascio, G., Feng, C. F., Feng, Z., Giroletti, E., Gou, Q. B., Guo, Y. Q., He, H. H., Hu, H., Huang, Q., Iacovacci, M., Iuppa, R., James, I., Jia, H. Y., Labaciren, Li, H. J., Li, J. Y., Li, X. X., Liguori, G., Liu, C., Liu, C. Q., Liu, J., Liu, M. Y., Lu, H., Ma, X. H., Mancarella, G., Mari, S. M., Marsella, G., Martello, D., Mastroianni, S., Montini, P., Ning, C. C., Pagliaro, A., Panareo, M., Panico, B., Perrone, L., Pistilli, P., Qu, X. B., Ruggieri, F., Salvini, P., Santonico, R., Shen, P. R., Sheng, X. D., Shi, F., Stanescu, C., Surdo, A., Tan, Y. H., Vallania, P., Vernetto, S., Vigorito, C., Wang, B., Wang, H., Wu, C. Y., Wu, H. R., Xu, B., Xue, L., Yan, X. X., Yang, Q. Y., Yang, X. C., Yao, Z. G., Yuan, A. F., Zha, M., Zhang, H. M., Zhang, J., Zhang, L., Zhang, P., Zhang, X. Y., Zhang, Y., Zhaxiciren, Zhaxisangzhu, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., Zizzi, G., Bartoli, B, Bernardini, P, Bi, Xj, Bleve, C, Bolognino, I, Branchini, P, Budano, A, Melcarne, Akc, Camarri, P, Cao, Z, Cardarelli, R, Catalanotti, S, Cattaneo, C, Chen, Sz, Chen, Tl, Chen, Y, Creti, P, Cui, Sw, Dai, Bz, Staiti, Gd, Dattoli, M, De Mitri, I, Piazzoli, Bd, Di Girolamo, T, Ding, Xh, Di Sciascio, G, Feng, Cf, Feng, Zy, Giroletti, E, Gou, Qb, Guo, Yq, He, Hh, Hu, Hb, Huang, Q, Iacovacci, M, Iuppa, R, James, I, Jia, Hy, Li, Hj, Li, Jy, Li, Xx, Liguori, G, Liu, C, Liu, Cq, Liu, J, Liu, My, Lu, H, Ma, Xh, Mancarella, G, Mari, Stefano Maria, Marsella, G, Martello, D, Mastroianni, S, Montini, P, Ning, Cc, Pagliaro, A, Panareo, M, Panico, B, Perrone, L, Pistilli, P, Qu, Xb, Ruggieri, F, Salvini, P, Santonico, R, Shen, Pr, Sheng, Xd, Shi, F, Stanescu, C, Surdo, A, Tan, Yh, Vallania, P, Vernetto, S, Vigorito, C, Wang, B, Wang, H, Wu, Cy, Wu, Hr, Xu, B, Xue, L, Yan, Xx, Yang, Qy, Yang, Xc, Yao, Zg, Yuan, Af, Zha, M, Zhang, Hm, Zhang, Jl, Zhang, L, Zhang, P, Zhang, Xy, Zhang, Y, Zhou, Xx, Zhu, Fr, Zhu, Qq, Bartoli, Bruno, X. J., Bi, A. K. C., Catalanotti, Sergio, Staiti, G. D., Mitri, I. D., D'ETTORRE PIAZZOLI, Benedetto, DI GIROLAMO, Tristano, Sciascio, G. D., Feng, Z. Y., H. H., He, H. B., Hu, Iacovacci, Michele, H. J., Li, J. Y., Li, X. X., Li, X. H., Ma, X. B., Qu, C. Y., Wu, H. R., Wu, Zhang, J. L., B., Bartoli, Bernardini, Paolo, C., Bleve, I., Bolognino, P., Branchini, A., Budano, A. K., Calabrese Melcarne, P., Camarri, Z., Cao, R., Cardarelli, S., Catalanotti, C., Cattaneo, S. Z., Chen, T. L., Chen, Y., Chen, P., Creti, S. W., Cui, B. Z., Dai, G., D’Alı´ Staiti, M., Dattoli, DE MITRI, Ivan, B., D’Ettorre Piazzoli, T., Di Girolamo, X. H., Ding, G., Di Sciascio, C. F., Feng, Zhaoyang, Feng, Zhenyong, Feng, E., Giroletti, Q. B., Gou, Y. Q., Guo, Haibing, Hu, Hongbo, Hu, Q., Huang, M., Iacovacci, R., Iuppa, I., Jame, H. Y., Jia, G., Liguori, C., Liu, C. Q., Liu, J., Liu, M. Y., Liu, H., Lu, Mancarella, Giovanni, S. M., Mari, Marsella, Giovanni, Martello, Daniele, S., Mastroianni, P., Montini, C. C., Ning, A., Pagliaro, Panareo, Marco, B., Panico, Perrone, Lorenzo, P., Pistilli, F., Ruggieri, P., Salvini, R., Santonico, P. R., Shen, X. D., Sheng, F., Shi, C., Stanescu, A., Surdo, Y. H., Tan, P., Vallania, S., Vernetto, C., Vigorito, B., Wang, H., Wang, B., Xu, L., Xue, X. X., Yan, Q. Y., Yang, X. C., Yang, Z. G., Yao, A. F., Yuan, M., Zha, H. M., Zhang, Jilong, Zhang, Jianli, Zhang, L., Zhang, P., Zhang, X. Y., Zhang, Y., Zhang, X. X., Zhou, F. R., Zhu, Q. Q., Zhu, G., Zizzi, Bi, XJ, Calabrese Melcarne, AK, Chen, SZ, Chen, TL, Cui, SW, Dai, BZ, D'ALI'STAITI, G, D’Ettorre Piazzoli, B, Ding, XH, Feng, CF, Feng, ZYa, Feng, ZYo, Gou, QB, Guo, YQ, He, HH, Hu, HBi, Hu, HBo, James, J, Jia, HY, Li, HJ, Li, JY, Li, XX, Liu, CQ, Liu, MY, Ma, XH, Mari, S, Ning, CC, Panareo, P, Qu, XB, Shen, PR, Sheng, XD, Tan, YH, Wu, CY, Wu, HR, Yan, XX, Yang, QY, Yang, XC, Yao, ZG, Yuan, AF, Zhang, HM, Zhang, JLi, Zhang, JLo, Zhang, XY, Zhou, XX, Zhu, FR, Zhu, QQ, and Zizzi, G

Subjects
Extended Air Showers, Cosmic Rays, Gamma Ray sources, Nuclear and High Energy Physics, Proton, TIBET, Astrophysics::High Energy Astrophysical Phenomena, Extensive air shower, chemistry.chemical_element, Cosmic ray, HELIUM SPECTRA, Astrophysics, PROTON, Bayesian method, CASCADES, Spectral line, Settore FIS/05 - Astronomia E Astrofisica, Nuclear magnetic resonance, Cosmic-ray observatory, Helium, Physics, Range (particle radiation), ENERGY-RANGE, BALLOON EXPERIMENT, NUCLEI, Settore FIS/01 - Fisica Sperimentale, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, light component spectrum, chemistry, Energy (signal processing), SYSTEM
Abstract

The ARGO-YBJ experiment detects extensive air showers in a wide energy range by means of a full-coverage detector which is in stable data taking in its full configuration since November 2007 at the YBJ International Cosmic Ray Observatory (4300 m a.s.l., Tibet, People's Republic of China). In this paper the measurement of the light-component spectrum of primary cosmic rays in the energy region $(5\textdiv{}200)\text{ }\text{ }\mathrm{TeV}$ is reported. The method exploited to analyze the experimental data is based on a Bayesian procedure. The measured intensities of the light component are consistent with the recent CREAM results and higher than that obtained adding the proton and helium spectra reported by the RUNJOB experiment.

Published
2012

18. ARGO-YBJ OBSERVATION OF THE LARGE-SCALE COSMIC RAY ANISOTROPY DURING THE SOLAR MINIMUM BETWEEN CYCLES 23 AND 24

Author

Lanqing Ma, M. Iacovacci, M. Zha, S. W. Cui, H. W. Wang, X. D. Sheng, G. Mancarella, Q. Y. Yang, B. D'Ettorre Piazzoli, Paolo Bernardini, Zhaxisangzhu, X. J. Bi, B. Bartoli, X. C. Yang, R. Santonico, L. Zhang, S. Z. Chen, C. Y. Wu, A. F. Yuan, Zhaxiciren, J. W. Zhao, Haibing Hu, F. R. Zhu, P. Salvini, W. Gao, A. D'Amone, L. Xue, Labaciren, G. Marsella, L. Perrone, Fudong Shi, Q. Q. Zhu, Danzengluobu, S. Mastroianni, Hong-peng Lu, Y. Zhang, I. De Mitri, C. X. Liu, J. K. K. Liu, Z. G. Yao, T. L. Chen, Zihuang Cao, Zhenyong Feng, S. M. Mari, Y. H. Tan, H. H. He, Carlo Vigorito, P. Pistilli, H. M. Zhang, X. X. Zhou, H. Y. Jia, G. Di Sciascio, X. Y. Zhang, Minghui Liu, B. Z. Dai, P. Montini, X. H. Ma, Y. Q. Guo, Piero Vallania, H. J. Li, H. R. Wu, Hongbo Hu, A. Surdo, C. F. Feng, Q. B. Gou, T. Di Girolamo, R. Iuppa, S. Vernetto, Pengnian Shen, S. Catalanotti, Chang-Chun Ning, Zhaoyang Feng, Bartoli, Bruno, Bernardini, P., Bi, X. J., Cao, Z., Catalanotti, Sergio, Chen, S. Z., Chen, T. L., Cui, S. W., Dai, B. Z., D’Amone, A., Danzengluobu, Null, D’Ettorre Piazzoli, B., DI GIROLAMO, Tristano, Sciascio, G. Di, Feng, C. F., Feng, Zhaoyang, Feng, Zhenyong, Gao, W., Gou, Q. B., Guo, Y. Q., He, H. H., Hu, Haibing, Hu, Hongbo, Iacovacci, Michele, Iuppa, R., Jia, H. Y., Labaciren, Null, Li, H. J., Liu, C., Liu, J., Liu, M. Y., Lu, H., Ma, L. L., Ma, X. H., Mancarella, G., Mari, S. M., Marsella, G., Mastroianni, S., Montini, P., Ning, C. C., Perrone, L., Pistilli, P., Salvini, P., Santonico, R., Shen, P. R., Sheng, X. D., Shi, F., Surdo, A., Tan, Y. H., Vallania, P., Vernetto, S., Vigorito, C., Wang, H., Wu, C. Y., Wu, H. R., Xue, L., Yang, Q. Y., Yang, X. C., Yao, Z. G., Yuan, A. F., Zha, M., Zhang, H. M., Zhang, L., Zhang, X. Y., Zhang, Y., Zhao, J., Zhaxiciren, Null, Zhaxisangzhu, Null, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., Bartoli, B., Catalanotti, S., D'Amone, A., Danzengluobu, Mitri, I. D., Piazzoli, B. D., Girolamo, T. D., Sciascio, G. D., Feng, Z., Hu, H., Iacovacci, M., Labaciren, Zhaxiciren, Zhaxisangzhu, ITA, Mitri, I. De, Piazzoli, B. D'Ettorre, and Girolamo, T. Di

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Solar minimum, Physics, cosmic rays, methods: data analysis, methods: observational, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, observational [methods], Phase (waves), FOS: Physical sciences, Flux, Cosmic ray, Astrophysics, Astronomy and Astrophysic, Amplitude, Air shower, data analysi [methods], Astrophysics - High Energy Astrophysical Phenomena, Anisotropy, Event (particle physics), cosmic ray
Abstract

This paper reports on the measurement of the large-scale anisotropy in the distribution of cosmic-ray arrival directions using the data collected by the air shower detector ARGO-YBJ from 2008 January to 2009 December,during the minimum of solar activity between cycles 23 and 24. In this period, more than 200 billion showers were recorded with energies between 1 and 30 TeV. The observed two-dimensional distribution of cosmic rays is characterized by two wide regions of excess and deficit, respectively, both of relative intensity 0.001 with respect to a uniform flux, superimposed on smaller size structures. The harmonic analysis shows that the large-scale cosmic-ray relative intensity as a function of R.A. can be described by the first and second terms of a Fouries series. The high event statistics allow the study of the energy dependence of the anistropy, showing that the amplitude increases with energy, with a maximum intensity at 10 TeV, and then decreases while the phase slowly shifts toward lower values of R.A. with increasing energy. The ARGO-YBJ data provide accurate observations over more than a decade of energy around this feature of the anisotropy spectrum., Comment: 9pages, 6figures

Published
2015
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19. CRAB NEBULA: FIVE-YEAR OBSERVATION WITH ARGO-YBJ

Author

X. C. Yang, B. Bartoli, R. Cardarelli, X. Y. Zhang, G. Marsella, B. D'Ettorre Piazzoli, Minghui Liu, Zhenyong Feng, H. H. He, C. Y. Wu, L. Xue, Q. B. Gou, Q. Y. Yang, M. Iacovacci, M. Zha, G. Zizzi, P. Salvini, L. Perrone, X. D. Sheng, Paolo Bernardini, J. W. Zhao, H. R. Wu, Piero Vallania, P. Creti, H. Y. Jia, Paolo Camarri, I. De Mitri, Zihuang Cao, L. Zhang, T. L. Chen, Haifeng Li, Cunfeng Feng, M. Panareo, S. M. Mari, B. Z. Dai, Pengnian Shen, Lanqing Ma, Z. G. Yao, F. Ruggieri, Danzengluobu, S. Catalanotti, Hongbo Hu, A. Surdo, Yicheng Guo, A. Budano, Y. H. Tan, S. W. Cui, R. Santonico, X. J. Bi, Fudong Shi, Chang-Chun Ning, X. H. Ma, H. Lu, P. Branchini, Zhaoyang Feng, G. Liguori, S. Z. Chen, S. Mastroianni, G. Mancarella, Paolo Montini, F. R. Zhu, R. Iuppa, C. X. Liu, S. Vernetto, G. Di Sciascio, E. Striani, Q. Q. Zhu, H. W. Wang, A. D'Amone, J. K. K. Liu, Zhaxiciren, Labaciren, A. F. Yuan, P. Pistilli, H. M. Zhang, X. X. Zhou, Haibing Hu, Y. Zhang, D. Martello, Carlo Vigorito, T. Di Girolamo, Zhaxisangzhu, ITA, Bartoli, B., Bernardini, P., Bi, X. J., Branchini, P., Budano, A., Camarri, P., Cao, Z., Cardarelli, R., Catalanotti, S., Chen, S. Z., Chen, T. L., Creti, P., Cui, S. W., Dai, B. Z., D'Amone, A., Danzengluobu, De Mitri, I., D'Ettorre Piazzoli, B., Di Girolamo, T., Di Sciascio, G., Feng, C. F., Feng, Zhaoyang, Feng, Zhenyong, Gou, Q. B., Guo, Y. Q., He, H. H., Hu, Haibing, Hu, Hongbo, Iacovacci, M., Iuppa, R., Jia, H. Y., Labaciren, Li, H. J., Liguori, G., Liu, C., Liu, J., Liu, M. Y., Lu, H., Ma, L. L., Ma, X. H., Mancarella, G., Mari, S. M., Marsella, G., Martello, D., Mastroianni, S., Montini, P., Ning, C. C., Panareo, M., Perrone, L., Pistilli, P., Ruggieri, F., Salvini, P., Santonico, R., Shen, P. R., Sheng, X. D., Shi, F., Surdo, A., Tan, Y. H., Vallania, P., Vernetto, S., Vigorito, C., Wang, H., Wu, C. Y., Wu, H. R., Xue, L., Yang, Q. Y., Yang, X. C., Yao, Z. G., Yuan, A. F., Zha, M., Zhang, H. M., Zhang, L., Zhang, X. Y., Zhang, Y., Zhao, J., Zhaxisangzhu, Zhaxiciren, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., Zizzi, G., Striani, E., B., Bartoli, Bernardini, Paolo, X. J., Bi, P., Branchini, A., Budano, P., Camarri, Z., Cao, R., Cardarelli, S., Catalanotti, S. Z., Chen, T. L., Chen, P., Creti, S. W., Cui, B. Z., Dai, D'Amone, Antonio, DE MITRI, Ivan, B., D'Ettorre Piazzoli, T., Di Girolamo, G., Di Sciascio, C. F., Feng, Zhaoyang, Feng, Zhenyong, Feng, Q. B., Gou, Y. Q., Guo, H. H., He, Haibing, Hu, Hongbo, Hu, M., Iacovacci, R., Iuppa, H. Y., Jia, H. J., Li, G., Liguori, C., Liu, J., Liu, M. Y., Liu, H., Lu, L. L., Ma, X. H., Ma, Mancarella, Giovanni, S. M., Mari, Marsella, Giovanni, Martello, Daniele, S., Mastroianni, P., Montini, C. C., Ning, Panareo, Marco, Perrone, Lorenzo, P., Pistilli, F., Ruggieri, P., Salvini, R., Santonico, P. R., Shen, X. D., Sheng, F., Shi, A., Surdo, Y. H., Tan, P., Vallania, S., Vernetto, C., Vigorito, H., Wang, C. Y., Wu, H. R., Wu, L., Xue, Q. Y., Yang, X. C., Yang, Z. G., Yao, A. F., Yuan, M., Zha, H. M., Zhang, L., Zhang, X. Y., Zhang, Y., Zhang, J., Zhao, Zhaxiciren, Zhaxisangzhu, X. X., Zhou, F. R., Zhu, Q. Q., Zhu, G., Zizzi, E., Striani, Bartoli, Bruno, Catalanotti, Sergio, Danzengluobu, Null, D'ETTORRE PIAZZOLI, Benedetto, DI GIROLAMO, Tristano, Iacovacci, Michele, Labaciren, Null, Zhaxiciren, Null, and Zhaxisangzhu, Null

Subjects
Physics, Spectral index, Astrophysics::High Energy Astrophysical Phenomena, Settore FIS/01 - Fisica Sperimentale, individual (Crab Nebula) [pulsars], Flux, Astronomy and Astrophysics, Astrophysics, Light curve, Power law, star [gamma rays], Air shower, Crab Nebula, Pulsar, Space and Planetary Science, Cutoff, High Energy Physics::Experiment, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The ARGO-YBJ air shower detector monitored the Crab Nebula gamma ray emission from 2007 November to 2013 February. The integrated signal, consisting of $\sim$3.3 $\times$ 10$^5$ events,reached the statistical significance of 21.1 standard deviations. The obtained energy spectrum in the energy range 0.3-20 TeV can be described by a power law function dN/dE = I$_0$ (E / 2 TeV)$^{-\alpha}$, with a flux normalization I$_0$ = (5.2 $\pm$ 0.2) $\times$ 10$^{-12}$ photons cm$^{-2}$ s$^{-1}$ TeV$^{-1}$ and $\alpha$ = 2.63 $\pm$ 0.05, corresponding to an integrated flux above 1 TeV of 1.97 $\times$ 10$^{-11}$ photons cm$^{-2}$ s$^{-1}$. The systematic error is estimated to be less than 30$\%$ for the flux normalization and 0.06 for the spectral index. Assuming a power law spectrum with an exponential cutoff dN/dE = I$_0$ (E / 2 TeV)$^{-\alpha}$ $\exp$ (-E / E$_{cut}$), the lower limit of the cutoff energy E$_{cut}$ is 12 TeV, at 90$\%$ confidence level. Our extended dataset allows the study of the TeV emission over long timescales. Over five years, the light curve of the Crab Nebula in 200-day bins is compatible with a steady emission with a probability of 7.3 $\times$ 10$^{-2}$. A correlated analysis with Fermi-LAT data over $\sim$4.5 years using the light curves of the two experiments gives a Pearson correlation coefficient $r$ = 0.56 $\pm$ 0.22. Concerning flux variations on timescales of days, a "blind" search for flares with a duration of 1-15 days gives no excess with a significance higher than four standard deviations. The average rate measured by ARGO-YBJ during the three most powerful flares detected by Fermi-LAT is 205 $\pm$ 91 photons day$^{-1}$, consistent with the average value of 137 $\pm$ 10 day$^{-1}$., Comment: 12 pages, 10 figures

Published
2015
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