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1. 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$-$000 should be further investigated as a new candidate for a Galactic PeV cosmic-ray accelerator, PeVatron., Comment: 10 pages, 2 figures, Accepted for publication from the Astrophysical Journal
Published: 2023
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2. Measurement of the Gamma-Ray Energy Spectrum beyond 100 TeV from the HESS J1843$-$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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3. 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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4. Search for gamma-ray emission from the Sun during solar minimum with the ARGO-YBJ experiment

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., Piazzoli, B. D'Ettorre, 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., Li, Z., Liu, C., Liu, J., Liu, M. Y., Lu, H., Ma, L. L., Ma, X. ., 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, Zhaxisangzhu, Zhou, X. X., Zhu, F. R., and Zhu, Q. Q.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The hadronic interaction of cosmic rays with solar atmosphere can produce high energy gamma rays. The gamma-ray luminosity is correlated both with the flux of primary cosmic rays and the intensity of the solar magnetic field. The gamma rays below 200 GeV have been observed by $Fermi$ without any evident energy cutoff. The bright gamma-ray flux above 100 GeV has been detected only during solar minimum. The only available data in TeV range come from the HAWC observations, however outside the solar minimum. The ARGO-YBJ dataset has been used to search for sub-TeV/TeV gamma rays from the Sun during the solar minimum from 2008 to 2010, the same time period covered by the Fermi data. A suitable model containing the Sun shadow, solar disk emission and inverse-Compton emission has been developed, and the chi-square minimization method was used to quantitatively estimate the disk gamma-ray signal. The result shows that no significant gamma-ray signal is detected and upper limits to the gamma-ray flux at 0.3$-$7 TeV are set at 95\% confidence level. In the low energy range these limits are consistent with the extrapolation of the Fermi-LAT measurements taken during solar minimum and are compatible with a softening of the gamma-ray spectrum below 1 TeV. They provide also an experimental upper bound to any solar disk emission at TeV energies. Models of dark matter annihilation via long-lived mediators predicting gamma-ray fluxes > $10^{-7}$ GeV $cm^{-2}$ $s^{-1}$ below 1 TeV are ruled out by the ARGO-YBJ limits.
Published: 2019
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5. A Regulatory sRNA rli41 is Implicated in Cell Adhesion, Invasion and Pathogenicity in Listeria monocytogenes

Author: Wang, L. X., Ji, C. H., Ning, C. C., Liu, Y. C., Li, Z. Y., Sun, Y. Q., Xia, X. Z., Cai, X. P., Meng, Q. L., and Qiao, J.
Published: 2022
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6. Galactic Cosmic-Ray Anisotropy in the Northern hemisphere from the ARGO-YBJ Experiment during 2008-2012

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., Piazzoli, B. D'Ettorre, Di Girolamo, T., Di Sciascio, G., Feng, C. F., Feng, Z. Y., 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., Ruffolo, D., 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, Zhaxisangzhu, Zhou, X. X., Zhu, F. R., and Zhu, Q. Q.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: This paper reports on the observation of the sidereal large-scale anisotropy of cosmic rays using data collected by the ARGO-YBJ experiment over 5 years (2008$-$2012). This analysis extends previous work limited to the period from 2008 January to 2009 December,near the minimum of solar activity between cycles 23 and 24.With the new data sample the period of solar cycle 24 from near minimum to maximum is investigated. A new method is used to improve the energy reconstruction, allowing us to cover a much wider energy range, from 4 to 520 TeV. Below 100 TeV, the anisotropy is dominated by two wide regions, the so-called "tail-in" and "loss-cone" features. At higher energies, a dramatic change of the morphology is confirmed. The yearly time dependence of the anisotropy is investigated. Finally, no noticeable variation of cosmic-ray anisotropy with solar activity is observed for a median energy of 7 TeV.
Published: 2018
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7. Observation of the thunderstorm-related ground cosmic ray flux variations by ARGO-YBJ

Author: Bartoli, B., Bernardini, P., Bi, X. J., Cao, Z., Catalanotti, S., Chen, S. Z., Chen, T. L., Cui, S. W., Dai, B. Z., Amone, A. D, Luobu, Danzeng, De Mitri, I., Piazzoli, B. D Ettorre, 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., Ren, Labaci, 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., Ren, Zhaxici, Zhu, Zhaxisang, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., and Alessandro, F. D.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: A correlation between the secondary cosmic ray flux and the near-earth electric field intensity, measured during thunderstorms, has been found by analyzing the data of the ARGO-YBJ experiment, a full coverage air shower array located at the Yangbajing Cosmic Ray Laboratory (4300 m a. s. l., Tibet, China). The counting rates of showers with different particle multiplicities, have been found to be strongly dependent upon the intensity and polarity of the electric field measured during the course of 15 thunderstorms. In negative electric fields (i.e. accelerating negative charges downwards), the counting rates increase with increasing electric field strength. In positive fields, the rates decrease with field intensity until a certain value of the field EFmin (whose value depends on the event multiplicity), above which the rates begin increasing. By using Monte Carlo simulations, we found that this peculiar behavior can be well described by the presence of an electric field in a layer of thickness of a few hundred meters in the atmosphere above the detector, which accelerates/decelerates the secondary shower particles of opposite charge, modifying the number of particles with energy exceeding the detector threshold. These results, for the first time, give a consistent explanation for the origin of the variation of the electron/positron flux observed for decades by high altitude cosmic ray detectors during thunderstorms., Comment: 17 pages, 11 figures. The paper has been accepted by PRD
Published: 2017
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8. EAS age determination from the study of the lateral distribution of charged particles near the shower axis with the ARGO-YBJ experiment

Author: Collaboration, ARGO-YBJ, 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., 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, 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, Zhaxisangzhu, Zhou, X. X., Zhu, F. R., and Zhu, Q. Q.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, High Energy Physics - Experiment
Abstract: The ARGO-YBJ experiment, a full coverage extensive air shower (EAS) detector located at high altitude (4300 m a.s.l.) in Tibet, China, has smoothly taken data, with very high stability, since November 2007 to the beginning of 2013. The array consisted of a carpet of about 7000 m$^2$ Resistive Plate Chambers (RPCs) operated in streamer mode and equipped with both digital and analog readout, providing the measurement of particle densities up to few particles per cm$^2$. The unique detector features (full coverage, readout granularity, wide dynamic range, etc) and location (very high altitude) allowed a detailed study of the lateral density profile of charged particles at ground very close to the shower axis and its description by a proper lateral distribution function (LDF). In particular, the information collected in the first 10 m from the shower axis have been shown to provide a very effective tool for the determination of the shower development stage ("age") in the energy range 50 TeV - 10 PeV. The sensitivity of the age parameter to the mass composition of primary Cosmic Rays is also discussed.
Published: 2017
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9. 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., Amone, A. D, Luobu, Danzeng, De Mitri, I., Piazzoli, B. D Ettorre, 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., Ren, Labaci, 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., Ren, Zhaxici, Zhu, Zhaxisang, Zhou, X. X., Zhu, F. R., and Zhu, Q. Q.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Phenomenology
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., Comment: 24pages and 12 figures
Published: 2017
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10. Detection of thermal neutrons with the PRISMA-YBJ array in Extensive Air Showers selected by the ARGO-YBJ experiment

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., 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, 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, Zhaxisangzhu, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., Stenkin, . Yu. V., Alekseenko, V. V., Aynutdinov, V., Cai, Z. Y., Guo, X. W., Liu, Y., Rulev, V., Shchegolev, O. B., Stepanov, V., Volchenko, V., and Zhang, H.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Physics - Instrumentation and Detectors
Abstract: We report on a measurement of thermal neutrons, generated by the hadronic component of extensive air showers (EAS), by means of a small array of EN-detectors developed for the PRISMA project (PRImary Spectrum Measurement Array), novel devices based on a compound alloy of ZnS(Ag) and $^{6}$LiF. This array has been operated within the ARGO-YBJ experiment at the high altitude Cosmic Ray Observatory in Yangbajing (Tibet, 4300 m a.s.l.). Due to the tight correlation between the air shower hadrons and thermal neutrons, this technique can be envisaged as a simple way to estimate the number of high energy hadrons in EAS. Coincident events generated by primary cosmic rays of energies greater than 100 TeV have been selected and analyzed. The EN-detectors have been used to record simultaneously thermal neutrons and the air shower electromagnetic component. The density distributions of both components and the total number of thermal neutrons have been measured. The correlation of these data with the measurements carried out by ARGO-YBJ confirms the excellent performance of the EN-detector., Comment: 35 pages, 16 figures
Published: 2015
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11. 4.5 years multi-wavelength observations of Mrk 421 during the ARGO-YBJ and Fermi common operation time

Author: Bartoli, B., Bernardini, P., Bi, X. J., Cao, Z., Catalanotti, S., Chen, S. Z., Chen, T. L., Cui, S. W., Dai, B. Z., Damone, A., Danzengluobu, 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, 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, Zhaxisangzhu, Zhou, X. X., Zhu, F. R., and Zhu, Q. Q.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
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., Comment: 17 pages, 9 figures, 5 tables, Accepted for publication in ApJS
Published: 2015
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12. Study of the diffuse gamma-ray emission from the Galactic plane with ARGO-YBJ

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, 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, 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, Zhaxisangzhu, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., and Zizzi, G.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Phenomenology
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
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13. The analog Resistive Plate Chamber detector of the ARGO-YBJ experiment

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., 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, Li, H. J., Liu, C., Liu, J., Liu, M. Y., Lu, H., Ma, L. L., Ma, X. H., Mancarella, G., Mari1, S. M., Marsella, G., Mastroianni, S., Montini, P., Ning, C. C., Perrone, L., Pistilli, P., Salvini1, 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, Zhaxisangzhu, Zhou, X. X., Zhu, F. R., and Zhu, Q. Q.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Instrumentation and Detectors
Abstract: The ARGO-YBJ experiment has been in stable data taking from November 2007 till February 2013 at the YangBaJing Cosmic Ray Observatory (4300 m a.s.l.). The detector consists of a single layer of Resistive Plate Chambers (RPCs) ( about 6700 m^2}) operated in streamer mode. The signal pick-up is obtained by means of strips facing one side of the gas volume. The digital readout of the signals, while allows a high space-time resolution in the shower front reconstruction, limits the measurable energy to a few hundred TeV. In order to fully investigate the 1-10 PeV region, an analog readout has been implemented by instrumenting each RPC with two large size electrodes facing the other side of the gas volume. Since December 2009 the RPC charge readout has been in operation on the entire central carpet (about 5800 m^2). In this configuration the detector is able to measure the particle density at the core position where it ranges from tens to many thousands of particles per m^2. Thus ARGO-YBJ provides a highly detailed image of the charge component at the core of air showers. In this paper we describe the analog readout of RPCs in ARGO-YBJ and discuss both the performance of the system and the physical impact on the EAS measurements.
Published: 2015
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14. The cosmic ray proton plus helium energy spectrum measured by the ARGO-YBJ experiment in the energy range 3-300 TeV

Author: Collaboration, The ARGO-YBJ, 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., 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, 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., and Zhu, Q. Q.
Subjects: 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
Published: 2015
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15. Search for GeV Gamma Ray Bursts with the ARGO-YBJ Detector: Summary of Eight Years of Observations

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, 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, 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, Zhaxisangzhu, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., and Zizzi, G.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The search for Gamma Ray Burst (GRB) emission in the energy range 1-100 GeV in coincidence with the satellite detection has been carried out using the Astrophysical Radiation with Ground-based Observatory at YangBaJing (ARGO-YBJ) experiment. The high altitude location (4300 m a.s.l.), the large active surface ($\sim$ 6700 m$^2$ of Resistive Plate Chambers), the wide field of view ($\sim 2~$sr, limited only by the atmospheric absorption) and the high duty cycle ($>$ 86 %) make the ARGO-YBJ experiment particularly suitable to detect short and unexpected events like GRBs. With the scaler mode technique, i.e., counting all the particles hitting the detector with no measurement of the primary energy and arrival direction, the minimum threshold of $\sim$ 1 GeV can be reached, overlapping the direct measurements carried out by satellites. During the experiment lifetime, from December 17, 2004 to February 7, 2013, a total of 206 GRBs occurring within the ARGO-YBJ field of view (zenith angle $\theta$ $\le$ 45$^{\circ}$) have been analyzed. This is the largest sample of GRBs investigated with a ground-based detector. Two lightcurve models have been assumed and since in both cases no significant excess has been found, the corresponding fluence upper limits in the 1-100 GeV energy region have been derived, with values as low as 10$^{-5}~$erg cm$^{-2}$. The analysis of a subset of 24 GRBs with known redshift has been used to constrain the fluence extrapolation to the GeV region together with possible cutoffs under different assumptions on the spectrum., Comment: 43 pages, 6 figures, published in APJ
Published: 2015
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16. The 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, 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, 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, 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., and Zuo, X.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract: The measurement of cosmic ray energy spectra, in particular for individual species, is an essential approach in finding their origin. Locating the "knees" of the spectra is an important part of the approach and has yet to be achieved. Here we report a measurement of the mixed Hydrogen and Helium spectrum using the combination of the ARGO-YBJ experiment and of a prototype Cherenkov telescope for the LHAASO experiment. A knee feature at 640+/-87 TeV, with a clear steepening of the spectrum, is observed. This gives fundamental inputs to galactic cosmic ray acceleration models.
Published: 2015
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17. Identification of the TeV Gamma-ray Source ARGO J2031+4157 with the Cygnus Cocoon

Author: Collaboration, The ARGO-YBJ, 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., DAmone, A., Danzengluobu, De Mitri, I., Piazzoli, B. DEttorre, 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, P., Zhang, X. Y., Zhang, Y., Zhao, J., Zhaxiciren, Zhaxisangzhu, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., and Zizzi, G.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The extended TeV gamma-ray source ARGO J2031+4157 (or MGRO J2031+41) is positionally consistent with the Cygnus Cocoon discovered by $Fermi$-LAT at GeV energies in the Cygnus superbubble. Reanalyzing the ARGO-YBJ data collected from November 2007 to January 2013, the angular extension and energy spectrum of ARGO J2031+4157 are evaluated. After subtracting the contribution of the overlapping TeV sources, the ARGO-YBJ excess map is fitted with a two-dimensional Gaussian function in a square region of $10^{\circ}\times 10^{\circ}$, finding a source extension $\sigma_{ext}$= 1$^{\circ}$.8$\pm$0$^{\circ}$.5. The observed differential energy spectrum is $dN/dE =(2.5\pm0.4) \times 10^{-11}(E/1 TeV)^{-2.6\pm0.3}$ photons cm$^{-2}$ s$^{-1}$ TeV$^{-1}$, in the energy range 0.2-10 TeV. The angular extension is consistent with that of the Cygnus Cocoon as measured by $Fermi$-LAT, and the spectrum also shows a good connection with the one measured in the 1-100 GeV energy range. These features suggest to identify ARGO J2031+4157 as the counterpart of the Cygnus Cocoon at TeV energies. The Cygnus Cocoon, located in the star-forming region of Cygnus X, is interpreted as a cocoon of freshly accelerated cosmic rays related to the Cygnus superbubble. The spectral similarity with Supernova Remnants indicates that the particle acceleration inside a superbubble is similar to that in a SNR. The spectral measurements from 1 GeV to 10 TeV allows for the first time to determine the possible spectrum slope of the underlying particle distribution. A hadronic model is adopted to explain the spectral energy distribution., Comment: 16 pages, 3 figures, has been accepted by ApJ for publication
Published: 2014
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18. Energy Spectrum of Cosmic Protons and Helium Nuclei by a Hybrid Measurement at 4300 m a.s.l

Author: Bartoli, B., Bernardini, P., Bi, X. J., Bolognino, I., Branchini, P., Budano, A., Melcarne, A. K. Calabrese, 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., 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, 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., Panico, B., Perrone, L., Pistilli8, 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, 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., Collaboration, G. Zizzi for ARGO-YBJ, 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., and Collaboration, X. Zuo for LHAASO
Subjects: Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract: The energy spectrum of cosmic Hydrogen and Helium nuclei has been measured, below the so-called "knee", by using a hybrid experiment with a wide field-of-view Cherenkov telescope and the Resistive Plate Chamber (RPC) array of the ARGO-YBJ experiment at 4300 m above sea level. The Hydrogen and Helium nuclei have been well separated from other cosmic ray components by using a multi-parameter technique. A highly uniform energy resolution of about 25% is achieved throughout the whole energy range (100 TeV - 700 TeV). The observed energy spectrum is compatible with a single power law with index gamma=-2.63+/-0.06., Comment: To be published on Chinese Physics C
Published: 2014
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19. TeV gamma-ray survey of the Northern sky using the ARGO-YBJ detector

Author: Collaboration, The ARGO-YBJ, Bartoli, B., Bernardini, P., Bi, X. J., Bolognino, I., Branchini, P., Budano, A., Melcarne, A. K. Calabrese, 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, De Mitri, I., Piazzoli, B. DEttorre, 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., Vallania, P., 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., and Zizzi, G.
Subjects: 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
Published: 2013
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20. Observation of TeV gamma-rays from the unidentified source HESS J1841-055 with the ARGO-YBJ experiment

Author: Collaboration, The ARGO-YBJ, Bartoli, B., Bernardini, P., Bi, X. J., Bolognino, I., Branchini, P., Budano, A., Melcarne, A. K. Calabrese, 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., Staiti, G. DAli, DAmone, A., Danzengluobu, De Mitri, I., Piazzoli, B. DEttorre, Di Girolamo, T., Ding, X. H., Di Sciascio, G., Feng, C. F., Feng, Zhaoyang, Feng, Zhenyong, Galeazzi, F., 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, L. L., 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., 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., 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., and Zizzi, G.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report the observation of a very high energy \gamma-ray source, whose position is coincident with HESS J1841-055. This source has been observed for 4.5 years by the ARGO-YBJ experiment from November 2007 to July 2012. Its emission is detected with a statistical significance of 5.3 standard deviations. Parameterizing the source shape with a two-dimensional Gaussian function we estimate an extension \sigma=(0.40(+0.32,-0.22}) degree, consistent with the HESS measurement. The observed energy spectrum is dN/dE =(9.0-+1.6) x 10^{-13}(E/5 TeV)^{-2.32-+0.23} photons cm^{-2} s^{-1} TeV^{-1}, in the energy range 0.9-50 TeV. The integral \gamma-ray flux above 1 TeV is 1.3-+0.4 Crab units, which is 3.2-+1.0 times the flux derived by HESS. The differences in the flux determination between HESS and ARGO-YBJ, and possible counterparts at other wavelengths are discussed., Comment: 17 pages, 4 figures, have been accepted for publication in ApJ
Published: 2013
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21. Long-term Monitoring on Mrk 501 for Its VHE gamma Emission and a Flare in October 2011

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., Cardarelli, R., Catalanotti, S., Cattaneo, C., Chen, S. Z., Chen, T. L., Chen, Y., Creti, P., Cui, S. W., Dai, B. Z., Staiti, G. DAl, 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., 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, L. L., 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., 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., 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., and Zizzi, G.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: As one of the brightest active blazars in both X-ray and very high energy $\gamma$-ray bands, Mrk 501 is very useful for physics associated with jets from AGNs. The ARGO-YBJ experiment is monitoring it for $\gamma$-rays above 0.3 TeV since November 2007. Starting from October 2011 the largest flare since 2005 is observed, which lasts to about April 2012. In this paper, a detailed analysis is reported. During the brightest $\gamma$-rays flaring episodes from October 17 to November 22, 2011, an excess of the event rate over 6 $\sigma$ is detected by ARGO-YBJ in the direction of Mrk 501, corresponding to an increase of the $\gamma$-ray flux above 1 TeV by a factor of 6.6$\pm$2.2 from its steady emission. In particular, the $\gamma$-ray flux above 8 TeV is detected with a significance better than 4 $\sigma$. Based on time-dependent synchrotron self-Compton (SSC) processes, the broad-band energy spectrum is interpreted as the emission from an electron energy distribution parameterized with a single power-law function with an exponential cutoff at its high energy end. The average spectral energy distribution for the steady emission is well described by this simple one-zone SSC model. However, the detection of $\gamma$-rays above 8 TeV during the flare challenges this model due to the hardness of the spectra. Correlations between X-rays and $\gamma$-rays are also investigated., Comment: have been accepted for publication at ApJ
Published: 2012
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22. Observation of TeV gamma rays from the Cygnus region with the ARGO-YBJ experiment

Author: Bartoli, B., Bernardini, P., Bi, X. J., Bleve, C., Bolognino, I., Branchini, P., Budano, A., Melcarne, A. K. Calabrese, 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., 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., 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, L. L., 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., 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., 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., and Zizzi, G.
Subjects: 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., Comment: 14 pages, 4 figures
Published: 2012
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23. 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., and Zizzi, G.
Subjects: 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., Comment: 30 pages, 8 figures
Published: 2011
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24. Mean Interplanetary Magnetic Field Measurement Using the ARGO-YBJ Experiment

Author: Aielli, G., Bacci, C., Bartoli, B., Bernardini, P., Bi, X. J., Bleve, C., Branchini, P., Budano, A., Bussino, S., 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, De Vincenzi, M., Di Girolamo, T., Ding, X. H., Di Sciascio, G., Feng, C. F., Feng, Z. Y., Feng, Zhenyong, Galeazzi, F., Galeotti, P., Gargana, R., 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., Liberti, B., Liguori, G., Liu, C., Liu, C. Q., Liu, M. Y., Liu, J., Lu, H., Ma, X. H., Mancarella, G., Mari, S. M., Marsella, G., Martello, D., Mastroianni, S., Meng, X. R., Montini, P., Ning, C. C., Pagliaro, A., Panareo, M., Perrone, L., Pistilli, P., Qu, X. B., Rossi, E., Ruggieri, F., Saggese, L., 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., Yao, Z. G., Xu, B., Xue, L., Yan, Y. X., Yang, Q. Y., Yang, X. C., Yuan, A. F., Zha, M., Zhang, H. M., Zhang, JiLong, Zhang, JianLi, Zhang, L., Zhang, P., Zhang, X. Y., Zhang, Y., Zhaxisangzhu, Zhaxiciren, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., and Zizzi, G.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract: The sun blocks cosmic ray particles from outside the solar system, forming a detectable shadow in the sky map of cosmic rays detected by the ARGO-YBJ experiment in Tibet. Because the cosmic ray particles are positive charged, the magnetic field between the sun and the earth deflects them from straight trajectories and results in a shift of the shadow from the true location of the sun. Here we show that the shift measures the intensity of the field which is transported by the solar wind from the sun to the earth., Comment: 6 papges,3 figures
Published: 2011
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25. Observation of gamma rays from the northern celestial sky up to the sub-PeV range with the Tibet air shower array and its underground muon detector array

Author: Kato, Sei, primary, Amenomori, M, additional, Bao, Y W, additional, Bi, X J, additional, Chen, D, additional, Chen, T L, additional, Chen, W Y, additional, Chen, Xu, additional, Chen, Y, additional, Cirennima, C, additional, Cui, S W, additional, Danzengluobu, D, additional, Ding, L, additional, Fang, J H, additional, Fang, K, additional, Feng, C F, additional, Feng, Zhaoyang, additional, Feng, Z Y, additional, GAO, Qi, additional, Gou, Q B, additional, Guo, Y Q, additional, Hayashi, Y, additional, He, H H, additional, He, Z T, additional, Hibino, K, additional, Hotta, N, additional, Hu, Haibing, additional, Hu, H B, additional, Hu, K Y, additional, Huang, J, additional, Jia, H Y, additional, Jiang, L, additional, Jiang, P, additional, Jin, H B, additional, Kasahara, K, additional, Katayose, Y, additional, Kato, C, additional, Kato, S, additional, Kawahara, I, additional, Kawashima, T, additional, Kawata, K, additional, Kozai, M, additional, Labaciren, L, additional, Le, G M, additional, Li, A F, additional, Li, H J, additional, Li, W J, additional, Li, Y, additional, Lin, Y H, additional, Liu, B, additional, Liu, C, additional, Liu, J S, additional, Liu, L Y, additional, Liu, M Y, additional, Liu, W, additional, Lu, H, additional, Makishima, T, additional, Masuda, Y, additional, Matsuhashi, S, additional, Matsumoto, M, additional, Meng, X R, additional, Meng, Y, additional, Mizuno, A, additional, Munakata, K, additional, Nakamura, Y, additional, Nanjo, H, additional, Ning, C C, additional, Nishizawa, M, additional, Noguchi, R, additional, Ohnishi, M, additional, Okukawa, S, additional, Ozawa, S, additional, Qian, X, additional, Qu, X B, additional, Saito, T, additional, Sakata, M, additional, Sako, T, additional, Sasaki, T, additional, Shao, J, additional, Shibasaki, T, additional, Shibata, M, additional, Shiomi, A, additional, Sugimoto, H, additional, Takano, W, additional, Takita, M, additional, Tan, Y H, additional, Tateyama, N, additional, Torii, S, additional, Tsuchiya, H, additional, Udo, S, additional, Usui, R, additional, Wang, H, additional, Wang, S F, additional, Wang, Y P, additional, Wangdui, W, additional, Wu, H R, additional, Wu, Q, additional, Xu, J L, additional, Xue, L, additional, Yang, Z, additional, Yao, Y Q, additional, Yin, J, additional, Yokoe, Y, additional, Yu, Y L, additional, Yuan, A F, additional, Zhai, L M, additional, Zhang, H M, additional, Zhang, J L, additional, Zhang, X, additional, Zhang, Y, additional, Zhang, Yi, additional, Zhang, Ying, additional, Zhao, S P, additional, Zhaxisangzhu, Z, additional, Zhou, X X, additional, and Zou, Y H, additional
Published: 2023
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26. Cosmic ray shower rate variations detected by the ARGO-YBJ experiment during thunderstorms

Author: Axikegu, null, 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. D., Di Girolamo, T., Di Sciascio, G., Feng, C. F., 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., Axikegu, Bartoli, B, Bernardini, P, Bi, Xj, Cao, Z, Catalanotti, S, Chen, Sz, Chen, Tl, Cui, Sw, Dai, Bz, D'Amone, A, Danzengluobu, De Mitri, I, Piazzoli, Bdd, Di Girolamo, T, Di Sciacio, G, Feng, Cf, Feng, Zy, Gao, W, Gou, Qb, Guo, Yq, He, Hh, Hu, Hb, Iacovacci, M, Iuppa, R, Jia, Hy, Labaciren, Li, Hj, Liu, C, Liu, J, Liu, My, Lu, H, Ma, Ll, Ma, Xh, Mancarella, G, Mari, Sm, Marcella, G, Matroinni, S, Montini, P, Ning, Cc, Perrone, L, Pistilli, P, Salvini, P, Santonico, R, Shen, R, Sheng, Xd, Shi, F, Surdo, A, Tan, Yh, Vallania, P, Vemetto, S, Vkorito, C, Wang, H, Wu, Cy, Wu, R, Xue, L, Yang, Qy, Yang, Xc, Yao, Zg, Yuan, A, Zha, M, Zhang, Hm, Zhang, L, Zhang, Xy, Zhang, Y, Zhao, J, Zhaxiciren, Zhaxisangzhu, Zhou, Xx, Zhu, R, Zhu, Qq, Axikegu, Null, 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. D., Di Girolamo, T., Di Sciascio, G., Feng, C. F., 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., and Zhu, Q. Q.
Subjects: Cosmic ray, thunderstorm
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. The high altitude location and the frequent occurrence of thunderstorms, made ARGO-YBJ suitable to study the effects of atmospheric electric fields (AEF) on secondary cosmic rays. By analyzing the data of the ARGO-YBJ detector recorded during thunderstorms, significant variations of the rate of detected showers have been observed. During 20 thunderstorm episodes in 2012, the variations of the shower rates (both increases and decreases of amplitudes up to a few percent) are found to be correlated to the intensity and polarity of the AEF, and strongly dependent on the primary zenith angle. To understand the observed behavior, Monte Carlo simulations have been performed with CORSIKA and G4argo (a code based on GEANT4). We found that the data are well consistent with simulations, assuming the presence of a uniform electric field in a layer of thickness of 500 m in the atmosphere above the observation level. Due to the AEF accelerates/decelerates and deflects the secondary charged particles (mainly electrons and positrons) according to their charge, modifying the number and position of particles with energy exceeding the detector threshold. For the differences in electron and positron flux, spectrum, and lateral distribution, the AEF has an asymmetric effect on the shower particles, producing significant variations of the particle pattern on the ground, and, consequently, on the rate of detected showers, consistent with observations.
Published: 2022

27. Cosmic ray shower rate variations detected by the ARGO-YBJ experiment during thunderstorms

Author: Axikegu, 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. D., Di Girolamo T., Di Sciascio G., Feng C. F., Feng Z., Gao W., 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., 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., Axikegu, 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. D., Di Girolamo, T., Di Sciascio, G., Feng, C. F., Feng, Z., Gao, W., 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., 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., and Zhu, Q. Q.
Abstract: The ARGO-YBJ detector, located at the Yangbajing Cosmic Ray Laboratory (4300 m a. s. l., Tibet, China), was a full coverageair shower array. The high altitude location and the frequent occurrence of thunderstorms, made ARGO-YBJ suitable to study the effects of atmospheric electric fields (AEF) on secondary cosmic rays. By analyzing the data of the ARGO-YBJ detector recorded during thunderstorms, significant variations of the rate of detected showers have been observed. During 20 thunderstorm episodes in 2012, the variations of the shower rates (both increases and decreases of amplitudes up to a few percent) are found to be correlated to the intensity and polarity of the AEF, and strongly dependent on the primary zenith angle. To understand the observed behavior, Monte Carlo simulations have been performed with corsika and g4argo (a code based on geant4). We found that the data are well consistent with simulations, assuming the presence of a uniform electric field in a layer of thickness of 500 m in the atmosphere above the observation level. Due to the AEF accelerates/decelerates and deflects the secondary charged particles (mainly electrons and positrons) according to their charge, modifying the number and position of particles with energy exceeding the detector threshold. For the differences in electron and positron flux, spectrum, and lateral distribution, the AEF has an asymmetric effect on the shower particles, producing significant variations of the particle pattern on the ground, and, consequently, on the rate of detected showers, consistent with observations.
Published: 2022

28. Epidermal Growth Factor Enhances a Microsomal 12 — Lipoxygenase Activity in A431 Cells

Author: Chang, W. C., Ning, C. C., Lin, M. T., Huang, J. D., Nigam, Santosh, editor, Honn, Kenneth V., editor, Marnett, Lawrence J., editor, and Walden, Thomas L., Jr., editor
Published: 1993
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29. Metformin plus megestrol acetate compared with megestrol acetate alone as fertility‐sparing treatment in patients with atypical endometrial hyperplasia and well‐differentiated endometrial cancer: a randomised controlled trial

Author: Yang, B‐Y, primary, Gulinazi, Y, additional, Du, Y, additional, Ning, C‐C, additional, Cheng, Y‐L, additional, Shan, W‐W, additional, Luo, X‐Z, additional, Zhang, H‐W, additional, Zhu, Q, additional, Ma, F‐H, additional, Liu, J, additional, Sun, L, additional, Yu, M, additional, Guan, J, additional, and Chen, X‐J, additional
Published: 2020
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30. Mutations in TRPS1 gene in trichorhinophalangeal syndrome type I in Asian patients

Author: Chen, L-H., Ning, C-C., and Chao, S-C.
Published: 2010
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31. VizieR Online Data Catalog: M16 CO maps (Xu+, 2019)

Author: Xu, J. -L., Zavagno, Annie, Yu, N., Liu, X. -L., Xu, Y., Yuan, J., Zhang, C. -P., Zhang, S. -J., Zhang, G. -Y., Ning, C. -C., Ju, B. -G., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), and Rice University [Houston]
Subjects: [SDU]Sciences of the Universe [physics], H II regions, Carbon monoxide
Abstract: CO data are observed by using the PMO 13.7m radio telescope. We map a 45'x45' region centered at l=17.023°, b=0.871° in the transitions of ^12CO J=1-0 (115.271GHz), ^13CO J=1-0 (110.201GHz), and C^18O J=1-0 (109.782GHz) lines. \\\\(2 data files).
Published: 2019

32. EAS age determination from the study of the lateral distribution of charged particles near the shower axis with the ARGO-YBJ experiment

Author: 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, 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, 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, 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, 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, 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., and Zhu, Q. Q.
Subjects: Shower age, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Extensive air shower, FOS: Physical sciences, Cosmic ray, 01 natural sciences, High Energy Physics - Experiment, Nuclear physics, High Energy Physics - Experiment (hep-ex), 0103 physical sciences, Wide dynamic range, Extensive air showers, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Cosmic rays, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Range (particle radiation), 010308 nuclear & particles physics, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Charged particle, Computational physics, Distribution function, Air shower, Particle, Composition, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The ARGO-YBJ experiment, a full coverage extensive air shower (EAS) detector located at high altitude (4300 m a.s.l.) in Tibet, China, has smoothly taken data, with very high stability, since November 2007 to the beginning of 2013. The array consisted of a carpet of about 7000 m2 Resistive Plate Chambers (RPCs) operated in streamer mode and equipped with both digital and analog readout, providing the measurement of particle densities up to few particles per cm2. The unique detector features (full coverage, readout granularity, wide dynamic range, ..) and location (very high altitude) allowed a detailed study of the lateral density profile of charged particles at ground very close to the shower axis and its description by a proper lateral distribution function (LDF). In particular, the information collected in the first 10 m from the shower axis have been shown to provide a very effective tool for the determination of the shower development stage ("age") in the energy range 50 TeV - 10 PeV. The sensitivity of the age parameter to the mass composition of primary Cosmic Rays is also discussed.
Published: 2017

33. 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

34. The decolouration of methyl orange using aluminum foam, ultrasound and direct electric current

Author: Liu, C M, primary, Huang, X Y, additional, Zhang, H Y, additional, Dai, J D, additional, and Ning, C C, additional
Published: 2018
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35. Long-term Monitoring of the TeV Emission from Mrk 421 with the ARGO-YBJ Experiment

Author: Bartoli, B., Bernardini, P., X. J., Bi, Bleve, C., Bolognino, I., Branchini, P., Budano, A., Calabrese, A. K., 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., Danzengluobu, Dattoli, M., Mitri, I. D., Piazzoli, B. D., Girolamo, T. D., Ding, X. H., Sciascio, G. D., Feng, C. F., Feng, Z., Galeazzi, F., Galeotti, Piero, Giroletti, E., Gou, Q. B., Guo, Y. Q., H. H., He, Hu, H., Huang, Q., Iacovacci, M., Iuppa, R., James, I., 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., X. H., Ma, 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., X. B., Qu, 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, Carlo Francesco, Wang, B., Wang, H., C. Y., Wu, H. R., Wu, 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, J., Zhang, L., Zhang, P., Zhang, X. Y., Zhang, Y., Zhaxiciren, Zhaxisangzhu, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., Zizzi, G., and Collaboration, T. A.
Published: 2011

36. Analysis of Ferroresonant Overvoltages at Maanshan Nuclear Power Station in Taiwan

Author: Tsao, T.-P., primary and Ning, C.-C., additional
Published: 2006
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37. The Optimization of Spectrum Analysis for Signal Harmonics

Author: Tsao, T. P., primary, Wu, R. C., additional, and Ning, C. C., additional
Published: 2001
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38. Unusual overvoltages caused by the generating effect of induction motors.

Author: Tsao, T. P., Ning, C. C., and Smith, J. R.
Subjects: *NUCLEAR power plants, *OVERVOLTAGE, *INDUCTION motors, *OCEAN waves, *ELECTRIC power failures
Abstract: An overvoltage phenomenon that occurred at a nuclear power station in Taiwan is investigated. Simulations of the event reveal that two individual low-frequency overvoltages were caused by the interaction of induction motors (with flywheels) with the power line capacitance after they had lost power. Although these low-frequency overvoltages are insufficient to cause the failure of a circuit breaker they could have caused sufficient damage to the bushing insulation of the breaker that when a subsequent switching surge could cause the failure of the breaker. This failure lead to a blackout event. [ABSTRACT FROM AUTHOR]
Published: 2006
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39. 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

40. 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

41. First Measurements with the ARGO-YBJ Detector

Author: Surdo, A., Argo-Ybj, Collaboration, Bernardini, P., Bleve, C., Creti, P., Mitri, I., Devicenzi, M., Mancarella, G., Marsella, G., Martello, D., Panareo, M., Pino, C., Barone, F., Bartoli, B., Catalanotti, S., Cavaliere, S., D Ettorre Piazzoli, B., Di Girolamo, T., Di Sciascio, G., Iacovacci, M., Mastroianni, S., Milano, L., Rossi, E., Saggese, L., Cusomano, G., D Ali Staiti, G., Nicastro, L., Sacco, B., Liguori, G., Salvini, P., Aielli, G., Camarri, P., Cardelli, R., Cavaliere, A., Valerio D'Elia, Liberti, B., Santonico, R., Bacci, C., Bussino, S., Celio, P., Cesaroni, F., Marinis, E., Fratini, K., Mari, S. M., Pieri, L., Pistilli, P., Stanescu, C., Storini, M., Vallania, P., Vernetto, S., Gou, Q. B., He, H. H., Hu, H. B., Jing, C. L., Kuang, H. H., Lu, H., Shen, P. R., Sheng, X. D., Tan, Y. H., Wang, H., Wang, H. Y., Wu, C. Y., Zhang, H. M., Zhang, J. L., Zhang, Y., Zhu, Q. Q., Feng, C. F., He, M., Li, J. Y., Wang, Y. G., Xue, L., Zhang, N. J., Zhang, X. Y., Feng, Z. Y., Huang, Q., Jia, H. Y., Yu, G. C., Zhou, X. X., Danzengluobu, Ding, X. H., Guo, H. W., Hu, H., Labaciren, Meng, X. R., Ning, C. C., Yuan, A. F., Zhaxisangzhu, Gao, X. Y., Geng, Q. X., Liu, C. Q., Liu, J., Mu, J., Yangv, H. T., Yang, X. C., Zhang, L., Zhang, P., Bao, K. Z., Sun, L. R., Sun, S. C., Yue, X. D., Yao, Q. K., Ma, Y. M., Cheng, K. S., A., Surdo, P., Bernardini, C., Bleve, P., Creti, I., DE MITRI, DE VINCENZI, Mario, G., Mancarella, G., Marsella, D., Martello, M., Panareo, C., Pinto, F., Barone, B., Bartoli, S., Catalanotti, A., Cavaliere, B., D'ETTORRE PIAZZOLI, T., DI GIROLAMO, G., DI SCIASCIO, M., Iacovacci, S., Mastroianni, L., Milano, E., Rossi, L., Saggese, G., Cusumano, G., D'ALI STAITI, L., Nicastro, B., Sacco, G., Liguori, P., Salvini, G., Aielli, P., Camarri, R., Cardarelli, V., D'Elia, B., Liberti, R., Santonico, C., Bacci, Bussino, Severino Angelo Maria, P., Celio, F., Cesaroni, E., DE MARINIS, K., Fratini, Mari, Stefano Maria, L., Pieri, P., Pistilli, C., Stanescu, M., Storini, P., Vallania, S., Vernetto, Q. B., Gou, H. H., He, H. B., Hu, C. L., Jing, H. H., Kuang, H., Lu, P. R., Shen, X. D., Sheng, Y. H., Tan, H., Wang, H. Y., Wang, C. Y., Wu, H. M., Zhang, J. L., Zhang, Y., Zhang, Q. Q., Zhu, C. F., Feng, M., He, J. Y., Li, Y. G., Wang, L., Xue, N. J., Zhang, X. Y., Zhang, Z. Y., Feng, Q., Huang, H. Y., Jia, G. C., Yu, X. X., Zhou, Danzengluobu, X. H., Ding, H. W., Guo, H., Hu, Labaciren, X. R., Meng, C. C., Ning, A. F., Yuan, Zhaxisangzhu, X. Y., Gao, Q. X., Geng, C. Q., Liu, J., Liu, J., Mu, H. T., Yang, Q. Y., Yang, X. C., Yang, L., Zhang, P., Zhang, K. Z., Bao, L. R., Sun, S. C., Sun, X. D., Yue, Q. K., Yao, Y. M., Ma, and K. S., Cheng

42. Enhanced TeV gamma ray flux from the Crab Nebula observed

Author: Aielli, G., Camarri, P., Iuppa, R., Santonico, R., Bacci, C., Branchini, P., Budano, A., Bussino, S., Celio, P., Vincenzi, M., James, I., Mari, S. M., Montini, P., Pistilli, P., Bartoli, B., Catalanotti, S., D Ettorre Piazzoli, B., Di Girolamo, T., Iacovacci, M., Saggese, L., Bernardini, P., Bleve, C., Mitri, I., Mancarella, G., Marsella, G., Martello, D., Panareo, M., Perrone, L., Bi, X. J., Cao, Z., Chen, S. Z., Chen, Y., Feng, Zhaoyang, Gou, Q. B., Guo, Y. Q., He, H. H., Hu, Hongbo, Li, X. X., Liu, C., Lu, H., Ma, X. H., Shen, P. R., Sheng, X. D., Shi, F., Tan, Y. H., Wang, B., Wang, H., Wu, C. Y., Wu, H. R., Yao, Z. G., Zha, M., Zhang, H. M., Zhang, Jilong, Zhang, Jianli, Zhang, Y., Zhu, Q. Q., Calabrese Melcarne, A. K., Zizzi, G., Cappa, A., Piero Vallania, Vernetto, S., Cardarelli, R., Di Sciascio, G., Liberti, B., Cattaneo, C., Salvini, P., Creti, P., Surdo, A., Cui, S. W., Dai, B. Z., Liu, C. Q., Liu, J., Yang, Q. Y., Yang, X. C., Zhang, L., Zhang, P., D Ali Staiti, G., Chen, T. L., Danzengluobu, Ding, X. H., Hu, Haibing, Labaciren, Li, H. J., Liu, M. Y., Ning, C. C., Yuan, A. F., Zhaxisangzhu, Zhaxiciren, Dattoli, M., Vigorito, C., Feng, C. F., Li, J. Y., Qu, X. B., Xue, L., Zhang, X. Y., Feng, Zhenyong, Huang, Q., Jia, H. Y., Xu, B., Zhou, X. X., Zhu, F. R., Galeazzi, F., Gargana, R., Ruggieri, F., Stanescu, C., Galeotti, P., Giroletti, E., Liguori, G., Mastroianni, S., Rossi, E., and Pagliaro, A.

43. TeV flare from the blazar Mrk421 observed by ARGO-YBJ

Author: Bartoli, B., Bernardini, P., Bi, X. J., Bolognino, I., Branchini, P., Budano, A., Melcarne, A. K. Calabrese, 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., Staiti, G. D. Alí, D Amone, A., Danzengluobu, Mitri, I., D Ettorre Piazzoli, B., Di Girolamo, T., Ding, X. H., Di Sciascio, G., Feng, C. F., Feng, Zhaoyang, Feng, Zhenyong, Galeazzi, F., 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, L. L., 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., 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., and Zizzi, G.

44. ARGO-YBJ detects a VHE gamma-ray flare from Mrk501

Author: Bartoli, B., Bernardini, P., Bi, X. J., Bleve, C., Bolognino, I., Branchini, P., Budano, A., Melcarne, A. K. Calabrese, 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 Alí Staiti, G., Danzengluobu, Dattoli, M., Mitri, I., Piazzoli, B. D. Ettorre, Di Girolamo, T., Ding, X. H., Di Sciascio, G., Feng, C. F., Feng, Zhaoyang, Feng, Zhenyong, Galeazzi, F., 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., Ruggieri, F., Salvini, P., Santonico, R., Shen, P. R., Sheng, X. D., Shi, F., Stanescu, C., Surdo, A., Tan, Y. H., Vallania, P., Silvia Teresa Vernetto, 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., and Argo-Ybj, Collaboration

45. Enhanced TeV gamma ray flux from the Crab Nebula observed by the ARGO-YBJ experiment

Author: Bartoli, B., Bernardini, P., Bi, X. J., Bolognino, I., Branchini, P., Budano, A., Melcarne, A. K. Calabrese, 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., Staiti, G. D. Alí, D Amone, A., Danzengluobu, Mitri, I., D Ettorre Piazzoli, B., Di Girolamo, T., Ding, X. H., Di Sciascio, G., Feng, C. F., Feng, Zhaoyang, Feng, Zhenyong, Galeazzi, F., 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, L. L., 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., 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., and Zizzi, G.

46. Intrinsic linearity of bakelite Resistive Plate Chambers operated in streamer mode

Author: M. Iacovacci, L. L. Ma, X. H. Ma, Hongbo Hu, X. Y. Zhang, Minghui Liu, L. Perrone, Zihuang Cao, P. Creti, Haifeng Li, R. Santonico, Yicheng Guo, J. B. Zhao, P. Salvini, A. Budano, Chang-Chun Ning, Cunfeng Feng, Zhaoyang Feng, Fudong Shi, Z. G. Yao, C. Y. Wu, B. D'Ettorre Piazzoli, H. Lu, F. R. Zhu, S. Mastroianni, Danzengluobu, G. Di Sciascio, I. De Mitri, S. M. Mari, X. C. Yang, Piero Vallania, T. L. Chen, Zhaxiciren, G. Liguori, L. Xue, Paolo Camarri, Zhenyong Feng, B. Bartoli, C. X. Liu, H. W. Wang, Zhaxisangzhu, J. K. K. Liu, H. Y. Jia, Longzhou Zhang, Q. Q. Zhu, M. Zha, X. J. Bi, M. Panareo, G. Mancarella, S. W. Cui, S. Z. Chen, T. Di Girolamo, H. R. Wu, B. Z. Dai, F. Ruggieri, P. Branchini, Q. B. Gou, A. F. Yuan, Labaciren, Q. Y. Yang, G. Zizzi, H. H. He, Y. H. Tan, A. D'Amone, X. D. Sheng, Paolo Bernardini, Paolo Montini, R. Iuppa, R. Cardarelli, G. Marsella, S. Vernetto, Pengnian Shen, S. Catalanotti, P. Pistilli, H. M. Zhang, X. X. Zhou, A. Surdo, Carlo Vigorito, Haibing Hu, Y. Zhang, D. Martello, 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 Z., Gou Q. B., Guo Y. Q., He H. H., Hu H., 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., Zhaxiciren Zhaxisangzhu, Zhou X. X., Zhu F. R., Zhu Q. Q., Zizzi G., 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., 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., 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, Zhaxisangzhu, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., Zizzi, G., D’Amone, A., Danzengluobu, Null, D’Ettorre Piazzoli, B., Feng, Zhaoyang, Feng, Zhenyong, Hu, Haibing, Hu, Hongbo, Labaciren, Null, Zhaxiciren, Null, and Zhaxisangzhu, Null
Subjects: Nuclear and High Energy Physics, Physics::Instrumentation and Detectors, Intrinsic linearity, Streamer mode, Cosmic ray, Calorimetry, 01 natural sciences, chemistry.chemical_compound, Optics, 0103 physical sciences, Bakelite, Particle density, 010303 astronomy & astrophysics, Instrumentation, Physics, Resistive touchscreen, 010308 nuclear & particles physics, business.industry, Detector, Settore FIS/01 - Fisica Sperimentale, Linearity, RPC detector, Streamer mode, Intrinsic linearity, Calorimetry, chemistry, Particle, Physics::Accelerator Physics, RPC detector, business, Beam (structure)
Abstract: Resistive Plate Chambers have largely been used in High Energy Physics and Cosmic Ray research. In view of using this detector for calorimetry applications it is important to know the maximum measurable particle density, or its intrinsic linearity limit, which is tightly related to the dimension of the discharge region. In this paper we report the results of measurements performed at the Beam Test Facility (INFN National Laboratory of Frascati, Italy) where the intrinsic linearity of bakelite RPCs operated in streamer mode has been tested at different impinging particle densities.
Published: 2019

47. Search for Gamma-Ray Emission from the Sun during Solar Minimum with the ARGO-YBJ Experiment

Author: C. Y. Wu, Labaciren, Q. Y. Yang, P. Montini, X. H. Ma, C. C. Ning, Haifeng Li, C. Q. Liu, Q. B. Gou, Q. Q. Zhu, L. Zhang, T. L. Chen, Danzengluobu, C. Vigorito, P. Bernardini, R. Santonico, Zhaxisangzhu, Hongbo Hu, Yicheng Guo, A. Surdo, Y. H. Tan, P. R. Shen, X. C. Yang, H. Y. Jia, H. R. Wu, S. Catalanotti, B. Z. Dai, J. Zhao, Huihai He, Zhaoyang Feng, F. R. Zhu, P. Pistilli, H. M. Zhang, H. Lu, Minghui Liu, G. Di Sciascio, X. Y. Zhang, Zihou Li, G. Mancarella, I. De Mitri, T. Di Girolamo, Zhaxiciren, Xiangdong Sheng, R. Iuppa, S. W. Cui, A. F. Yuan, S. Vernetto, S. Z. Chen, A. D'Amone, Cunfeng Feng, H. Wang, S. Mastroianni, Y. J. Zhang, Haibing Hu, B. Bartoli, X. J. Bi, L. Perrone, J. K. K. Liu, L. L. Ma, W. Gao, M. Zha, Zhenyong Feng, X. X. Zhou, P. Vallania, B. D'Ettorre Piazzoli, L. Xue, Z. G. Yao, M. Iacovacci, Zhengguo Cao, F. Shi, P. Salvini, G. Marsella, S. M. Mari, 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., Piazzoli B. D., Girolamo T. D., Sciascio G. D., Feng C. F., Feng Z., Gao W., Gou Q. B., Guo Y. Q., He H. H., Hu H., Iacovacci M., Iuppa R., Jia H. Y., Labaciren, Li H. J., Li Z., 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 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., Mitri, I. D., Piazzoli, B. D., Girolamo, T. D., Sciascio, G. D., Feng, C. F., Feng, Z., Gao, W., Gou, Q. B., Guo, Y. Q., He, H. H., Hu, H., Iacovacci, M., Iuppa, R., Jia, H. Y., Li, H. J., Li, Z., 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, Zhaxisangzhu, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., D’Amone, A., Danzengluobu, Null, Mitri, I. De, Piazzoli, B. D’Ettorre, Di Girolamo, T., Sciascio, G. Di, Feng, Zhaoyang, Feng, Zhenyong, Hu, Haibing, Hu, Hongbo, Labaciren, Null, Zhaxiciren, Null, and Zhaxisangzhu, Null
Subjects: Solar minimum, Sun: general, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cosmic ray, astroparticle physics, cosmic rays, gamma rays: general, 7. Clean energy, 01 natural sciences, Atmosphere, 0103 physical sciences, general [Sun], 010303 astronomy & astrophysics, Argo, cosmic ray, High Energy Astrophysical Phenomena (astro-ph.HE), Astroparticle physics, Physics, 010308 nuclear & particles physics, Settore FIS/01 - Fisica Sperimentale, Gamma ray, Astronomy, astroparticle physic, Astronomy and Astrophysics, 13. Climate action, Space and Planetary Science, High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, general [gamma rays]
Abstract: The hadronic interaction of cosmic rays with solar atmosphere can produce high energy gamma-rays. The gamma-ray luminosity is correlated both with the flux of primary cosmic rays and the intensity of the solar magnetic field. The gamma-rays below 200 GeV have been observed by Fermi without any evident energy cutoff. The bright gamma-ray flux above 100 GeV has been detected only during solar minimum. The only available data in the TeV range come from the HAWC observations, however, outside the solar minimum. The ARGO-YBJ data set has been used to search for sub-TeV/TeV gamma-rays from the Sun during the solar minimum from 2008 to 2010, the same time period covered by the Fermi data. A suitable model containing the Sun shadow, solar disk emission, and inverse-Compton emission has been developed, and the chi-square minimization method was used to quantitatively estimate the disk gamma-ray signal. The result shows that no significant gamma-ray signal is detected and upper limits to the gamma-ray flux at 0.3-7 TeV are set at the 95% confidence level. In the low energy range these limits are consistent with the extrapolation of the Fermi-LAT measurements taken during solar minimum and are compatible with a softening of the gamma-ray spectrum below 1 TeV. They also provide an experimental upper bound to any solar disk emission at TeV energies. Models of dark matter annihilation via long-lived mediators predicting gamma-ray fluxes >10-7 GeV cm-2 s-1 below 1 TeV are ruled out by the ARGO-YBJ limits.
Published: 2019

48. Evidence of a geomagnetic effect on extensive air showers detected with the ARGO-YBJ experiment

Author: MARI, Stefano Maria, B. Bartoli1, 2, P. Bernardini3, 4, X. .J. Bi5, I. Bolognino6, 7, P. Branchini8, A. Budano8, A. .K. Calabrese Melcarne3, P. Camarri9, Z. Cao5, R. Cardarelli10, S. Catalanotti1, S. .Z. Chen5, T. .L. Chen11, Y. Chen5, P. Creti4, S. .W. Cui12, B. .Z. Dai13, A. D’Amone3, 4, Danzengluobu11, I. De Mitri3, B. D’Ettorre Piazzoli1, T. Di Girolamo1, X. .H. Ding11, G. Di Sciascio10, C. .F. Feng14, Zhaoyang Feng5, Zhenyong Feng15, Q. .B. Gou5, Y. .Q. Guo5, H. .H. He5, Haibing Hu11, Hongbo Hu5, Q. Huang15, M. Iacovacci1, R. Iuppa9, H. .Y. Jia15, Labaciren11, H. .J. Li11, J. .Y. Li14, X. .X. Li5, G. Liguori6, C. Liu5, C. .Q. Liu13, J. Liu13, M. .Y. Liu11, H. Lu5, X. .H. Ma5, G. Mancarella3, SM Mari 8, G. Marsella3, D. Martello3, S. Mastroianni2, P. Montini8, C. .C. Ning11, M. Panareo3, B. Panico9, L. Perrone3, P. Pistilli8, F. Ruggieri8, P. Salvini7, R. Santonico9, S. .N. Sbano3, P. .R. Shen5, X. .D. Sheng5, F. Shi5, A. Surdo4, Y. .H. Tan5, P. Vallania17, S. Vernetto17, C. Vigorito18, B. Wang5, H. Wang5, C. .Y. Wu5, H. .R. Wu5, B. Xu15, L. Xue14, Y. .X. Yan13, Q. .Y. Yang13, X. .C. Yang13, Z. .G. Yao5, A. .F. Yuan11, M. Zha5, H. .M. Zhang5, Jilong Zhang5, Jianli Zhang5, L. Zhang13, P. Zhang13, X. .Y. Zhang14, Y. Zhang5, Zhaxiciren11, Zhaxisangzhu11, X. .X. Zhou15, F. .R. Zhu15, Q. .Q. Zhu5, G. Zizzi20 ( 1Dipartimento di Fisica dell’Università di Napoli 'Federico II, ' Complesso Universitario di Monte Sant’Angelo, via Cinthia, 80126 Napoli, Italy 2Istituto Nazionale di Fisica Nucleare, Sezione di Napoli, Complesso Universitario di Monte Sant’Angelo, Italy 3Dipartimento Matematica e. Fisica 'Ennio De Giorgi, ' Università del Salento, via per Arnesano, 73100 Lecce, Italy 4Istituto Nazionale di Fisica Nucleare, Sezione di Lecce, Italy 5Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, P. O. Box 918, 100049 Beijing, People’s Republic of China 6Dipartimento di Fisica dell’Università di Pavia, via Bassi 6, 27100 Pavia, Italy 7Istituto Nazionale di Fisica Nucleare, Sezione di Pavia, Italy 8Istituto Nazionale di Fisica Nucleare, Sezione di Roma Tre, via della Vasca Navale 84, 00146 Roma, Italy 9Dipartimento di Fisica dell’Università di Roma 'Tor Vergata, ' via della Ricerca Scientifica 1, 00133 Roma, Italy 10Istituto Nazionale di Fisica Nucleare, Sezione di Roma Tor Vergata, via della Ricerca Scientifica 1, Italy 11Tibet University, 850000 Lhasa, Xizang, People’s Republic of China 12Hebei Normal University, Shijiazhuang 050016, Hebei, People’s Republic of China 13Yunnan University, 2 North Cuihu Road, 650091 Kunming, Yunnan, People’s Republic of China 14Shandong University, 250100 Jinan, Shandong, People’s Republic of China 15Southwest Jiaotong University, 610031 Chengdu, Sichuan, People’s Republic of China 16Dipartimento di Fisica dell’Università 'Roma Tre, ' via della Vasca Navale 84, Italy 17Istituto di Fisica dello Spazio Interplanetario dell’Istituto Nazionale di Astrofisica, corso Fiume 4, 10133 Torino, Italy 18Istituto Nazionale di Fisica Nucleare, Sezione di Torino, via Pietro Giuria 1, 10125 Torino, Italy 19Dipartimento di Fisica Generale dell’Università di Torino, Italy 20Istituto Nazionale di Fisica Nucleare CNAF, Viale Berti Pichat 6/2, 40127 Bologna, Italy, Mari, Stefano Maria, B., Bartoli1, P., Bernardini3, Bi5, X. . J., I., Bolognino6, P., Branchini8, A., Budano8, Calabrese Melcarne3, A. . K., P., Camarri9, Z., Cao5, R., Cardarelli10, S., Catalanotti1, Chen5, S. . Z., Chen11, T. . L., Y., Chen5, P., Creti4, Cui12, S. . W., Dai13, B. . Z., A., D’Amone3, 4, Danzengluobu11, I., De Mitri3, B., D’Ettorre Piazzoli1, T., Di Girolamo1, Ding11, X. . H., G., Di Sciascio10, Feng14, C. . F., Zhaoyang, Feng5, Zhenyong, Feng15, Gou5, Q. . B., Guo5, Y. . Q., He5, H. . H., Haibing, Hu11, Hongbo, Hu5, Q., Huang15, M., Iacovacci1, R., Iuppa9, Jia15, H. . Y., Labaciren11, Li11, H. . J., Li14, J. . Y., Li5, X. . X., G., Liguori6, C., Liu5, Liu13, C. . Q., J., Liu13, Liu11, M. . Y., H., Lu5, Ma5, X. . H., G., Mancarella3, SM Mari, 8, G., Marsella3, D., Martello3, S., Mastroianni2, Montini8, P., Ning11, C. . C., M., Panareo3, B., Panico9, L., Perrone3, P., Pistilli8, Ruggieri8, F., P., Salvini7, R., Santonico9, Sbano3, S. . N., Shen5, P. . R., Sheng5, X. . D., F., Shi5, A., Surdo4, Tan5, Y. . H., P., Vallania17, S., Vernetto17, C., Vigorito18, B., Wang5, H., Wang5, Wu5, C. . Y., Wu5, H. . R., B., Xu15, L., Xue14, Yan13, Y. . X., Yang13, Q. . Y., Yang13, X. . C., Yao5, Z. . G., Yuan11, A. . F., M., Zha5, Zhang5, H. . M., Jilong, Zhang5, Jianli, Zhang5, L., Zhang13, P., Zhang13, Zhang14, X. . Y., Y., Zhang5, Zhaxiciren11, Zhaxisangzhu11, Zhou15, X. . X., Zhu15, F. . R., Zhu5, Q. . Q., G., Zizzi20 ( 1Dipartimento di Fisica dell’Università di Napoli 'Federico II, ' Complesso Universitario di Monte, Sant’Angelo, Via, Cinthia, 80126, Napoli, Italy 2Istituto Nazionale di Fisica, Nucleare, Sezione di, Napoli, Complesso Universitario di Monte, Sant’Angelo, Italy 3Dipartimento Matematica e., Fisica 'Ennio De Giorgi, ' Università del, Salento, via per, Arnesano, 73100, Lecce, Italy 4Istituto Nazionale di Fisica, Nucleare, Sezione di, Lecce, Italy 5Key Laboratory of Particle, Astrophysic, Institute of High Energy, Physic, Chinese Academy of, Science, P. O., Box 918, 100049, Beijing, People’s Republic of China 6Dipartimento di Fisica dell’Università di, Pavia, via Bassi, 6, 27100, Pavia, Italy 7Istituto Nazionale di Fisica, Nucleare, Sezione di, Pavia, Italy 8Istituto Nazionale di Fisica, Nucleare, Sezione di Roma, Tre, via della Vasca Navale, 84, 00146, Roma, Italy 9Dipartimento di Fisica dell’Università di Roma 'Tor, Vergata, ' via della Ricerca Scientifica, 1, 00133, Roma, Italy 10Istituto Nazionale di Fisica, Nucleare, Sezione di Roma Tor, Vergata, via della Ricerca Scientifica, 1, Italy 11Tibet, University, 850000, Lhasa, Xizang, People’s Republic of China 12Hebei Normal, University, Shijiazhuang, 050016, Hebei, People’s Republic of China 13Yunnan, University, 2 North Cuihu, Road, 650091, Kunming, Yunnan, People’s Republic of China 14Shandong, University, 250100, Jinan, Shandong, People’s Republic of China 15Southwest Jiaotong, University, 610031, Chengdu, Sichuan, People’s Republic of China 16Dipartimento di Fisica dell’Università 'Roma, Tre, ' via della Vasca Navale, 84, Italy 17Istituto di Fisica dello Spazio Interplanetario dell’Istituto Nazionale di, Astrofisica, corso Fiume, 4, 10133, Torino, Italy 18Istituto Nazionale di Fisica, Nucleare, Sezione di, Torino, via Pietro Giuria, 1, 10125, Torino, Italy 19Dipartimento di Fisica Generale dell’Università di, Torino, Italy 20Istituto Nazionale di Fisica Nucleare, Cnaf, Viale Berti Pichat, 6/2, 40127, Bologna, Italy, B., Bartoli, Bernardini, Paolo, X. . J., Bi, I., Bolognino, P., Branchini, A., Budano, Calabrese Melcarne, A. . K., P., Camarri, Z., Cao, R., Cardarelli, S., Catalanotti, Chen, S. . Z., Chen, T. . L., Y., Chen, P., Creti, Cui, S. . W., Dai, B. . Z., A., D’Amone, Danzengluobu, DE MITRI, Ivan, B., D’Ettorre Piazzoli, T., Di Girolamo, Ding, X. . H., G., Di Sciascio, Feng, C. . F., Zhaoyang, Feng, Zhenyong, Feng, Gou, Q. . B., Guo, Y. . Q., H. . H., He, Haibing, Hu, Hongbo, Hu, Q., Huang, M., Iacovacci, R., Iuppa, Jia, H. . Y., Labaciren, H. . J., Li, J. . Y., Li, X. . X., Li, G., Liguori, C., Liu, Liu, C. . Q., J., Liu, Liu, M. . Y., H., Lu, X. . H., Ma, Mancarella, Giovanni, Mari, S. . M., Marsella, Giovanni, Martello, Daniele, S., Mastroianni, P., Montini, Ning, C. . C., Panareo, Marco, B., Panico, Perrone, Lorenzo, P., Pistilli, F., Ruggieri, P., Salvini, R., Santonico, Sbano, S. . N., Shen, P. . R., Sheng, X. . D., F., Shi, A., Surdo, Tan, Y. . H., P., Vallania, S., Vernetto, C., Vigorito, B., Wang, H., Wang, C. . Y., Wu, H. . R., Wu, B., Xu, L., Xue, Yan, Y. . X., Yang, Q. . Y., Yang, X. . C., Yao, Z. . G., Yuan, A. . F., M., Zha, Zhang, H. . M., Jilong, Zhang, Jianli, Zhang, L., Zhang, P., Zhang, Zhang, X. . Y., Y., Zhang, Zhaxiciren, Zhaxisangzhu, Zhou, X. . X., Zhu, F. . R., Zhu, Q. . Q., G., Zizzi, Bartoli, B., 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., De Mitri, I., D'Ettorre Piazzoli, B., DI GIROLAMO, Tristano, Ding, X. H., Di Sciascio, G., Feng, C. F., Gou, Q. B., Guo, Y. Q., H. H., He, Huang, Q., Iacovacci, Michele, Iuppa, R., Jia, H. Y., H. J., Li, J. Y., Li, X. X., Li, Liguori, G., Liu, C., Liu, C. Q., Liu, J., Liu, M. Y., Lu, H., 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., Yan, Y. X., Yang, Q. Y., Yang, X. C., Yao, Z. G., Yuan, A. F., Zha, M., Zhang, H. M., Zhang, L., Zhang, P., Zhang, X. Y., Zhang, Y., Zhou, X. X., Zhu, F. R., Zhu, Q. Q., and Zizzi, G.
Subjects: Physics, Nuclear and High Energy Physics, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Detector, Settore FIS/01 - Fisica Sperimentale, Geomagnetic field, cosmic ray, extensive air showers , azimuthal distribution, Astrophysics::Instrumentation and Methods for Astrophysics, Cosmic ray, Astrophysics, Charged particle, Azimuth, Earth's magnetic field, High Energy Physics::Experiment, Zenith, Argo
Abstract: The geomagnetic field causes not only the east-west effect on primary cosmic rays but also affects the trajectories of the secondary charged particles in the shower, causing their lateral distribution to be stretched. Thus, both the density of the secondaries near the shower axis and the trigger efficiency of detector arrays decrease. The effect depends on the direction of the showers, thus, introducing a modulation in the measured azimuthal distribution. The azimuthal distribution of the events collected by the ARGO-YBJ detector is deeply investigated for different zenith angles in light of this effect.
Published: 2014

49. 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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50. Galactic Cosmic-Ray Anisotropy in the Northern hemisphere from the ARGO-YBJ Experiment during 2008-2012

Author: J. Zhao, Hongbo Hu, P. R. Shen, X. C. Yang, A. Surdo, Yicheng Guo, Y. H. Tan, Zhaoyang Feng, F. R. Zhu, X. J. Bi, T. Di Girolamo, J. K. K. Liu, S. Vernetto, Zhaxisangzhu, Zhengguo Cao, S. Z. Chen, Q. Q. Zhu, L. Zhang, T. L. Chen, R. Santonico, S. Mastroianni, C. Vigorito, C. Y. Wu, S. W. Cui, C. Q. Liu, Q. B. Gou, C. C. Ning, P. Vallania, F. Shi, S. M. Mari, B. D'Ettorre Piazzoli, A. D'Amone, H. J. Li, H. R. Wu, Zhaxiciren, R. Iuppa, L. Xue, P. Salvini, G. Marsella, W. Gao, P. Bernardini, H. Wang, H. Lu, Danzengluobu, S. Catalanotti, David Ruffolo, A. F. Yuan, B. Z. Dai, Y. J. Zhang, Huihai He, M. Zha, G. Di Sciascio, X. Y. Zhang, Labaciren, Xiangdong Sheng, P. Pistilli, H. M. Zhang, Minghui Liu, I. De Mitri, Q. Y. Yang, P. Montini, X. H. Ma, X. X. Zhou, L. Perrone, Haibing Hu, L. L. Ma, H. Y. Jia, G. Mancarella, B. Bartoli, Cunfeng Feng, M. Iacovacci, Z. G. Yao, 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, Z. Y., 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., Ruffolo, D., 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., D'Amone, A., Piazzoli, B. D'Ettorre, Mastroianni, Stefano, Danzengluobu, null, Labaciren, null, Zhaxiciren, null, and Zhaxisangzhu, null
Subjects: Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cosmic ray, 01 natural sciences, cosmic rays, 0103 physical sciences, Anisotropy, 010303 astronomy & astrophysics, Argo, cosmic ray, Astroparticle physics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Settore FIS/01 - Fisica Sperimentale, Northern Hemisphere, Astronomy, astroparticle physic, Astronomy and Astrophysics, astroparticle physics, cosmic ray anysotropy, argo-ybj, Astronomy and Astrophysic, astroparticle physics, Space and Planetary Science, 13. Climate action, Astrophysics - High Energy Astrophysical Phenomena
Abstract: This paper reports on the observation of the sidereal large-scale anisotropy of cosmic rays using data collected by the ARGO-YBJ experiment over 5 years (2008-2012). This analysis extends previous work limited to the period from 2008 January to 2009 December, near the minimum of solar activity between cycles 23 and 24. With the new data sample, the period of solar cycle 24 from near minimum to maximum is investigated. A new method is used to improve the energy reconstruction, allowing us to cover a much wider energy range, from 4 to 520 TeV. Below 100 TeV, the anisotropy is dominated by two wide regions, the so-called “tail-in” and “loss-cone” features. At higher energies, a dramatic change of the morphology is confirmed. The yearly time dependence of the anisotropy is investigated. Finally, no noticeable variation of cosmic-ray anisotropy with solar activity is observed for a median energy of 7 TeV.
Published: 2018
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