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1. Detailed Report on the Measurement of the Positive Muon Anomalous Magnetic Moment to 0.20 ppm

Author

Aguillard, D. P., Albahri, T., Allspach, D., Anisenkov, A., Badgley, K., Baeßler, S., Bailey, I., Bailey, L., Baranov, V. A., Barlas-Yucel, E., Barrett, T., Barzi, E., Bedeschi, F., Berz, M., Bhattacharya, M., Binney, H. P., Bloom, P., Bono, J., Bottalico, E., Bowcock, T., Braun, S., Bressler, M., Cantatore, G., Carey, R. M., Casey, B. C. K., Cauz, D., Chakraborty, R., Chapelain, A., Chappa, S., Charity, S., Chen, C., Cheng, M., Chislett, R., Chu, Z., Chupp, T. E., Claessens, C., Convery, M. E., Corrodi, S., Cotrozzi, L., Crnkovic, J. D., Dabagov, S., Debevec, P. T., Di Falco, S., Di Sciascio, G., Donati, S., Drendel, B., Driutti, A., Duginov, V. N., Eads, M., Edmonds, A., Esquivel, J., Farooq, M., Fatemi, R., Ferrari, C., Fertl, M., Fienberg, A. T., Fioretti, A., Flay, D., Foster, S. B., Friedsam, H., Froemming, N. S., Gabbanini, C., Gaines, I., Galati, M. D., Ganguly, S., Garcia, A., George, J., Gibbons, L. K., Gioiosa, A., Giovanetti, K. L., Girotti, P., Gohn, W., Goodenough, L., Gorringe, T., Grange, J., Grant, S., Gray, F., Haciomeroglu, S., Halewood-Leagas, T., Hampai, D., Han, F., Hempstead, J., Hertzog, D. W., Hesketh, G., Hess, E., Hibbert, A., Hodge, Z., Hong, K. W., Hong, R., Hu, T., Hu, Y., Iacovacci, M., Incagli, M., Kammel, P., Kargiantoulakis, M., Karuza, M., Kaspar, J., Kawall, D., Kelton, L., Keshavarzi, A., Kessler, D. S., Khaw, K. S., Khechadoorian, Z., Khomutov, N. V., Kiburg, B., Kiburg, M., Kim, O., Kinnaird, N., Kraegeloh, E., Krylov, V. A., Kuchinskiy, N. A., Labe, K. R., LaBounty, J., Lancaster, M., Lee, S., Li, B., Li, D., Li, L., Logashenko, I., Campos, A. Lorente, Lu, Z., Lucà, A., Lukicov, G., Lusiani, A., Lyon, A. L., MacCoy, B., Madrak, R., Makino, K., Mastroianni, S., Miller, J. P., Miozzi, S., Mitra, B., Morgan, J. P., Morse, W. M., Mott, J., Nath, A., Ng, J. K., Nguyen, H., Oksuzian, Y., Omarov, Z., Osofsky, R., Park, S., Pauletta, G., Piacentino, G. M., Pilato, R. N., Pitts, K. T., Plaster, B., Počanić, D., Pohlman, N., Polly, C. C., Price, J., Quinn, B., Qureshi, M. U. H., Ramachandran, S., Ramberg, E., Reimann, R., Roberts, B. L., Rubin, D. L., Sakurai, M., Santi, L., Schlesier, C., Schreckenberger, A., Semertzidis, Y. K., Shemyakin, D., Sorbara, M., Stapleton, J., Still, D., Stöckinger, D., Stoughton, C., Stratakis, D., Swanson, H. E., Sweetmore, G., Sweigart, D. A., Syphers, M. J., Tarazona, D. A., Teubner, T., Tewsley-Booth, A. E., Tishchenko, V., Tran, N. H., Turner, W., Valetov, E., Vasilkova, D., Venanzoni, G., Volnykh, V. P., Walton, T., Weisskopf, A., Welty-Rieger, L., Winter, P., Wu, Y., Yu, B., Yucel, M., Zeng, Y., and Zhang, C.

Subjects
High Energy Physics - Experiment, High Energy Physics - Phenomenology, Nuclear Experiment
Abstract

We present details on a new measurement of the muon magnetic anomaly, $a_\mu = (g_\mu -2)/2$. The result is based on positive muon data taken at Fermilab's Muon Campus during the 2019 and 2020 accelerator runs. The measurement uses $3.1$ GeV$/c$ polarized muons stored in a $7.1$-m-radius storage ring with a $1.45$ T uniform magnetic field. The value of $ a_{\mu}$ is determined from the measured difference between the muon spin precession frequency and its cyclotron frequency. This difference is normalized to the strength of the magnetic field, measured using Nuclear Magnetic Resonance (NMR). The ratio is then corrected for small contributions from beam motion, beam dispersion, and transient magnetic fields. We measure $a_\mu = 116 592 057 (25) \times 10^{-11}$ (0.21 ppm). This is the world's most precise measurement of this quantity and represents a factor of $2.2$ improvement over our previous result based on the 2018 dataset. In combination, the two datasets yield $a_\mu(\text{FNAL}) = 116 592 055 (24) \times 10^{-11}$ (0.20 ppm). Combining this with the measurements from Brookhaven National Laboratory for both positive and negative muons, the new world average is $a_\mu$(exp) $ = 116 592 059 (22) \times 10^{-11}$ (0.19 ppm)., Comment: 48 pages, 29 figures; 4 pages of Supplement Material; version accepted for publication in Physical Review D

Published
2024

2. Measurement of the Positive Muon Anomalous Magnetic Moment to 0.20 ppm

Author

Aguillard, D. P., Albahri, T., Allspach, D., Anisenkov, A., Badgley, K., Baeßler, S., Bailey, I., Bailey, L., Baranov, V. A., Barlas-Yucel, E., Barrett, T., Barzi, E., Bedeschi, F., Berz, M., Bhattacharya, M., Binney, H. P., Bloom, P., Bono, J., Bottalico, E., Bowcock, T., Braun, S., Bressler, M., Cantatore, G., Carey, R. M., Casey, B. C. K., Cauz, D., Chakraborty, R., Chapelain, A., Chappa, S., Charity, S., Chen, C., Cheng, M., Chislett, R., Chu, Z., Chupp, T. E., Claessens, C., Convery, M. E., Corrodi, S., Cotrozzi, L., Crnkovic, J. D., Dabagov, S., Debevec, P. T., Di Falco, S., Di Sciascio, G., Drendel, B., Driutti, A., Duginov, V. N., Eads, M., Edmonds, A., Esquivel, J., Farooq, M., Fatemi, R., Ferrari, C., Fertl, M., Fienberg, A. T., Fioretti, A., Flay, D., Foster, S. B., Friedsam, H., Froemming, N. S., Gabbanini, C., Gaines, I., Galati, M. D., Ganguly, S., Garcia, A., George, J., Gibbons, L. K., Gioiosa, A., Giovanetti, K. L., Girotti, P., Gohn, W., Goodenough, L., Gorringe, T., Grange, J., Grant, S., Gray, F., Haciomeroglu, S., Halewood-Leagas, T., Hampai, D., Han, F., Hempstead, J., Hertzog, D. W., Hesketh, G., Hess, E., Hibbert, A., Hodge, Z., Hong, K. W., Hong, R., Hu, T., Hu, Y., Iacovacci, M., Incagli, M., Kammel, P., Kargiantoulakis, M., Karuza, M., Kaspar, J., Kawall, D., Kelton, L., Keshavarzi, A., Kessler, D. S., Khaw, K. S., Khechadoorian, Z., Khomutov, N. V., Kiburg, B., Kiburg, M., Kim, O., Kinnaird, N., Kraegeloh, E., Krylov, V. A., Kuchinskiy, N. A., Labe, K. R., LaBounty, J., Lancaster, M., Lee, S., Li, B., Li, D., Li, L., Logashenko, I., Campos, A. Lorente, Lu, Z., Lucà, A., Lukicov, G., Lusiani, A., Lyon, A. L., MacCoy, B., Madrak, R., Makino, K., Mastroianni, S., Miller, J. P., Miozzi, S., Mitra, B., Morgan, J. P., Morse, W. M., Mott, J., Nath, A., Ng, J. K., Nguyen, H., Oksuzian, Y., Omarov, Z., Osofsky, R., Park, S., Pauletta, G., Piacentino, G. M., Pilato, R. N., Pitts, K. T., Plaster, B., Počanić, D., Pohlman, N., Polly, C. C., Price, J., Quinn, B., Qureshi, M. U. H., Ramachandran, S., Ramberg, E., Reimann, R., Roberts, B. L., Rubin, D. L., Santi, L., Schlesier, C., Schreckenberger, A., Semertzidis, Y. K., Shemyakin, D., Sorbara, M., Stapleton, J., Still, D., Stöckinger, D., Stoughton, C., Stratakis, D., Swanson, H. E., Sweetmore, G., Sweigart, D. A., Syphers, M. J., Tarazona, D. A., Teubner, T., Tewsley-Booth, A. E., Tishchenko, V., Tran, N. H., Turner, W., Valetov, E., Vasilkova, D., Venanzoni, G., Volnykh, V. P., Walton, T., Weisskopf, A., Welty-Rieger, L., Winter, P., Wu, Y., Yu, B., Yucel, M., Zeng, Y., and Zhang, C.

Subjects
High Energy Physics - Experiment
Abstract

We present a new measurement of the positive muon magnetic anomaly, $a_\mu \equiv (g_\mu - 2)/2$, from the Fermilab Muon $g\!-\!2$ Experiment using data collected in 2019 and 2020. We have analyzed more than 4 times the number of positrons from muon decay than in our previous result from 2018 data. The systematic error is reduced by more than a factor of 2 due to better running conditions, a more stable beam, and improved knowledge of the magnetic field weighted by the muon distribution, $\tilde{\omega}'^{}_p$, and of the anomalous precession frequency corrected for beam dynamics effects, $\omega_a$. From the ratio $\omega_a / \tilde{\omega}'^{}_p$, together with precisely determined external parameters, we determine $a_\mu = 116\,592\,057(25) \times 10^{-11}$ (0.21 ppm). Combining this result with our previous result from the 2018 data, we obtain $a_\mu\text{(FNAL)} = 116\,592\,055(24) \times 10^{-11}$ (0.20 ppm). The new experimental world average is $a_\mu (\text{Exp}) = 116\,592\,059(22)\times 10^{-11}$ (0.19 ppm), which represents a factor of 2 improvement in precision., Comment: 8 pages, 3 figures

Published
2023
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3. The full coverage approach to the detection of Extensive Air Showers

Author

Di Sciascio, G. and Vergata, INFN - Roma Tor

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, High Energy Physics - Experiment, Physics - Instrumentation and Detectors
Abstract

A shower array exploiting the full coverage approach with a high segmentation of the readout allow to image the front of atmospheric showers with unprecedented resolution and detail. The grid distance determines the energy threshold (small energy showers are lost in the gap between detectors) and the quality of the shower sampling. Therefore, this experimental solution is needed to detect showers with a threshold in the 100 GeV range. The full coverage approach has been exploited in the ARGO-YBJ experiment. In this contribution we will summarise the advantages of this technique and discuss possible applications in new wide field of view detectors., Comment: Invited Talk to 21st International Symposium on Very High Energy Cosmic Ray Interactions (ISVHECRI 2022

Published
2022

4. Measurement of the Proton Maximum Acceleration Energy in Galactic Cosmic Rays

Author

Di Sciascio, G. and Vergata, INFN - Roma Tor

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract

Cosmic rays represent one of the most important energy transformation processes of the universe. They bring information about the surrounding universe, our galaxy, and very probably also the extragalactic space, at least at the highest observed energies. More than one century after their discovery, we have no definitive models yet about the origin, acceleration and propagation processes of the radiation. The main reason is that there are still significant discrepancies among the results obtained by different experiments, probably due to some still unknown systematic uncertainties affecting the measurements. In this paper, we will focus on the detection of galactic cosmic rays in the 10$^{15}$ eV energy range, where the so-called \emph{`knee'} in the all-particle energy spectrum is observed. The measurement of the (p+He) energy spectrum is presented and discussed., Comment: Invited Talk, Moriond conference on Very High Energy Phenomena in the Universe (March 19-26, 2022 La Thuile, Italy). arXiv admin note: substantial text overlap with arXiv:2202.11618

Published
2022

5. Measurement of Energy Spectrum and Elemental Composition of PeV Cosmic Rays: Open Problems and Prospects

Author

Di Sciascio, G.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract

Cosmic rays represent one of the most important energy transformation processes of the universe. They bring information about the surrounding universe, our galaxy, and very probably also the extragalactic space, at least at the highest observed energies. More than one century after their discovery, we have no definitive models yet about the origin, acceleration and propagation processes of the radiation. The main reason is that there are still significant discrepancies among the results obtained by different experiments located at ground level, probably due to unknown systematic uncertainties affecting the measurements. In this document, we will focus on the detection of galactic cosmic rays from ground with air shower arrays up to 10$^{18}$ eV. The aim of this paper is to discuss the conflicting results in the 10$^{15}$ eV energy range and the perspectives to clarify the origin of the so-called `knee' in the all-particle energy spectrum, crucial to give a solid basis for models up to the end of the cosmic ray spectrum. We will provide elements useful to understand the basic techniques used in reconstructing primary particle characteristics (energy, mass, and arrival direction) from the ground, and to show why indirect measurements are difficult and results are still conflicting., Comment: Invited Review, Special Issue "Research on Cosmic Rays and Their Impact on Human Activities", Applied Sciences (2022) 12(2):705. https://doi.org/10.3390/app12020705

Published
2022

6. Measurement of fundamental physical quantities in the framework of the Lab2Go project

Author

Casaburo, F., Marcelli, N., Sorbara, M., Agostinelli, M., Astone, P., Baldassarre, F., Brunori, F., Crisci, S., De Bonis, G., De Lucia, X., De Pedis, D., De Valeri, G., Di Sciascio, G., Faccini, R., Falato, J., Fraietta, V., Gatto, C., Guadagnini, S., Oliviero, V., Organtini, G., Passamonti, V., Piacentini, F., Ruggiero, N., Salerno, M., Sarti, S., and Tedesco, L.

Subjects
Physics - Physics Education
Abstract

To establish a closer contact between school and experimental sciences, Sapienza Universit\`a di Roma and the Istituto Nazionale di Fisica Nucleare (INFN) launched the Lab2Go project. Lab2Go has the goal of spreading laboratory practice among students and teachers in high schools. In this article, it is presented a measurement, carried out in the framework of the Lab2Go project, of the ratio hc/e where h, c and e are respectively the Planck constant, the speed of light in the vacuum, and the electric charge.

Published
2022

7. Composition Sensitivity (for the Cosmic Ray Anisotropy with SWGO)

Author

Taylor, A. M., Giacinti, G., Desiati, P., Velez, J. C. Diaz, Chiavassa, A., Di Sciascio, G., Velazquez, J. C. Arteaga, and Kunwar, S.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

A number of cosmic-ray observatories have measured a change in both phase and amplitude of the dipole component in the distribution of cosmic-ray arrival directions above a primary energy of 100 TeV. We focus on probing the cosmic-ray dipole and multipole evolution in the energy region of mutli TeV to beyond PeV with a future large-area gamma-ray observatory, such as the Southern Wide-field Gamma-ray Observatory (SWGO). The ability to discriminate between different mass groups is essential to understand the origin of this evolution. Through a consideration of the energy and mass resolution for cosmic-ray detection by such an observatory, we estimate its separation power for decomposing the full-particle anisotropy into mass groups. In particular, we explore the feasibility of probing the dipole evolution with rigidity with SWGO. In this way, we demonstrate the great potential that this instrument offers for providing a deeper understanding of the origin of the cosmic-ray anisotropy., Comment: Proceedings of the 37th International Cosmic Ray Conference (ICRC2021), 12-23 July 2021, Berlin, Germany - Online

Published
2021

8. Measurement of the anomalous precession frequency of the muon in the Fermilab Muon g-2 experiment

Author

Albahri, T., Anastasi, A., Anisenkov, A., Badgley, K., Baeßler, S., Bailey, I., Baranov, V. A., Barlas-Yucel, E., Barrett, T., Basti, A., Bedeschi, F., Berz, M., Bhattacharya, M., Binney, H. P., Bloom, P., Bono, J., Bottalico, E., Bowcock, T., Cantatore, G., Carey, R. M., Casey, B. C. K., Cauz, D., Chakraborty, R., Chang, S. P., Chapelain, A., Charity, S., Chislett, R., Choi, J., Chu, Z., Chupp, T. E., Corrodi, S., Cotrozzi, L., Crnkovic, J. D., Dabagov, S., Debevec, P. T., Di Falco, S., Di Meo, P., Di Sciascio, G., Di Stefano, R., Driutti, A., Duginov, V. N., Eads, M., Esquivel, J., Farooq, M., Fatemi, R., Ferrari, C., Fertl, M., Fienberg, A. T., Fioretti, A., Flay, D., Frlež, E., Froemming, N. S., Fry, J., Gabbanini, C., Galati, M. D., Ganguly, S., Garcia, A., George, J., Gibbons, L. K., Gioiosa, A., Giovanetti, K. L., Girotti, P., Gohn, W., Gorringe, T., Grange, J., Grant, S., Gray, F., Haciomeroglu, S., Halewood-Leagas, T., Hampai, D., Han, F., Hempstead, J., Herrod, A. T., Hertzog, D. W., Hesketh, G., Hibbert, A., Hodge, Z., Holzbauer, J. L., Hong, K. W., Hong, R., Iacovacci, M., Incagli, M., Kammel, P., Kargiantoulakis, M., Karuza, M., Kaspar, J., Kawall, D., Kelton, L., Keshavarzi, A., Kessler, D., Khaw, K. S., Khechadoorian, Z., Khomutov, N. V., Kiburg, B., Kiburg, M., Kim, O., Kim, Y. I., King, B., Kinnaird, N., Kraegeloh, E., Kuchibhotla, A., Kuchinskiy, N. A., Labe, K. R., LaBounty, J., Lancaster, M., Lee, M. J., Lee, S., Leo, S., Li, B., Li, D., Li, L., Logashenko, I., Campos, A. Lorente, Lucà, A., Lukicov, G., Lusiani, A., Lyon, A. L., MacCoy, B., Madrak, R., Makino, K., Marignetti, F., Mastroianni, S., Miller, J. P., Miozzi, S., Morse, W. M., Mott, J., Nath, A., Nguyen, H., Osofsky, R., Park, S., Pauletta, G., Piacentino, G. M., Pilato, R. N., Pitts, K. T., Plaster, B., Počanić, D., Pohlman, N., Polly, C. C., Price, J., Quinn, B., Raha, N., Ramachandran, S., Ramberg, E., Ritchie, J. L., Roberts, B. L., Rubin, D. L., Santi, L., Schlesier, C., Schreckenberger, A., Semertzidis, Y. K., Shemyakin, D., Smith, M. W., Sorbara, M., Stöckinger, D., Stapleton, J., Stoughton, C., Stratakis, D., Stuttard, T., Swanson, H. E., Sweetmore, G., Sweigart, D. A., Syphers, M. J., Tarazona, D. A., Teubner, T., Tewsley-Booth, A. E., Thomson, K., Tishchenko, V., Tran, N. H., Turner, W., Valetov, E., Vasilkova, D., Venanzoni, G., Walton, T., Weisskopf, A., Welty-Rieger, L., Winter, P., Wolski, A., and Wu, W.

Subjects
High Energy Physics - Experiment, Nuclear Experiment
Abstract

The Muon g-2 Experiment at Fermi National Accelerator Laboratory (FNAL) has measured the muon anomalous precession frequency $\omega_a$ to an uncertainty of 434 parts per billion (ppb), statistical, and 56 ppb, systematic, with data collected in four storage ring configurations during its first physics run in 2018. When combined with a precision measurement of the magnetic field of the experiment's muon storage ring, the precession frequency measurement determines a muon magnetic anomaly of $a_{\mu}({\rm FNAL}) = 116\,592\,040(54) \times 10^{-11}$ (0.46 ppm). This article describes the multiple techniques employed in the reconstruction, analysis and fitting of the data to measure the precession frequency. It also presents the averaging of the results from the eleven separate determinations of \omega_a, and the systematic uncertainties on the result., Comment: 29 pages, 19 figures. Published in Physical Review D

Published
2021
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9. Magnetic Field Measurement and Analysis for the Muon g-2 Experiment at Fermilab

Author

Albahri, T., Anastasi, A., Badgley, K., Baeßler, S., Bailey, I., Baranov, V. A., Barlas-Yucel, E., Barrett, T., Bedeschi, F., Berz, M., Bhattacharya, M., Binney, H. P., Bloom, P., Bono, J., Bottalico, E., Bowcock, T., Cantatore, G., Carey, R. M., Casey, B. C. K., Cauz, D., Chakraborty, R., Chang, S. P., Chapelain, A., Charity, S., Chislett, R., Choi, J., Chu, Z., Chupp, T. E., Conway, A., Corrodi, S., Cotrozzi, L., Crnkovic, J. D., Dabagov, S., Debevec, P. T., Di Falco, S., Di Meo, P., Di Sciascio, G., Di Stefano, R., Driutti, A., Duginov, V. N., Eads, M., Esquivel, J., Farooq, M., Fatemi, R., Ferrari, C., Fertl, M., Fienberg, A. T., Fioretti, A., Flay, D., Froemming, N. S., Gabbanini, C., Galati, M. D., Ganguly, S., Garcia, A., George, J., Gibbons, L. K., Gioiosa, A., Giovanetti, K. L., Girotti, P., Gohn, W., Gorringe, T., Grange, J., Grant, S., Gray, F., Haciomeroglu, S., Halewood-Leagas, T., Hampai, D., Han, F., Hempstead, J., Herrod, A. T., Hertzog, D. W., Hesketh, G., Hibbert, A., Hodge, Z., Holzbauer, J. L., Hong, K. W., Hong, R., Iacovacci, M., Incagli, M., Kammel, P., Kargiantoulakis, M., Karuza, M., Kaspar, J., Kawall, D., Kelton, L., Keshavarzi, A., Kessler, D., Khaw, K. S., Khechadoorian, Z., Khomutov, N. V., Kiburg, B., Kiburg, M., Kim, O., Kim, Y. I., King, B., Kinnaird, N., Kraegeloh, E., Kuchinskiy, N. A., Labe, K. R., LaBounty, J., Lancaster, M., Lee, M. J., Lee, S., Li, B., Li, D., Li, L., Logashenko, I., Campos, A. Lorente, Lucà, A., Lukicov, G., Lusiani, A., Lyon, A. L., MacCoy, B., Madrak, R., Makino, K., Marignetti, F., Mastroianni, S., Miller, J. P., Miozzi, S., Morse, W. M., Mott, J., Nath, A., Nguyen, H., Osofsky, R., Park, S., Pauletta, G., Piacentino, G. M., Pilato, R. N., Pitts, K. T., Plaster, B., Počanić, D., Pohlman, N., Polly, C. C., Price, J., Quinn, B., Raha, N., Ramachandran, S., Ramberg, E., Ritchie, J. L., Roberts, B. L., Rubin, D. L., Santi, L., Schlesier, C., Schreckenberger, A., Semertzidis, Y. K., Shemyakin, D., Smith, M. W., Sorbara, M., Stöckinger, D., Stapleton, J., Stoughton, C., Stratakis, D., Stuttard, T., Swanson, H. E., Sweetmore, G., Sweigart, D. A., Syphers, M. J., Tarazona, D. A., Teubner, T., Tewsley-Booth, A. E., Thomson, K., Tishchenko, V., Tran, N. H., Turner, W., Valetov, E., Vasilkova, D., Venanzoni, G., Walton, T., Weisskopf, A., Welty-Rieger, L., Winter, P., Wolski, A., and Wu, W.

Subjects
High Energy Physics - Experiment, Nuclear Experiment
Abstract

The Fermi National Accelerator Laboratory has measured the anomalous precession frequency $a^{}_\mu = (g^{}_\mu-2)/2$ of the muon to a combined precision of 0.46 parts per million with data collected during its first physics run in 2018. This paper documents the measurement of the magnetic field in the muon storage ring. The magnetic field is monitored by nuclear magnetic resonance systems and calibrated in terms of the equivalent proton spin precession frequency in a spherical water sample at 34.7$^\circ$C. The measured field is weighted by the muon distribution resulting in $\tilde{\omega}'^{}_p$, the denominator in the ratio $\omega^{}_a$/$\tilde{\omega}'^{}_p$ that together with known fundamental constants yields $a^{}_\mu$. The reported uncertainty on $\tilde{\omega}'^{}_p$ for the Run-1 data set is 114 ppb consisting of uncertainty contributions from frequency extraction, calibration, mapping, tracking, and averaging of 56 ppb, and contributions from fast transient fields of 99 ppb., Comment: Added one citation and corrected missing normalization in Eqs (35) and (36)

Published
2021
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10. Measurement of the Positive Muon Anomalous Magnetic Moment to 0.46 ppm

Author

Abi, B., Albahri, T., Al-Kilani, S., Allspach, D., Alonzi, L. P., Anastasi, A., Anisenkov, A., Azfar, F., Badgley, K., Baeßler, S., Bailey, I., Baranov, V. A., Barlas-Yucel, E., Barrett, T., Barzi, E., Basti, A., Bedeschi, F., Behnke, A., Berz, M., Bhattacharya, M., Binney, H. P., Bjorkquist, R., Bloom, P., Bono, J., Bottalico, E., Bowcock, T., Boyden, D., Cantatore, G., Carey, R. M., Carroll, J., Casey, B. C. K., Cauz, D., Ceravolo, S., Chakraborty, R., Chang, S. P., Chapelain, A., Chappa, S., Charity, S., Chislett, R., Choi, J., Chu, Z., Chupp, T. E., Convery, M. E., Conway, A., Corradi, G., Corrodi, S., Cotrozzi, L., Crnkovic, J. D., Dabagov, S., De Lurgio, P. M., Debevec, P. T., Di Falco, S., Di Meo, P., Di Sciascio, G., Di Stefano, R., Drendel, B., Driutti, A., Duginov, V. N., Eads, M., Eggert, N., Epps, A., Esquivel, J., Farooq, M., Fatemi, R., Ferrari, C., Fertl, M., Fiedler, A., Fienberg, A. T., Fioretti, A., Flay, D., Foster, S. B., Friedsam, H., Frlež, E., Froemming, N. S., Fry, J., Fu, C., Gabbanini, C., Galati, M. D., Ganguly, S., Garcia, A., Gastler, D. E., George, J., Gibbons, L. K., Gioiosa, A., Giovanetti, K. L., Girotti, P., Gohn, W., Gorringe, T., Grange, J., Grant, S., Gray, F., Haciomeroglu, S., Hahn, D., Halewood-Leagas, T., Hampai, D., Han, F., Hazen, E., Hempstead, J., Henry, S., Herrod, A. T., Hertzog, D. W., Hesketh, G., Hibbert, A., Hodge, Z., Holzbauer, J. L., Hong, K. W., Hong, R., Iacovacci, M., Incagli, M., Johnstone, C., Johnstone, J. A., Kammel, P., Kargiantoulakis, M., Karuza, M., Kaspar, J., Kawall, D., Kelton, L., Keshavarzi, A., Kessler, D., Khaw, K. S., Khechadoorian, Z., Khomutov, N. V., Kiburg, B., Kiburg, M., Kim, O., Kim, S. C., Kim, Y. I., King, B., Kinnaird, N., Korostelev, M., Kourbanis, I., Kraegeloh, E., Krylov, V. A., Kuchibhotla, A., Kuchinskiy, N. A., Labe, K. R., LaBounty, J., Lancaster, M., Lee, M. J., Lee, S., Leo, S., Li, B., Li, D., Li, L., Logashenko, I., Campos, A. Lorente, Lucà, A., Lukicov, G., Luo, G., Lusiani, A., Lyon, A. L., MacCoy, B., Madrak, R., Makino, K., Marignetti, F., Mastroianni, S., Maxfield, S., McEvoy, M., Merritt, W., Mikhailichenko, A. A., Miller, J. P., Miozzi, S., Morgan, J. P., Morse, W. M., Mott, J., Motuk, E., Nath, A., Newton, D., Nguyen, H., Oberling, M., Osofsky, R., Ostiguy, J. -F., Park, S., Pauletta, G., Piacentino, G. M., Pilato, R. N., Pitts, K. T., Plaster, B., Počanić, D., Pohlman, N., Polly, C. C., Popovic, M., Price, J., Quinn, B., Raha, N., Ramachandran, S., Ramberg, E., Rider, N. T., Ritchie, J. L., Roberts, B. L., Rubin, D. L., Santi, L., Sathyan, D., Schellman, H., Schlesier, C., Schreckenberger, A., Semertzidis, Y. K., Shatunov, Y. M., Shemyakin, D., Shenk, M., Sim, D., Smith, M. W., Smith, A., Soha, A. K., Sorbara, M., Stöckinger, D., Stapleton, J., Still, D., Stoughton, C., Stratakis, D., Strohman, C., Stuttard, T., Swanson, H. E., Sweetmore, G., Sweigart, D. A., Syphers, M. J., Tarazona, D. A., Teubner, T., Tewsley-Booth, A. E., Thomson, K., Tishchenko, V., Tran, N. H., Turner, W., Valetov, E., Vasilkova, D., Venanzoni, G., Volnykh, V. P., Walton, T., Warren, M., Weisskopf, A., Welty-Rieger, L., Whitley, M., Winter, P., Wolski, A., Wormald, M., Wu, W., and Yoshikawa, C.

Subjects
High Energy Physics - Experiment, Nuclear Experiment
Abstract

We present the first results of the Fermilab Muon g-2 Experiment for the positive muon magnetic anomaly $a_\mu \equiv (g_\mu-2)/2$. The anomaly is determined from the precision measurements of two angular frequencies. Intensity variation of high-energy positrons from muon decays directly encodes the difference frequency $\omega_a$ between the spin-precession and cyclotron frequencies for polarized muons in a magnetic storage ring. The storage ring magnetic field is measured using nuclear magnetic resonance probes calibrated in terms of the equivalent proton spin precession frequency ${\tilde{\omega}'^{}_p}$ in a spherical water sample at 34.7$^{\circ}$C. The ratio $\omega_a / {\tilde{\omega}'^{}_p}$, together with known fundamental constants, determines $a_\mu({\rm FNAL}) = 116\,592\,040(54)\times 10^{-11}$ (0.46\,ppm). The result is 3.3 standard deviations greater than the standard model prediction and is in excellent agreement with the previous Brookhaven National Laboratory (BNL) E821 measurement. After combination with previous measurements of both $\mu^+$ and $\mu^-$, the new experimental average of $a_\mu({\rm Exp}) = 116\,592\,061(41)\times 10^{-11}$ (0.35\,ppm) increases the tension between experiment and theory to 4.2 standard deviations, Comment: 10 pages; 4 figures

Published
2021
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11. Beam dynamics corrections to the Run-1 measurement of the muon anomalous magnetic moment at Fermilab

Author

Albahri, T., Anastasi, A., Badgley, K., Baeßler, S., Bailey, I., Baranov, V. A., Barlas-Yucel, E., Barrett, T., Bedeschi, F., Berz, M., Bhattacharya, M., Binney, H. P., Bloom, P., Bono, J., Bottalico, E., Bowcock, T., Cantatore, G., Carey, R. M., Casey, B. C. K., Cauz, D., Chakraborty, R., Chang, S. P., Chapelain, A., Charity, S., Chislett, R., Choi, J., Chu, Z., Chupp, T. E., Corrodi, S., Cotrozzi, L., Crnkovic, J. D., Dabagov, S., Debevec, P. T., Di Falco, S., Di Meo, P., Di Sciascio, G., Di Stefano, R., Driutti, A., Duginov, V. N., Eads, M., Esquivel, J., Farooq, M., Fatemi, R., Ferrari, C., Fertl, M., Fiedler, A., Fienberg, A. T., Fioretti, A., Flay, D., Frlež, E., Froemming, N. S., Fry, J., Gabbanini, C., Galati, M. D., Ganguly, S., Garcia, A., George, J., Gibbons, L. K., Gioiosa, A., Giovanetti, K. L., Girotti, P., Gohn, W., Gorringe, T., Grange, J., Grant, S., Gray, F., Haciomeroglu, S., Halewood-Leagas, T., Hampai, D., Han, F., Hempstead, J., Herrod, A. T., Hertzog, D. W., Hesketh, G., Hibbert, A., Hodge, Z., Holzbauer, J. L., Hong, K. W., Hong, R., Iacovacci, M., Incagli, M., Kammel, P., Kargiantoulakis, M., Karuza, M., Kaspar, J., Kawall, D., Kelton, L., Keshavarzi, A., Kessler, D., Khaw, K. S., Khechadoorian, Z., Khomutov, N. V., Kiburg, B., Kiburg, M., Kim, O., Kim, Y. I., King, B., Kinnaird, N., Korostelev, M., Kraegeloh, E., Kuchinskiy, N. A., Labe, K. R., LaBounty, J., Lancaster, M., Lee, M. J., Lee, S., Li, B., Li, D., Li, L., Logashenko, I., Campos, A. Lorente, Lucà, A., Lukicov, G., Lusiani, A., Lyon, A. L., MacCoy, B., Madrak, R., Makino, K., Marignetti, F., Mastroianni, S., Miller, J. P., Miozzi, S., Morse, W. M., Mott, J., Nath, A., Newton, D., Nguyen, H., Osofsky, R., Park, S., Pauletta, G., Piacentino, G. M., Pilato, R. N., Pitts, K. T., Plaster, B., Počanić, D., Pohlman, N., Polly, C. C., Price, J., Quinn, B., Raha, N., Ramachandran, S., Ramberg, E., Ritchie, J. L., Roberts, B. L., Rubin, D. L., Santi, L., Sathyan, D., Schlesier, C., Schreckenberger, A., Semertzidis, Y. K., Smith, M. W., Sorbara, M., Stöckinger, D., Stapleton, J., Stoughton, C., Stratakis, D., Stuttard, T., Swanson, H. E., Sweetmore, G., Sweigart, D. A., Syphers, M. J., Tarazona, D. A., Teubner, T., Tewsley-Booth, A. E., Thomson, K., Tishchenko, V., Tran, N. H., Turner, W., Valetov, E., Vasilkova, D., Venanzoni, G., Walton, T., Weisskopf, A., Welty-Rieger, L., Winter, P., Wolski, A., and Wu, W.

Subjects
Physics - Accelerator Physics, High Energy Physics - Experiment
Abstract

This paper presents the beam dynamics systematic corrections and their uncertainties for the Run-1 data set of the Fermilab Muon g-2 Experiment. Two corrections to the measured muon precession frequency $\omega_a^m$ are associated with well-known effects owing to the use of electrostatic quadrupole (ESQ) vertical focusing in the storage ring. An average vertically oriented motional magnetic field is felt by relativistic muons passing transversely through the radial electric field components created by the ESQ system. The correction depends on the stored momentum distribution and the tunes of the ring, which has relatively weak vertical focusing. Vertical betatron motions imply that the muons do not orbit the ring in a plane exactly orthogonal to the vertical magnetic field direction. A correction is necessary to account for an average pitch angle associated with their trajectories. A third small correction is necessary because muons that escape the ring during the storage time are slightly biased in initial spin phase compared to the parent distribution. Finally, because two high-voltage resistors in the ESQ network had longer than designed RC time constants, the vertical and horizontal centroids and envelopes of the stored muon beam drifted slightly, but coherently, during each storage ring fill. This led to the discovery of an important phase-acceptance relationship that requires a correction. The sum of the corrections to $\omega_a^m$ is 0.50 $\pm$ 0.09 ppm; the uncertainty is small compared to the 0.43 ppm statistical precision of $\omega_a^m$., Comment: 35 pages, 29 figures. Accepted by Phys. Rev. Accel. Beams

Published
2021
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12. Measurement of Cosmic Ray Spectrum and Anisotropy with ARGO-YBJ

Author

Di Sciascio G.

Subjects
Physics, QC1-999
Abstract

The combined measurement of the cosmic ray (CR) energy spectrum and anisotropy in their arrival direction distribution needs the knowledge of the elemental composition of the radiation to discriminate between different origin and propagation models. Important information on the CR mass composition can be obtained studying the EAS muon content through the measurement of the CR rate at different zenith angles. In this paper we report on the observation of the anisotropy of galactic CRs at different angular scales with the ARGO-YBJ experiment. We report also on the study of the primary CR rate for different zenith angles. The light component (p+He) has been selected and its energy spectrum measured in the energy range (5 – 200) TeV for quasi-vertical events. With this analysis for the first time a ground-based measurement of the CR spectrum overlaps data obtained with direct methods for more than one energy decade, thus providing a solid anchorage to the CR spectrum measurements carried out by EAS arrays in the knee region. Finally, a preliminary study of the non-attenuated shower component at a zenith angle θ > 70° (through the observation of the so-called horizantal air showers) is presented.

Published
2013
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13. Prevalence and predictive role of hypertriglyceridemia in statin-treated patients at very high risk: Insights from the START study

Author

Steering Committee, De Luca (Chairman), L., Gulizia (co-chairman), M.M., Temporelli, P.L., Riccio, C., Colivicchi, F., Amico, A.F., Formigli, D., Geraci, G., Di Lenarda, A., Executive Committee, De Luca, L., Maggioni, A.P., Lucci, D., Coordinating Center, Lorimer, A., Orsini, G., Gonzini, L., Fabbri, G., Priami, P., Maras, P., Ramani, F., Falcone, C., Passarelli, I., Mauri, S., Calabrò, P., Bianchi, R., Di Palma, G., Mascia, F., Vetrano, A., Fusco, A., Proia, E., Aiello, A., Tomai, F., Licitra, R., Petrolini, A., Bosco, B., Magliari, F., Callerame, M., Mazzella, T., Lettica, G.V., Coco, G., Incao, F., Marinacci, L., D'Addario, S., Tartaglione, S.N., Ubaldi, S., Sanchez, F.A., Costa, P., Manca, G., Failla, M., Scherillo, M., Procaccini, V., Senni, M., Luminita, E.M., Bonomo, P., Mossa, C., Corda, S., Colavita, A.R., Trevisonno, G., Vizzari, G., Cosentino, N., Formaro, C., Paolillo, C., Nalin, I.L., De Rosa, F.M., Fontana, F., Fuscaldo, G.F., Passamonti, E., Bertella, E., Calvaruso, E.V., Varani, E., Tani, F., Cicchitelli, G., Gabrielli, D., Paoloni, P., Marziali, A., Campo, G., Tebaldi, M., Biscaglia, S., Biase, M Di, Brunetti, N.D., Gallotta, A.M., Mattei, L., Marini, R., Balsemin, F., Urbano, M.D., Naio, R., Vicinelli, P., Arena, G., Mazzini, M., Gigli, N., Miserrafiti, B., Monopoli, A., Mortara, A., Delfino, P., Chioffi, M.M., Marino, P., Gravellone, M., Barbieri, L., Ledda, A., Carmina, M.G., Raisaro, A.E., Di Giacomo, C., Somaschini, A., Fasano, M.L., Sannazzaro, M., Arcieri, R., Pantaleoni, M., Leuzzi, C., Gorlato, G., Greco, G., Chiera, A., Ammaturo, T.A., Malanchini, G., Del Corral, M.P., Tedesco, L., Pede, S., Urso, L.G., Piscione, F., Galasso, G., Provasoli, S., Fattore, L., Lucca, G., Cresti, A., Cardillo, A., Fera, M.S., Vennettilli, F., Gaudio, C., Paravati, V., Caldarola, P., Locuratolo, N., Verlato, R., De Conti, F., Turiano, G., Preti, G., Moretti, L., Silenzi, S., Colonna, G., Picciolo, A., Nicosia, A., Cascone, C., Di Sciascio, G., Mangiacapra, F., Russo, A., Mastroianno, S., Esposito, G., Cosmi, F., D'Orazio, S., Costantini, C., Lanari, A., De Rosa, P., Esposito, L., Bilato, C., Valle, C Dalla, Ceresa, M., Colombo, E., Pennisi, V., Casciola, G., Driussi, M., Bisceglia, T., Scalvini, S., Rivadossi, F., Volpe, M., Comito, F., Scorzoni, D., Grimoldi, P., Lagioia, R., Santoro, D., De Cesare, N., Comotti, T., Poli, A., Martina, P., Musolino, M.F., Multari, E.I., Bilardo, G., Scalchi, G., Olivieri, C., Caranci, F., Pavan, D., Ganci, G., Mariani, A., Falchetti, E., Lanzillo, T., Caccavale, A., Bongo, A.S., Rizzi, A., Favilli, R., Maffei, S., Mallardo, M., Fulgione, C., Bordin, F., Bonmassari, R., Battaia, E., Puzzo, A., Vianello, G., D'Arpino, A., Romei, M., Pajes, G., Petronzelli, S., Ghezzi, F., Brigido, S., Pignatelli, L., Brscic, E., Sori, P., Russo, M., Biancolillo, E., Ignone, G., De Giorgio, N.A., Campaniello, C., Ponticelli, P., Margonato, A., Gerosa, S., Cutaia, A., Casalicchio, C., Bartolomucci, F., Larosa, C., Spadafina, T., Putignano, A., De Cristofaro, R., Bernardi, L., Sommariva, L., Celestini, A., Bertucci, C.M., Marchetti, M., Grisolia, E Franceschini, Ammendolea, C., Carini, M., Scipione, P., Politano, M., Rubino, G., Reina, C., Peccerillo, N., Paloscia, L., D'Alleva, A., Petacchi, R., Pignalosa, M., Lucchetti, D., Di Palma, F., La Mastra, R.A., Filippis, M De, Fontanella, B., Zanini, G., Casolo, G., Del Meglio, J., Parato, V.M., Genovesi, E., D'Alimonte, A., Miglioranza, A., Alessandri, N., Moscariello, F., Mauro, C., Sasso, A., Caso, P., Petrillo, C., Napoletano, C., Paparoni, S.R., Bernardo, V., Serdoz, R., Rotunno, R., Oppo, I., Aloisio, A., Aurelio, A., Licciardello, G., Cassaniti, L., Gulizia, M.M., Francese, G.M., Marcassa, C., Villani, R., Zorzoli, F., Mileto, F., Vecchis, M De, Scolozzi, D., Lupi, G., Caruso, D., Rebulla, E., La Fata, B., Anselmi, M., Girardi, P., Borruso, E., Ferrantelli, G., Sassone, B., Bressan, S., Capriolo, M., Pelissero, E., Piancastelli, M., Gobbi, M., Cocco, F., Bruno, M.G., Berti, S., Lo Surdo, G., Tanzi, P., De Rosa, R., Vilei, E., De Iaco, M.R., Grassi, G., Zanella, C., Marullo, L., Alfano, G., Pelaggi, P., Talarico, R., Tuccillo, B., Irace, L., Proietti, F., Di Croce, G., Di Lorenzo, L., Zarrilli, A., Bongini, M., Ranise, A., Aprile, A., Fornengo, C., Capogrosso, V., Tranghese, A., Golia, B., Marziano, A., Roncon, L., Picariello, C., Bagni, E., Leci, E., Gregorio, G., Gatto, F., Piemonte, F., Gervasio, F., Navazio, A., Guerri, E., Belmonte, E., Marino, F., Di Belardino, N., Di Nuzzo, M.R., Epifani, M., Comolatti, G., Conconi, B., Benea, D., Casu, G., Merella, P., Ammirati, M.A., Corrado, V.M., Spagnolo, D., Caico, S.I., Bonizzato, S., Margheri, M., Corrado, L., Antonicelli, R., Ferrigno, C., Merlino, A., Nassiacos, D., Antonelli, A., Marchese, A., Uguccioni, M., Villella, A., Bechi, S., Lo Bianco, F., Bedogni, F., Negro, L., Donato, L., Statile, D., Cassin, M., Fedele, F., Granatelli, A., Calcagno, S., Politi, A., Pani, A., De Luca, Leonardo, Temporelli, Pier Luigi, Gulizia, Michele Massimo, Gonzini, Lucio, Ammaturo, Tiziana Anita, Tedesco, Luigi, Pede, Silvia, Oliva, Fabrizio, Gabrielli, Domenico, Colivicchi, Furio, and Averna, Maurizio R.

Published
2023
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14. The sub-TeV transient Gamma-Ray sky: challenges and opportunities

Author

La Mura, G., Assis, P., Blanco, A., Conceição, R., Fonte, P., Lopes, L., Pimenta, M., Tomé, B., Santo, C. Espírito, Mendes, L., Ferreira, M., Abreu, P., Brogueira, P., Mendes, L. Filipe, Barão, F., de Almeida, U. Barres, Shellard, R. C., Giaccari, U., Lippmann, O., Piazzoli, B. D'Ettorre, Doro, M., Prandini, E., Perennes, C., Matthiae, G., Tavani, M., Santonico, R., De Angelis, A., Coto, R. Lopez, Chiavassa, A., Vícha, J., Trávničék, P., and Di Sciascio, G.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The detection of gravitational waves and neutrinos from astrophysical sources with gamma-ray counterparts officially started the era of Multi-Messenger Astronomy. Their transient and extreme nature implies that monitoring the VHE sky is fundamental to investigate the non-electromagnetic signals. However, the limited effective area of space-borne instruments prevents observations above a few hundred GeV, while the small field of view and low duty cycle of IACTs make them unsuited for extensive monitoring activities and prompt response to transients. Extensive Air Shower arrays (EAS) can provide a large field of view, a wide effective area and a very high duty cycle. Their main difficulty is the distinction between gamma-ray and cosmic-ray initiated air showers, especially below the TeV range. Here we present some case studies stressing the importance that a new EAS array in the Southern Hemisphere will be able to survey the sky from below 100 GeV up to several TeV. In the energy domain between 100 and 400 GeV we expect the strongest electromagnetic signatures of the acceleration of ultra-relativistic particles in sources like SNRs, blazar jets and gamma-ray bursts, as recently proved by IACT observations. This spectral window is also crucial to understand the Universe opacity to high energy radiation, thus providing constraints on the cosmological parameters. We will discuss the implications of VHE radiation on the mechanisms at work and we will focus on the advantages resulting from the ability to monitor the energy window lying between the domain of space-borne detectors and ground-based facilities., Comment: 8 pages, 2 color figures. Proceedings of Science, presented at the 36th International Cosmic Rays Conference (ICRC 2019)

Published
2019

15. The Southern Wide-Field Gamma-Ray Observatory (SWGO): A Next-Generation Ground-Based Survey Instrument for VHE Gamma-Ray Astronomy

Author

Abreu, P., Albert, A., Alfaro, R., Alvarez, C., Arceo, R., Assis, P., Barao, F., Bazo, J., Beacom, J. F., Bellido, J., BenZvi, S., Bretz, T., Brisbois, C., Brown, A. M., Brun, F., Buscemi, M., Mora, K. S. Caballero, Camarri, P., Carramiñana, A., Casanova, S., Chiavassa, A., Conceição, R., Cotter, G., Cristofari, P., Dasso, S., De Angelis, A., De Maria, M., Desiati, P., Di Sciascio, G., Vélez, J. C. Díaz, Dib, C., Dingus, B., Dorner, D., Doro, M., Duffy, C., DuVernois, M., Engel, R., Alonso, M. Fernandez, Fleischhack, H., Fonte, P., Fraija, N., Funk, S., García-González, J. A., González, M. M., Goodman, J. A., Greenshaw, T., Harding, J. P., Haungs, A., Hona, B., Huentemeyer, P., Insolia, A., Jardin-Blicq, A., Joshi, V., Kawata, K., Kunwar, S., La Mura, G., Lapington, J., Lenain, J. P., López-Coto, R., Malone, K., Martinez-Castro, J., Martínez-Huerta, H., Mendes, L., Moreno, E., Mostafá, M., Ng, K. C. Y., Nisa, M. U., Peron, F., Pichel, A., Pimenta, M., Prandini, E., Rainò, S., Reisenegger, A., Rodriguez, J., Roth, M., Rovero, A., Ruiz-Velasco, E., Sako, T., Sandoval, A., Santander, M., Satalecka, K., Schneider, M., Schoorlemmer, H., Schüssler, F., Shellard, R. C., Smith, A., Spencer, S., Springer, W., Surajbali, P., Tollefson, K., Tomé, B., Torres, I., Viana, A., Weisgarber, T., Wischnewski, R., Zepeda, A., Zhou, B., and Zhou, H.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We describe plans for the development of the Southern Wide-field Gamma-ray Observatory (SWGO), a next-generation instrument with sensitivity to the very-high-energy (VHE) band to be constructed in the Southern Hemisphere. SWGO will provide wide-field coverage of a large portion of the southern sky, effectively complementing current and future instruments in the global multi-messenger effort to understand extreme astrophysical phenomena throughout the universe. A detailed description of science topics addressed by SWGO is available in the science case white paper [1]. The development of SWGO will draw on extensive experience within the community in designing, constructing, and successfully operating wide-field instruments using observations of extensive air showers. The detector will consist of a compact inner array of particle detection units surrounded by a sparser outer array. A key advantage of the design of SWGO is that it can be constructed using current, already proven technology. We estimate a construction cost of 54M USD and a cost of 7.5M USD for 5 years of operation, with an anticipated US contribution of 20M USD ensuring that the US will be a driving force for the SWGO effort. The recently formed SWGO collaboration will conduct site selection and detector optimization studies prior to construction, with full operations foreseen to begin in 2026. Throughout this document, references to science white papers submitted to the Astro2020 Decadal Survey with particular relevance to the key science goals of SWGO, which include unveiling Galactic particle accelerators [2-10], exploring the dynamic universe [11-21], and probing physics beyond the Standard Model [22-25], are highlighted in red boldface., Comment: Astro2020 APC White Paper

Published
2019

16. STACEX: RPC-based detector for a multi-messenger observatory in the Southern Hemisphere

Author

Di Sciascio, G., Ciro, Bigongiari, Andrea, Bulgarelli, Paolo, Camarri, Martina, Cardillo, Sabrina, Casanova, Valentina, Fioretti, Fabrizio, Marchese, Giovanni, Piano, Rinaldo, Santonico, and Marco, Tavani

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment, Physics - Instrumentation and Detectors
Abstract

Extensice Air Shower (EAS) arrays are survey instruments able to monitor continuously all the overhead sky. Their wide field of view (about 2 sr) is ideal to complement directional detectors by performing unbiased sky surveys, by monitoring variable or flaring sources, such as AGNs, and to discover transients or explosive events (GRBs). With an energy threshold in the 100 GeV range EAS arrays are transient factories. All EAS arrays presently in operation or under installation are located in the Northern hemisphere. A new survey instrument located in the Southern Hemisphere should be a high priority to monitor the Inner Galaxy and the Galactic Center. STACEX is the proposal of a hybrid detector with ARGO-like RPCs coupled to Water Cherenkov Detectors (WCDs) mainly to lower the energy threshold at 100 GeV level. In this contribution we introduce the possibility of improving the low energy sensitivity of survey instruments by equipping RPCs, which were proved to be optimal detectors at 100 GeV energies by the ARGO-YBJ Collaboration, with WCDs. An EAS detector with high sensitivity between 100 GeV and 1 TeV would be a valuable complementary transient detector in the CTA era., Comment: Proc. of 36th International Cosmic Ray Conference -ICRC2019, July 24th - August 1st, 2019 Madison, WI, U.S.A

Published
2019

17. The laser-based gain monitoring system of the calorimeters in the Muon $g-2$ experiment at Fermilab

Author

Anastasi, A., Basti, A., Bedeschi, F., Boiano, A., Bottalico, E., Cantatore, G., Cauz, D., Chapelain, A. T., Corradi, G., Dabagov, S., Di Falco, S., Di Meo, P., Di Sciascio, G., Di Stefano, R., Donati, S., Driutti, A., Ferrari, C., Fienberg, A. T., Fioretti, A., Gabbanini, C., Gibbons, L. K., Gioiosa, A., Girotti, P., Hampai, D., Hempstead, J. B., Hertzog, D. W., Iacovacci, M., Incagli, M., Karuza, M., Kaspar, J., Khaw, K. S., Lusiani, A., Marignetti, F., Mastroianni, S., Miozzi, S., Nath, A., Pauletta, G., Piacentino, G. M., Raha, N., Santi, L., Smith, M., Sorbara, M., Sweigart, D. A., and Venanzoni, G.

Subjects
Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract

The Muon $g-2$ experiment, E989, is currently taking data at Fermilab with the aim of reducing the experimental error on the muon anomaly by a factor of four and possibly clarifying the current discrepancy with the theoretical prediction. A central component of this four-fold improvement in precision is the laser calibration system of the calorimeters, which has to monitor the gain variations of the photo-sensors with a 0.04\% precision on the short-term ($\sim 1\,$ms). This is about one order of magnitude better than what has ever been achieved for the calibration of a particle physics calorimeter. The system is designed to monitor also long-term gain variations, mostly due to temperature effects, with a precision below the per mille level. This article reviews the design, the implementation and the performance of the Muon $g-2$ laser calibration system, showing how the experimental requirements have been met., Comment: 33 pages,24 figures. Matches the published version

Published
2019
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18. The Science Case for a Southern Wide Field of View Detector

Author

Di Sciascio, G.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract

EAS arrays are survey instruments able to monitor continuously all the overhead sky. Their sensitivity in the sub-TeV/TeV energy domain cannot compete with that of Cherenkov telescopes, but the wide field of view (about 2 sr) is ideal to complement directional detectors by performing unbiased sky surveys, by monitoring variable or flaring sources such as Active Galactic Nuclei (AGN) and to discover transients or explosive events (GRBs). Arrays are well suited to study extended sources, such as the Galactic diffuse emission, and to measure the spectra of Galactic sources at the highest energies (near or beyond 100 TeV). An EAS array is able to detect at the same time events induced by photons and charged cosmic rays, thus studying the connection between these two messengers of the non-thermal Universe. Therefore, these detectors are, by definition, multi-messenger instruments. All EAS arrays presently in operation or under installation are located in the Northern hemisphere. The scientific potential of a next-generation survey instrument in the Southern Hemisphere will be presented and briefly discussed., Comment: Plenary Talk, Roma International Conference on Astroparticle Physics - RICAP 2018, Sept. 2018, Rome (Italy)

Published
2019

19. Science Case for a Wide Field-of-View Very-High-Energy Gamma-Ray Observatory in the Southern Hemisphere

Author

Albert, A., Alfaro, R., Ashkar, H., Alvarez, C., Álvarez, J., Arteaga-Velázquez, J. C., Solares, H. A. Ayala, Arceo, R., Bellido, J. A., BenZvi, S., Bretz, T., Brisbois, C. A., Brown, A. M., Brun, F., Caballero-Mora, K. S., Carosi, A., Carramiñana, A., Casanova, S., Chadwick, P. M., Cotter, G., De León, S. Coutiño, Cristofari, P., Dasso, S., de la Fuente, E., Dingus, B. L., Desiati, P., Salles, F. de O., de Souza, V., Dorner, D., Díaz-Vélez, J. C., García-González, J. A., DuVernois, M. A., Di Sciascio, G., Engel, K., Fleischhack, H., Fraija, N., Funk, S., Glicenstein, J-F., Gonzalez, J., González, M. M., Goodman, J. A., Harding, J. P., Haungs, A., Hinton, J., Hona, B., Hoyos, D., Huentemeyer, P., Iriarte, A., Jardin-Blicq, A., Joshi, V., Kaufmann, S., Kawata, K., Kunwar, S., Lefaucheur, J., Lenain, J. -P., Link, K., López-Coto, R., Marandon, V., Mariotti, M., Martínez-Castro, J., Martínez-Huerta, H., Mostafá, M., Nayerhoda, A., Nellen, L., Wilhelmi, E. de Oña, Parsons, R. D., Patricelli, B., Pichel, A., Piel, Q., Prandini, E., Pueschel, E., Procureur, S., Reisenegger, A., Rivière, C., Rodriguez, J., Rovero, A. C., Rowell, G., Ruiz-Velasco, E. L., Sandoval, A., Santander, M., Sako, T., Sako, T. K., Satalecka, K., Schoorlemmer, H., Schüssler, F., Seglar-Arroyo, M., Smith, A. J., Spencer, S., Surajbali, P., Tabachnick, E., Taylor, A. M., Tibolla, O., Torres, I., Vallage, B., Viana, A., Watson, J. J., Weisgarber, T., Werner, F., White, R., Wischnewski, R., Yang, R., Zepeda, A., and Zhou, H.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We outline the science motivation for SGSO, the Southern Gamma-Ray Survey Observatory. SGSO will be a next-generation wide field-of-view gamma-ray survey instrument, sensitive to gamma-rays in the energy range from 100 GeV to hundreds of TeV. Its science topics include unveiling galactic and extragalactic particle accelerators, monitoring the transient sky at very high energies, probing particle physics beyond the Standard Model, and the characterization of the cosmic ray flux. SGSO will consist of an air shower detector array, located in South America. Due to its location and large field of view, SGSO will be complementary to other current and planned gamma-ray observatories such as HAWC, LHAASO, and CTA.

Published
2019

20. 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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21. 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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22. 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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23. 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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24. 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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25. Electron beam test of key elements of the laser-based calibration system for the muon $g$ $-$ $2$ experiment

Author

Anastasi, A., Basti, A., Bedeschi, F., Bartolini, M., Cantatore, G., Cauz, D., Corradi, G., Dabagov, S., DI Sciascio, G., Di Stefano, R., Driutti, A., Escalante, O., Ferrari, C., Fienberg, A. T., Fioretti, A., Gabbanini, C., Gioiosa, A., Hampai, D., Hertzog, D. W., Iacovacci, M., Karuza, M., Kaspar, J., Liedl, A., Lusiani, A., Marignetti, F., Mastroianni, S., Moricciani, D., Pauletta, G., Piacentino, G. M., Raha, N., Rossi, E., Santi, L., and Venanzoni, G.

Subjects
Physics - Instrumentation and Detectors
Abstract

We report the test of many of the key elements of the laser-based calibration system for muon g - 2 experiment E989 at Fermilab. The test was performed at the Laboratori Nazionali di Frascati's Beam Test Facility using a 450 MeV electron beam impinging on a small subset of the final g - 2 lead-fluoride crystal calorimeter system. The calibration system was configured as planned for the E989 experiment and uses the same type of laser and most of the final optical elements. We show results regarding the calorimeter's response calibration, the maximum equivalent electron energy which can be provided by the laser and the stability of the calibration system components., Comment: Submitted to Nuclear Instrument and Methods A

Published
2016
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26. The LHAASO experiment: from Gamma-Ray Astronomy to Cosmic Rays

Author

Di Sciascio, G.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract

LHAASO is expected to be the most sensitive project to face the open problems in Galactic cosmic ray physics through a combined study of photon- and charged particle-induced extensive air showers in the energy range 10$^{11}$ - 10$^{17}$ eV. This new generation multi-component experiment will be able of continuously surveying the gamma-ray sky for steady and transient sources from about 100 GeV to PeV energies, thus opening for the first time the 10$^2$--10$^3$ TeV range to the direct observations of the high energy cosmic ray sources. In addition, the different observables (electronic, muonic and Cherenkov components) that will be measured in LHAASO will allow the study of the origin, acceleration and propagation of the radiation through a measurement of energy spectrum, elemental composition and anisotropy with unprecedented resolution. The installation of the experiment started at very high altitude in China (Daocheng site, Sichuan province, 4410 m a.s.l.). The commissioning of one fourth of the detector will be implemented in 2018. The completion of the installation is expected by the end of 2021., Comment: 8 pages, Invited talk at CRIS 2015 Conference, Gallipoli (Italy), Sept. 14-16, 2015

Published
2016

27. 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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28. 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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29. CTA Contributions to the 34th International Cosmic Ray Conference (ICRC2015)

Author

Consortium, The CTA, Abchiche, A., Abeysekara, U., Abril, Ó., Acero, F., Acharya, B. S., Actis, M., Agnetta, G., Aguilar, J. A., Aharonian, F., Akhperjanian, A., Albert, A., Alcubierre, M., Alfaro, R., Aliu, E., Allafort, A. J., Allan, D., Allekotte, I., Aloisio, R., Amans, J. -P., Amato, E., Ambrogi, L., Ambrosi, G., Ambrosio, M., Anderson, J., Anduze, M., Angüner, E. O., Antolini, E., Antonelli, L. A., Antonucci, M., Antonuccio, V., Antoranz, P., Aramo, C., Aravantinos, A., Argan, A., Armstrong, T., Arnaldi, H., Arnold, L., Arrabito, L., Arrieta, M., Asano, K., Asorey, H. G., Aune, T., Singh, C. B., Babic, A., Backes, M., Bais, A., Bajtlik, S., Balazs, C., Balbo, M., Balis, D., Balkowski, C., Ballester, O., Ballet, J., Balzer, A., Bamba, A., Bandiera, R., Barber, A., Barbier, C., Barceló, M., Barnacka, A., de Almeida, U. Barres, Barrio, J. A., Basso, S., Bastieri, D., Bauer, C., Baushev, A., Becciani, U., Becherini, Y., Tjus, J. Becker, Beckmann, V., Bednarek, W., Benbow, W., Ventura, D. Benedico, Berdugo, J., Berge, D., Bernardini, E., Bernhard, S., Bernlöhr, K., Bertucci, B., Besel, M. -A., Bhatt, N., Bhattacharjee, P., Bhattachryya, S., Biasuzzi, B., Bicknell, G., Bigongiari, C., Biland, A., Billotta, S., Bilnik, W., Biondo, B., Bird, T., Birsin, E., Bissaldi, E., Biteau, J., Bitossi, M., Bigas, O. Blanch, Blasi, P., Boehm, C., Bogacz, L., Bogdan, M., Bohacova, M., Boisson, C., Gargallo, J. Boix, Bolmont, J., Bonanno, G., Bonardi, A., Bonifacio, P., Bonnoli, G., Borkowski, J., Bose, R., Bosnjak, Z., Bottani, A., Böttcher, M., Bousquet, J. -J., Boutonnet, C., Bouyjou, F., Braiding, C., Brandt, L., Brau-Nogué, S., Bregeon, J., Bretz, T., Briggs, M., Brigida, M., Bringmann, T., Brisken, W., Brocato, E., Brook, P., Brown, A. M., Brun, P., Brunetti, G., Brunetti, L., Bruno, P., Bryan, M., Buanes, T., Bucciantini, N., Buchholtz, G., Buckley, J., Bugaev, V., Bühler, R., Bulgarelli, A., Bulik, T., Burton, M., Burtovoi, A., Busetto, G., Buson, S., Buss, J., Byrum, K., Cameron, R., Camprecios, J., Canelli, F., Canestrari, R., Cantu, S., Capalbi, M., Capasso, M., Capobianco, G., Caraveo, P., Cardenzana, J., Carius, S., Carlile, C., Carmona, E., Carosi, A., Carosi, R., Carr, J., Carroll, M., Carter, J., Carton, P. -H., Caruso, R., Casandjian, J. -M., Casanova, S., Cascone, E., Casiraghi, M., Castellina, A., Catalano, O., Catalanotti, S., Cavazzani, S., Cazaux, S., Cefalà, M., Cerchiara, P., Cereda, M., Cerruti, M., Chabanne, E., Chadwick, P., Champion, C., Chaty, S., Chaves, R., Cheimets, P., Chen, A., Chen, X., Chernyakova, M., Chiappetti, L., Chikawa, M., Chinn, D., Chitnis, V. R., Cho, N., Christov, A., Chudoba, J., Cieślar, M., Cillis, A., Ciocci, M. A., Clay, R., Cohen-Tanugi, J., Colafrancesco, S., Colin, P., Colombo, E., Colome, J., Colonges, S., Compin, M., Conforti, V., Connaughton, V., Connell, S., Conrad, J., Contreras, J. L., Coppi, P., Corbel, S., Coridian, J., Corona, P., Corti, D., Cortina, J., Cossio, L., Costa, A., Costantini, H., Cotter, G., Courty, B., Covino, S., Covone, G., Crimi, G., Criswell, S. J., Crocker, R., Croston, J., Cusumano, G., Da Vela, P., Dale, Ø., D'Ammando, F., Dang, D., Daniel, M., Davids, I., Dawson, B., Dazzi, F., Costa, B. de Aguiar, De Angelis, A., Cardoso, R. F. de Araujo, De Caprio, V., De Cesare, G., De Franco, A., De Frondat, F., Pino, E. M. de Gouveia Dal, de la Calle, I., De La Vega, G. A., Lopez, R. de los Reyes, De Lotto, B., De Luca, A., Neto, J. R. T. de Mello, de Naurois, M., Wilhelmi, E. de Oña, De Palma, F., de Souza, V., Decock, G., Deil, C., Del Santo, M., Delagnes, E., Deleglise, G., Delgado, C., della Volpe, D., Deloye, P., Depaola, G., Detournay, M., Dettlaff, A., Di Girolamo, T., Di Giulio, C., Di Paola, A., Di Pierro, F., Di Sciascio, G., Díaz, C., Dick, J., Dickinson, H., Diebold, S., Diez, V., Digel, S., Dipold, J., Disset, G., Distefano, A., Djannati-Ataï, A., Doert, M., Dohmke, M., Domainko, W., Dominik, N., Prester, D. Dominis, Donat, A., Donnarumma, I., Dorner, D., Doro, M., Dournaux, J. -L., Doyle, K., Drake, G., Dravins, D., Drury, L., Dubus, G., Dumas, D., Dumm, J., Durand, D., D'Urso, D., Dwarkadas, V., Dyks, J., Dyrda, M., Ebr, J., Echaniz, J. C., Edy, E., Egberts, K., Eger, P., Einecke, S., Eisch, J., Eisenkolb, F., Eleftheriadis, C., Elsässer, D., Emmanoulopoulos, D., Engelbrecht, C., Engelhaupt, D., Ernenwein, J. -P., Errando, M., Eschbach, S., Etchegoyen, A., Evans, P., Fairbairn, M., Falcone, A., Fantinel, D., Farakos, K., Farnier, C., Farrell, E., Farrell, S., Fasola, G., Fegan, S., Feinstein, F., Ferenc, D., Fernandez, A., Fernandez-Alonso, M., Ferreira, O., Fesquet, M., Fetfatzis, P., Fiasson, A., Filipčič, A., Filipovic, M., Fink, D., Finley, C., Finley, J. P., Finoguenov, A., Fioretti, V., Fiorini, M., Curcoll, R. Firpo, Fleischhack, H., Flores, H., Florin, D., Föhr, C., Fokitis, E., Font, L., Fontaine, G., Fontes, B., Forest, F., Fornasa, M., Förster, A., Fortin, P., Fortson, L., Fouque, N., Franckowiak, A., Franco, F. J., Frankowski, A., Frega, N., Albuquerque, I. Freire Mota, Coromina, L. Freixas, Fresnillo, L., Fruck, C., Fuessling, M., Fugazza, D., Fujita, Y., Fukami, S., Fukazawa, Y., Fukuda, T., Fukui, Y., Funk, S., Gäbele, W., Gabici, S., Gadola, A., Galante, N., Gall, D. D., Gallant, Y., Galloway, D., Gallozzi, S., Gao, S., Garcia, B., Gil, R. García, López, R. Garcia, Garczarczyk, M., Gardiol, D., Gargano, C., Gargano, F., Garozzo, S., Garrecht, F., Garrido, D., Garrido, L., Gascon, D., Gaskins, J., Gaudemard, J., Gaug, M., Gaweda, J., Geffroy, N., Gérard, L., Ghalumyan, A., Ghedina, A., Ghigo, M., Ghislain, P., Giannakaki, E., Gianotti, F., Giarrusso, S., Giavitto, G., Giebels, B., Giglietto, N., Gika, V., Gimenes, R., Giomi, M., Giommi, P., Giordano, F., Giovannini, G., Giro, E., Giroletti, M., Giuliani, A., Glicenstein, J. -F., Godinovic, N., Goldoni, P., Berisso, M. Gomez, Vargas, G. A. Gomez, Gonzalez, M. M., González, A., González, F., Muñoz, A. González, Gothe, K. S., Gotz, D., Grabarczyk, T., Graciani, R., Grandi, P., Grañena, F., Granot, J., Grasseau, G., Gredig, R., Green, A. J., Green, A. M., Greenshaw, T., Grenier, I., Grillo, A., Grondin, M. -H., Grube, J., Grudzinska, M., Grygorczuk, J., Guarino, V., Guberman, D., Gunji, S., Gyuk, G., Hadasch, D., Hagedorn, A., Hahn, J., Hakansson, N., Heras, N. Hamer, Hanabata, Y., Hara, S., Hardcastle, M. J., Harris, J., Hassan, T., Hatanaka, K., Haubold, T., Haupt, A., Hayakawa, T., Hayashida, M., Heller, M., Heller, R., Henault, F., Henri, G., Hermann, G., Hermel, R., Llorente, J. Herrera, Herrero, A., Hervet, O., Hidaka, N., Hinton, J., Hirai, W., Hirotani, K., Hoard, D., Hoffmann, D., Hofmann, W., Hofverberg, P., Holch, T., Holder, J., Hooper, S., Horan, D., Hörandel, J. R., Hormigos, S., Horns, D., Hose, J., Houles, J., Hovatta, T., Hrabovsky, M., Hrupec, D., Huet, J. -M., Hütten, M., Humensky, T. B., Huovelin, J., Huppert, J. -F., Iacovacci, M., Ibarra, A., Idźkowski, B., Ikawa, D., Illa, J. M., Impiombato, D., Incorvaia, S., Inome, Y., Inoue, S., Inoue, T., Inoue, Y., Iocco, F., Ioka, K., Iori, M., Ishio, K., Israel, G. L., Jablonski, C., Jacholkowska, A., Jacquemier, J., Jamrozy, M., Janecek, P., Janiak, M., Jankowsky, F., Jean, P., Jeanney, C., Jegouzo, I., Jenke, P., Jimenez, J. J., Jingo, M., Jocou, L., Jogler, T., Johnson, C. A., Journet, L., Juffroy, C., Jung, I., Kaaret, P. E., Kagaya, M., Kakuwa, J., Kalekin, O., Kalkuhl, C., Kankanyan, R., Karastergiou, A., Kärcher, K., Karczewski, M., Karkar, S., Karn, P., Kasperek, J., Katagiri, H., Kataoka, J., Katarzyński, K., Katz, U., Kaufmann, S., Kawanaka, N., Kawashima, T., Kazanas, D., Kelley-Hoskins, N., Kellner-Leidel, B., Kendziorra, E., Kersten, J., Khélifi, B., Kieda, D. B., Kihm, T., Kisaka, S., Kissmann, R., Klepser, S., Kluźniak, W., Knapen, J., Knapp, J., Knödlseder, J., Köck, F., Kocot, J., Kodakkadan, A., Kodani, K., Kohri, K., Kojima, T., Kokkotas, K., Kolitzus, D., Komin, N., Kominis, I., Konno, Y., Kosack, K., Koss, G., Koul, R., Kowal, G., Koyama, S., Kozioł, J., Kraus, M., Krause, J., Krause, M., Krawzcynski, H., Krennrich, F., Kretzschmann, A., Kruger, P., Kubo, H., Kudryavtsev, V., Mezek, G. Kukec, Kushida, J., Kuznetsov, A., La Barbera, A., La Palombara, N., La Parola, V., La Rosa, G., Laffon, H., Lagadec, T., Lahmann, R., Lalik, K., Lamanna, G., Landriu, D., Landt, H., Lang, R. G., Languignon, D., Lapington, J., Laporte, P., Latovski, N., Law-Green, D., Fèvre, J. -P. Le, Flour, T. Le, Sidaner, P. Le, Lee, S. -H., Lee, W. H., Leffhalm, K., Leich, H., de Oliveira, M. A. Leigui, Lelas, D., Lemière, A., Lemoine-Goumard, M., Lenain, J. -P., Leonard, R., Leoni, R., Lessio, L., Leto, G., Leveque, A., Lieunard, B., Limon, M., Lindemann, R., Lindfors, E., Liolios, A., Lipniacka, A., Lockart, H., Lohse, T., Loiseau, D., Łokas, E., Lombardi, S., Longo, F., Longo, G., Lopatin, A., Lopez, M., López-Coto, R., López-Oramas, A., Loreggia, D., Louge, T., Louis, F., Lu, C. -C., Lucarelli, F., Lucchesi, D., Lüdecke, H., Luque-Escamilla, P. L., Luz, O., Lyard, E., Maccarone, M. C., Maccarone, T. J., Mach, E., Madejski, G. M., Madonna, A., Mahabir, M., Maier, G., Majumdar, P., Makariev, M., Malaguti, G., Malaspina, G., Mallot, A. K., Maltezos, S., Mancilla, A., Mandat, D., Maneva, G., Manigot, P., Mankushiyil, N., Mannheim, K., Maragos, N., Marano, D., Marchegiani, P., Marcomini, J. A., Marcowith, A., Mariotti, M., Marisaldi, M., Markoff, S., Marszałek, A., Martens, C., Martí, J., Martin, J. -M., Martin, P., Martínez, G., Martínez, M., Martínez, O., Marx, R., Massimino, P., Mastichiadis, A., Mastroianni, S., Mastropietro, M., Masuda, S., Matsumoto, H., Matsuoka, S., Mattiazzo, S., Maurin, G., Maxted, N., Maya, J., Mayer, M., Mazin, D., Mazureau, E., Mazziotta, M. N., Comb, L. Mc, McCann, A., McCubbin, N., McHardy, I., McKay, R., McKinney, K., Meagher, K., Medina, C., Mehrez, F., Melioli, C., Melkumyan, D., Melo, D., Melse, T., Mereghetti, S., Mertsch, P., Meyer, M., Meyrelles jr, J. L., Miccichè, A., Michałowski, J., Micolon, P., Mientjes, P., Mignot, S., Mihailidis, A., Mineo, T., Minuti, M., Mirabal, N., Mirabel, F., Miranda, J. M., Mirzoyan, R., Mistò, A., Mitchell, A., Mizuno, T., Moderski, R., Mognet, I., Mohammed, M., Moharana, R., Molinari, E., Monmarthe, E., Monnier, G., Montaruli, T., Monte, C., Monteiro, I., Moore, P., Olaizola, A. Moralejo, Morello, C., Moretti, E., Mori, K., Morlino, G., Morselli, A., Mottez, F., Moudden, Y., Moulin, E., Mrusek, I., Mueller, S., Mukherjee, R., Munar-Adrover, P., Mundell, C., Muraishi, H., Murase, K., Muronga, A., Murphy, A., Nagataki, S., Nagayoshi, T., Nagesh, B. K., Naito, T., Nakajima, D., Nakamori, T., Nakayama, K., Naumann, D., Nayman, P., Nellen, L., Nemmen, R., Neronov, A., Neustroev, V., Neyroud, N., Nguyen, T., Nicastro, L., Nicolau-Kukliński, J., Niederwanger, F., Niedźwiecki, A., Niemiec, J., Nieto, D., Nievas, M., Nikolaidis, A., Nishijima, K., Nishikawa, K. -I., Noda, K., Nogues, L., Nolan, S., Northrop, R., Nosek, D., Nozka, L., Nunio, F., Oakes, L., O'Brien, P., Occhipinti, G., de Bhroithe, A. O'Faolain, Ogino, M., Ohira, Y., Ohishi, M., Ohm, S., Ohoka, H., Okumura, A., Olive, J. -F., Olszowski, D., Ong, R. A., Ono, S., Orienti, M., Orito, R., Orlati, A., Osborne, J., Ostrowski, M., Otero, L. A., Ottaway, D., Otte, N., Oya, I., Ozieblo, A., Padovani, M., Pagano, I., Paiano, S., Paizis, A., Palacio, J., Palatka, M., Pallotta, J., Panagiotidis, K., Panazol, J. -L., Paneque, D., Panter, M., Panzera, M. R., Paoletti, R., Paolillo, M., Papayannis, A., Papyan, G., Paravac, A., Paredes, J. M., Pareschi, G., Park, N., Parsons, D., Paśko, P., Pavy, S., Arribas, M. Paz, Pech, M., Peck, A., Pedaletti, G., Peet, S., Pelassa, V., Pelat, D., Peres, C., Perez, M. d. C., Perri, L., Persic, M., Petrashyk, A., Petrucci, P. -O., Peyaud, B., Pfeifer, M., Pfeiffer, G., Piano, G., Pichel, A., Pieloth, D., Pierbattista, M., Pierre, E., de Pinho, F. Pinto, García, C. Pio, Piret, Y., Pita, S., Planes, A., Platino, M., Platos, Ł., Platzer, R., Podkladkin, S., Pogosyan, L., Pohl, M., Poinsignon, P., Ponz, J. D., Porcelli, A., Potter, W., Poulios, S., Poutanen, J., Prandini, E., Prast, J., Preece, R., Profeti, F., Prokhorov, D., Prokoph, H., Prouza, M., Proyetti, M., Pruchniewicz, R., Pueschel, E., Pühlhofer, G., Puljak, I., Punch, M., Pyzioł, R., Queiroz, F., Quel, E. J., Quinn, J., Quirrenbach, A., Racero, E., Räck, T., Rafalski, J., Rafighi, I., Rainò, S., Rajda, P. J., Rameez, M., Rando, R., Rannot, R. C., Rataj, M., Rateau, S., Ravel, T., Ravignani, D., Razzaque, S., Reardon, P., Reimann, O., Reimer, A., Reimer, O., Reitberger, K., Renaud, M., Renner, S., Reposeur, T., Rettig, R., Reville, B., Rhode, W., Ribeiro, D., Ribó, M., Richards, G., Richer, M. G., Rico, J., Ridky, J., Rieger, F., Ringegni, P., Ristori, P. R., Rivière, A., Rivoire, S., Roache, E., Rodeghiero, G., Rodriguez, J., Fernandez, G. Rodriguez, Vázquez, J. J. Rodríguez, Rogers, T., Rojas, G., Romano, P., Rodriguez, M. P. Romay, Romeo, G., Romero, G. E., Roncadelli, M., Rose, J., Rosen, S., Lees, S. Rosier, Ross, D., Rossiter, P., Rouaix, G., Rousselle, J., Rovero, A. C., Rowell, G., Roy, F., Royer, S., Różańska, A., Rudak, B., Rugliancich, A., Rulten, C., Rupiński, M., Russo, F., Rutkowski, K., Saavedra, O., Sabatini, S., Sacco, B., Saemann, E. O., Saggion, A., Saha, L., Sahakian, V., Saito, K., Saito, T., Sakaki, N., Salega, M., Salek, D., Salgado, J., Salini, A., Sanchez, D., Sanchez, F., Sanchez-Conde, M., Sandaker, H., Sandoval, A., Sangiorgi, P., Sanguillon, M., Sano, H., Santander, M., Santangelo, A., Santos, E. M., Santos-Lima, R., Sanuy, A., Sapozhnikov, L., Sarkar, S., Satalecka, K., Savalle, R., Sawada, M., Sayède, F., Schafer, J., Schanne, S., Schanz, T., Schioppa, E. J., Schlenstedt, S., Schlickeiser, R., Schmidt, T., Schmoll, J., Schneider, M., Schovanek, P., Schubert, A., Schultz, C., Schultze, J., Schulz, A., Schulz, S., Schure, K., Schussler, F., Schwab, T., Schwanke, U., Schwarz, J., Schweizer, T., Schwemmer, S., Schwendicke, U., Schwerdt, C., Segreto, A., Seiradakis, J. -H., Sembroski, G. H., Semikoz, D., Serre, N., Servillat, M., Seweryn, K., Shafi, N., Sharma, M., Shayduk, M., Shellard, R. C., Shibata, T., Pandeni, K. Shiningayamwe, Shukla, A., Shum, E., Sidoli, L., Sidz, M., Sieiro, J., Siejkowski, H., Silk, J., Sillanpää, A., Simone, D., Singh, B. B., Sinha, A., Sironi, G., Sitarek, J., Sizun, P., Slyusar, V., Smith, A., Smith, J., Sobczyńska, D., Sol, H., Sottile, G., Sowiński, M., Spanier, F., Spengler, G., Spiga, D., Stadler, R., Stahl, O., Stamatescu, V., Stamerra, A., Stanič, S., Starling, R., Stawarz, Ł., Steenkamp, R., Stefanik, S., Stegmann, C., Steiner, S., Stella, C., Stergioulas, N., Sternberger, R., Sterzel, M., Stevenson, B., Stinzing, F., Stodulska, M., Stodulski, M., Stolarczyk, T., Straumann, U., Strazzeri, E., Stringhetti, L., Strzys, M., Stuik, R., Sulanke, K. -H., Supanitsky, A. D., Suric, T., Sushch, I., Sutcliffe, P., Sykes, J., Szanecki, M., Szepieniec, T., Szwarnog, P., Tacchini, A., Tachihara, K., Tagliaferri, G., Tajima, H., Takahashi, H., Takahashi, K., Takahashi, M., Takalo, L., Takami, H., Talbot, G., Tammi, J., Tanaka, M., Tanaka, S., Tanaka, T., Tanaka, Y., Tanci, C., Tarantino, E., Tavani, M., Tavecchio, F., Tavernet, J. -P., Tayabaly, K., Tejedor, L. A., Telezhinsky, I., Temme, F., Temnikov, P., Tenzer, C., Terada, Y., Terrier, R., Tescaro, D., Teshima, M., Testa, V., Tezier, D., Thayer, J., Thomas, V., Thornhill, J., Thuermann, D., Tibaldo, L., Tibolla, O., Tiengo, A., Tijsseling, G., Timpanaro, M. C., Tluczykont, M., Peixoto, C. J. Todero, Tokanai, F., Tokarz, M., Toma, K., Tomastik, J., Tomono, Y., Tonachini, A., Tonev, D., Torii, K., Tornikoski, M., Torres, D. F., Torres, M., Torresi, E., Toscano, S., Toso, G., Tosti, G., Totani, T., Tothill, N., Toussenel, F., Tovmassian, G., Townsley, C., Toyama, T., Travnicek, P., Trifoglio, M., Pujadas, I. Troyano, Trzeciak, M., Tsinganos, K., Tsubone, Y., Tsuchiya, Y., Tsujimoto, S., Tsuru, T., Uchiyama, Y., Umana, G., Umetsu, Y., Underwood, C., Upadhya, S. S., Uslenghi, M., Vagnetti, F., Valdes-Galicia, J., Vallania, P., Vallejo, G., Valore, L., van Driel, W., van Eldik, C., van Soelen, B., Vandenbroucke, J., Vanderwalt, J., Vasileiadis, G., Vassiliev, V., Acosta, M. L. Vázquez, Vecchi, M., Vegas, I., Veitch, P., Venema, L., Venter, C., Vercellone, S., Vergani, S., Verma, K., Verzi, V., Vettolani, G. P., Viana, A., Vicha, J., Videla, M., Vigorito, C., Vincent, P., Vincent, S., Vink, J., Vittorini, V., Vlahakis, N., Vlahos, L., Voelk, H., Vogler, P., Voisin, V., Vollhardt, A., Volpicelli, A., Vorobiov, S., Vovk, I., Vu, L. V., Wagner, R., Wagner, R. M., Wagner, R. G., Wagner, S. J., Wakely, S. P., Walter, R., Walther, T., Ward, J. E., Ward, M., Warda, K., Warwick, R., Wassberg, S., Watson, J., Wawer, P., Wawrzaszek, R., Webb, N., Wegner, P., Weinstein, A., Weitzel, Q., Wells, R., Werner, F., Werner, M., Wetteskind, H., White, M., White, R., Więcek, M., Wierzcholska, A., Wiesand, S., Wijers, R., Wild, N., Wilhelm, A., Wilkinson, M., Will, M., Williams, D. A., Williams, J. T., Willingale, R., Winde, M., Winiarski, K., Winkler, H., Wischnewski, R., Wojcik, P., Wolf, D., Wood, M., Wörnlein, A., Wu, E., Wu, T., Yadav, K. K., Yamamoto, H., Yamamoto, T., Yamazaki, R., Yanagita, S., Yang, L., Yebras, J. M., Yelos, D., Yeung, W., Yoshida, A., Yoshida, T., Yoshiike, S., Yoshikoshi, T., Yu, P., Zabalza, V., Zacharias, M., Zaharijas, G., Zajczyk, A., Zampieri, L., Zandanel, F., Zanin, R., Sanchez, R. Zanmar, Zavrtanik, D., Zavrtanik, M., Zdziarski, A., Zech, A., Zechlin, H., Zhao, A., Ziegler, A., Ziemann, J., Ziętara, K., Ziółkowski, J., Zitelli, V., Zoli, A., Zurbach, C., and Żychowski, P.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

List of contributions from the CTA Consortium presented at the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The Netherlands., Comment: Index of CTA conference proceedings at the ICRC2015, The Hague (The Netherlands). v1: placeholder with no arXiv links yet, to be replaced once individual contributions have been all submitted; v2: final with arXiv links to all CTA contributions and full author list

Published
2015

30. 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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31. 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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32. Test of candidate light distributors for the muon (g$-$2) laser calibration system

Author

Anastasi, A., Babusci, D., Baffigi, F., Cantatore, G., Cauz, D., Corradi, G., Dabagov, S., Di Sciascio, G., Di Stefano, R., Ferrari, C., Fienberg, A. T., Fioretti, A., Fulgentini, L., Gabbanini, C., Gizzi, L. A., Hampai, D., Hertzog, D. W., Iacovacci, M., Karuza, M., Kaspar, J., Koester, P., Labate, L., Mastroianni, S., Moricciani, D., Pauletta, G., Santi, L., and Venanzoni, G.

Subjects
Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract

The new muon (g-2) experiment E989 at Fermilab will be equipped with a laser calibration system for all the 1296 channels of the calorimeters. An integrating sphere and an alternative system based on an engineered diffuser have been considered as possible light distributors for the experiment. We present here a detailed comparison of the two based on temporal response, spatial uniformity, transmittance and time stability., Comment: accepted to Nucl.Instrum.Meth. A

Published
2015
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33. 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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34. 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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35. 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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36. Muon (g-2) Technical Design Report

Author

Grange, J., Guarino, V., Winter, P., Wood, K., Zhao, H., Carey, R. M., Gastler, D., Hazen, E., Kinnaird, N., Miller, J. P., Mott, J., Roberts, B. L., Benante, J., Crnkovic, J., Morse, W. M., Sayed, H., Tishchenko, V., Druzhinin, V. P., Khazin, B. I., Koop, I. A., Logashenko, I., Shatunov, Y. M., Solodov, E., Korostelev, M., Newton, D., Wolski, A., Chapelain, A., Bjorkquist, R., Eggert, N., Frankenthal, A., Gibbons, L., Kim, S., Mikhailichenko, A., Orlov, Y., Rubin, D., Sweigart, D., Allspach, D., Annala, G., Barzi, E., Bourland, K., Brown, G., Casey, B. C. K., Chappa, S., Convery, M. E., Drendel, B., Friedsam, H., Gadfort, T., Hardin, K., Hawke, S., Hayes, S., Jaskierny, W., Johnstone, C., Johnstone, J., Kashikhin, V., Kendziora, C., Kiburg, B., Klebaner, A., Kourbanis, I., Kyle, J., Larson, N., Leveling, A., Lyon, A. L., Markley, D., McArthur, D., Merritt, K. W., Mokhov, N., Morgan, J. P., Nguyen, H., Ostiguy, J-F., Para, A., Popovic, C. C. Polly M., Ramberg, E., Rominsky, M., Schoo, D., Schultz, R., Still, D., Soha, A. K., Strigonov, S., Tassotto, G., Turrioni, D., Villegas, E., Voirin, E., Velev, G., Welty-Rieger, L., Wolff, D., Worel, C., Wu, J-Y., Zifko, R., Jungmann, K., Onderwater, C. J. G., Debevec, P. T., Ganguly, S., Kasten, M., Leo, S., Pitts, K., Schlesier, C., Gaisser, M., Haciomeroglu, S., Kim, Y-I., Lee, S., Lee, M-J, Semertzidis, Y. K., Giovanetti, K., Baranov, V. A., Duginov, V. N., Khomutov, N. V., Krylov, V. A., Kuchinskiy, N. A., Volnykh, V. P., Crawford, C., Fatemi, R., Gohn, W. P., Gorringe, T. P., Korsch, W., Plaster, B., Anastasi, A., Babusci, D., Dabagov, S., Ferrari, C., Fioretti, A., Gabbanini, C., Hampai, D., Palladino, A., Venanzoni, G., Bowcock, T., Carroll, J., King, B., Maxfield, S., McCormick, K., Price, J., Sim, D., Smith, A., Teubner, T., Turner, W., Whitley, M., Wormald, M., Chislett, R., Kilani, S., Lancaster, M., Motuk, E., Stuttard, T., Warren, M., Flay, D., Kawall, D., Meadows, Z., Chupp, T., Raymond, R., Tewlsey-Booth, A., Syphers, M. J., Tarazona, D., Catalonotti, S., Di Stefano, R., Iacovacci, M., Mastroianni, S., Chattopadhyay, S., Eads, M., Fortner, M., Hedin, D., Pohlman, N., de Gouvea, A., Schellman, H., Azfar, F., Henry, S., Alkhazov, G. D., Golovtsov, V. L., Neustroev, P. V., Uvarov, L. N., Vasilyev, A. A., Vorobyov, A. A., Zhalov, M. B., Cerrito, L., Gray, F., Di Sciascio, G., Moricciani, D., Fu, C., Ji, X., Li, L., Yang, H., Stöckinger, D., Cantatore, G., Cauz, D., Karuza, M., Pauletta, G., Santi, L., Baeßler, S., Bychkov, M., Frlez, E., Pocanic, D., Alonzi, L. P., Fertl, M., Fienberg, A., Froemming, N., Garcia, A., Kaspar, D. W. Hertzog J., Kammel, P., Osofsky, R., Smith, M., Swanson, E., van Wechel, T., and Lynch, K.

Subjects
Physics - Instrumentation and Detectors, High Energy Physics - Experiment
Abstract

The Muon (g-2) Experiment, E989 at Fermilab, will measure the muon anomalous magnetic moment a factor-of-four more precisely than was done in E821 at the Brookhaven National Laboratory AGS. The E821 result appears to be greater than the Standard-Model prediction by more than three standard deviations. When combined with expected improvement in the Standard-Model hadronic contributions, E989 should be able to determine definitively whether or not the E821 result is evidence for physics beyond the Standard Model. After a review of the physics motivation and the basic technique, which will use the muon storage ring built at BNL and now relocated to Fermilab, the design of the new experiment is presented. This document was created in partial fulfillment of the requirements necessary to obtain DOE CD-2/3 approval., Comment: 666 pages

Published
2015

37. Measurement of the Cosmic Ray Energy Spectrum with ARGO-YBJ

Author

Di Sciascio, G.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract

The ARGO-YBJ detector, located at high altitude in the Cosmic Ray Observatory of Yangbajing in Tibet (4300 m asl, about 600 g/cm2 of atmospheric depth) provides the opportunity to study, with unprecedented resolution, the cosmic ray physics in the primary energy region between 10^{12} and 10^{16} eV. The preliminary results of the measurement of all-particle and light-component (i.e. protons and helium) energy spectra between approximately 5 TeV and 5 PeV are reported and discussed. The study of such energy region is particularly interesting because not only it allows a better understanding of the so called 'knee' of the energy spectrum and of its origin, but also provides a powerful cross-check among very different experimental techniques. The comparison between direct measurements by balloons/satellites and the results by surface detectors, implying the knowledge of shower development in the atmosphere, also allows to test the hadronic interaction models currently used for understanding particle and cosmic ray physics up the highest energies., Comment: 12 pages, 7 figures, to appear in the Proceedings of the VULCANO Workshop 2014, "Frontier Objects in Astrophysics and Particle Physics", Vulcano May 18-24, 2014, Frascati Physics Series Vol. 58 (2014)

Published
2014

38. On the Observation of the Cosmic Ray Anisotropy below 10$^{15}$ eV

Author

Di Sciascio, G. and Iuppa, R.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract

The measurement of the anisotropy in the arrival direction of cosmic rays is complementary to the study of their energy spectrum and chemical composition to understand their origin and propagation. It is also a tool to probe the structure of the magnetic fields through which cosmic rays travel. As cosmic rays are mostly charged nuclei, their trajectories are deflected by the action of galactic magnetic field they propagate through before reaching the Earth atmosphere, so that their detection carries directional information only up to distances as large as their gyro-radius. If cosmic rays below $10^{15}{\rm\,eV}$ are considered and the local galactic magnetic field ($\sim3{\rm\,\mu G}$) is accounted for, gyro-radii are so short that isotropy is expected. At most, a weak di-polar distribution may exist, reflecting the contribution of the closest CR sources. However, a number of experiments observed an energy-dependent \emph{"large scale"} anisotropy in the sidereal time frame with an amplitude of about 10$^{-4}$ - 10$^{-3}$, revealing the existence of two distinct broad regions: an excess distributed around 40$^{\circ}$ to 90$^{\circ}$ in Right Ascension (commonly referred to as "tail.in" excess) and a deficit (the "loss cone") around 150$^{\circ}$ to 240$^{\circ}$ in Right Ascension. In recent years the Milagro and ARGO-YBJ collaborations reported the of a "medium" scale anisotropy inside the tail-in region. The observation of such small features has been recently claimed by the IceCube experiment also in the Southern hemisphere. So far, no theory of cosmic rays in the Galaxy exists which is able to explain the origin of these different anisotropies leaving the standard model of cosmic rays and that of the galactic magnetic field unchanged at the same time., Comment: 42 pages, updated version of the invited review in the book "Homage to the discovery of Cosmic Rays", Nova Science Publishers, New York, 2013

Published
2014

39. 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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40. 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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41. 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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42. CTA contributions to the 33rd International Cosmic Ray Conference (ICRC2013)

Author

Consortium, The CTA, Abril, O., Acharya, B. S., Actis, M., Agnetta, G., Aguilar, J. A., Aharonian, F., Ajello, M., Akhperjanian, A., Alcubierre, M., Aleksic, J., Alfaro, R., Aliu, E., Allafort, A. J., Allan, D., Allekotte, I., Aloisio, R., Amato, E., Ambrosi, G., Ambrosio, M., Anderson, J., Angüner, E. O., Antonelli, L. A., Antonuccio, V., Antonucci, M., Antoranz, P., Aravantinos, A., Argan, A., Arlen, T., Aramo, C., Armstrong, T., Arnaldi, H., Arrabito, L., Asano, K., Ashton, T., Asorey, H. G., Aune, T., Awane, Y., Baba, H., Babic, A., Baby, N., Bähr, J., Bais, A., Baixeras, C., Bajtlik, S., Balbo, M., Balis, D., Balkowski, C., Ballet, J., Bamba, A., Bandiera, R., Barber, A., Barbier, C., Barceló, M., Barnacka, A., Barnstedt, J., de Almeida, U. Barres, Barrio, J. A., Basili, A., Basso, S., Bastieri, D., Bauer, C., Baushev, A., Becciani, U., Becerra, J., Becherini, Y., Bechtol, K. C., Tjus, J. Becker, Beckmann, V., Bednarek, W., Behera, B., Belluso, M., Benbow, W., Berdugo, J., Berge, D., Berger, K., Bernard, F., Bernardino, T., Bernlöhr, K., Bertucci, B., Bhat, N., Bhattacharyya, S., Biasuzzi, B., Bigongiari, C., Biland, A., Billotta, S., Bird, T., Birsin, E., Bissaldi, E., Biteau, J., Bitossi, M., Blake, S., Bigas, O. Blanch, Blasi, P., Bobkov, A., Boccone, V., Böttcher, M., Bogacz, L., Bogart, J., Bogdan, M., Boisson, C., Gargallo, J. Boix, Bolmont, J., Bonanno, G., Bonardi, A., Bonev, T., Bonifacio, P., Bonnoli, G., Bordas, P., Borgland, A., Borkowski, J., Bose, R., Botner, O., Bottani, A., Bouchet, L., Bourgeat, M., Boutonnet, C., Bouvier, A., Brau-Nogué, S., Braun, I., Bretz, T., Briggs, M., Brigida, M., Bringmann, T., Britto, R., Brook, P., Brun, P., Brunetti, L., Bruno, P., Bucciantini, N., Buanes, T., Buckley, J., Bühler, R., Bugaev, V., Bulgarelli, A., Bulik, T., Busetto, G., Buson, S., Byrum, K., Cailles, M., Cameron, R., Camprecios, J., Canestrari, R., Cantu, S., Capalbi, M., Caraveo, P., Carmona, E., Carosi, A., Carosi, R., Carr, J., Carter, J., Carton, P. -H., Caruso, R., Casanova, S., Cascone, E., Casiraghi, M., Castellina, A., Catalano, O., Cavazzani, S., Cazaux, S., Cerchiara, P., Cerruti, M., Chabanne, E., Chadwick, P., Champion, C., Chaves, R., Cheimets, P., Chen, A., Chiang, J., Chiappetti, L., Chikawa, M., Chitnis, V. R., Chollet, F., Christof, A., Chudoba, J., Cieślar, M., Cillis, A., Cilmo, M., Codino, A., Cohen-Tanugi, J., Colafrancesco, S., Colin, P., Colome, J., Colonges, S., Compin, M., Conconi, P., Conforti, V., Connaughton, V., Conrad, J., Contreras, J. L., Coppi, P., Coridian, J., Corona, P., Corti, D., Cortina, J., Cossio, L., Costa, A., Costantini, H., Cotter, G., Courty, B., Couturier, S., Covino, S., Crimi, G., Criswell, S. J., Croston, J., Cusumano, G., Dafonseca, M., Dale, O., Daniel, M., Darling, J., Davids, I., Dazzi, F., de Angelis, A., De Caprio, V., De Frondat, F., Pino, E. M. de Gouveia Dal, de la Calle, I., De La Vega, G. A., Lopez, R. de los Reyes, de Lotto, B., De Luca, A., de Naurois, M., de Oliveira, Y., Wilhelmi, E. de Oña, de Palma, F., de Souza, V., Decerprit, G., Decock, G., Deil, C., Delagnes, E., Deleglise, G., Delgado, C., della Volpe, D., Demange, P., Depaola, G., Dettlaff, A., Di Girolamo, T., Di Giulio, C., Di Paola, A., Di Pierro, F., di Sciascio, G., Díaz, C., Dick, J., Dickherber, R., Dickinson, H., Diez-Blanco, V., Digel, S., Dimitrov, D., Disset, G., Djannati-Ataï, A., Doert, M., Dohmke, M., Domainko, W., Prester, D. Dominis, Donat, A., Dorner, D., Doro, M., Dournaux, J. -L., Drake, G., Dravins, D., Drury, L., Dubois, F., Dubois, R., Dubus, G., Dufour, C., Dumas, D., Dumm, J., Durand, D., Dwarkadas, V., Dyks, J., Dyrda, M., Ebr, J., Edy, E., Egberts, K., Eger, P., Einecke, S., Eleftheriadis, C., Elles, S., Emmanoulopoulos, D., Engelhaupt, D., Enomoto, R., Ernenwein, J. -P., Errando, M., Etchegoyen, A., Evans, P. A., Falcone, A., Faltenbacher, A., Fantinel, D., Farakos, K., Farnier, C., Farrell, E., Fasola, G., Favill, B. W., Fede, E., Federici, S., Fegan, S., Feinstein, F., Ferenc, D., Ferrando, P., Fesquet, M., Fetfatzis, P., Fiasson, A., Fillin-Martino, E., Fink, D., Finley, C., Finley, J. P., Fiorini, M., Curcoll, R. Firpo, Flandrini, E., Fleischhack, H., Flores, H., Florin, D., Focke, W., Föhr, C., Fokitis, E., Font, L., Fontaine, G., Fornasa, M., Förster, A., Fortson, L., Fouque, N., Franckowiak, A., Franco, F. J., Frankowski, A., Fransson, C., Fraser, G. W., Frei, R., Fresnillo, L., Fruck, C., Fugazza, D., Fujita, Y., Fukazawa, Y., Fukui, Y., Funk, S., Gäbele, W., Gabici, S., Gabriele, R., Gadola, A., Galante, N., Gall, D., Gallant, Y., Gámez-García, J., Garczarczyk, M., García, B., López, R. Garcia, Gardiol, D., Gargano, F., Garrido, D., Garrido, L., Gascon, D., Gaug, M., Gaweda, J., Gebremedhin, L., Geffroy, N., Gerard, L., Ghedina, A., Ghigo, M., Ghislain, P., Giannakaki, E., Gianotti, F., Giarrusso, S., Giavitto, G., Giebels, B., Giglietto, N., Gika, V., Giomi, M., Giommi, P., Giordano, F., Girard, N., Giro, E., Giuliani, A., Glanzman, T., Glicenstein, J. -F., Godinovic, N., Golev, V., Berisso, M. Gomez, Gómez-Ortega, J., Gonzalez, M. M., González, A., González, F., Muñoz, A. González, Gothe, K. S., Grabarczyk, T., Gougerot, M., Graciani, R., Grandi, P., Grañena, F., Granot, J., Grasseau, G., Gredig, R., Green, A., Greenshaw, T., Grégoire, T., Grillo, A., Grimm, O., Grondin, M. -H., Grube, J., Grudzinska, M., Gruev, V., Grünewald, S., Grygorczuk, J., Guarino, V., Gunji, S., Gyuk, G., Hadasch, D., Hagedorn, A., Hagiwara, R., Hahn, J., Hakansson, N., Hallgren, A., Heras, N. Hamer, Hara, S., Hardcastle, M. J., Harezlak, D., Harris, J., Hassan, T., Hatanaka, K., Haubold, T., Haupt, A., Hayakawa, T., Hayashida, M., Heller, R., Henault, F., Henri, G., Hermann, G., Hermel, R., Herrero, A., Hervet, O., Hidaka, N., Hinton, J. A., Hirotani, K., Hoffmann, D., Hofmann, W., Hofverberg, P., Holder, J., Hörandel, J. R., Horns, D., Horville, D., Houles, J., Hrabovsky, M., Hrupec, D., Huan, H., Huber, B., Huet, J. -M., Hughes, G., Humensky, T. B., Huovelin, J., Huppert, J. -F., Ibarra, A., Ikawa, D., Illa, J. M., Impiombato, D., Incorvaia, S., Inoue, S., Inoue, Y., Iocco, F., Ioka, K., Israel, G. L., Jablonski, C., Jacholkowska, A., Jacquemier, J., Jamrozy, M., Janiak, M., Jean, P., Jeanney, C., Jimenez, J. J., Jogler, T., Johnson, C., Johnson, T., Journet, L., Juffroy, C., Jung, I., Kaaret, P., Kabuki, S., Kagaya, M., Kakuwa, J., Kalkuhl, C., Kankanyan, R., Karastergiou, A., Kärcher, K., Karczewski, M., Karkar, S., Kasperek, J., Kastana, D., Katagiri, H., Kataoka, J., Katarzyński, K., Katz, U., Kawanaka, N., Kazanas, D., Kelley-Hoskins, N., Kellner-Leidel, B., Kelly, H., Kendziorra, E., Khélifi, B., Kieda, D. B., Kifune, T., Kihm, T., Kishimoto, T., Kitamoto, K., Kluźniak, W., Knapic, C., Knapp, J., Knödlseder, J., Köck, F., Kocot, J., Kodani, K., Köhne, J. -H., Kohri, K., Kokkotas, K., Kolitzus, D., Komin, N., Kominis, I., Konno, Y., Köppel, H., Korohoda, P., Kosack, K., Koss, G., Kossakowski, R., Koul, R., Kowal, G., Koyama, S., Kozioł, J., Krähenbühl, T., Krause, J., Krawzcynski, H., Krennrich, F., Krepps, A., Kretzschmann, A., Krobot, R., Krueger, P., Kubo, H., Kudryavtsev, V. A., Kushida, J., Kuznetsov, A., La Barbera, A., La Palombara, N., La Parola, V., La Rosa, G., Lacombe, K., Lamanna, G., Lande, J., Languignon, D., Lapington, J. S., Laporte, P., Laurent, B., Lavalley, C., Flour, T. Le, Padellec, A. Le, Lee, S. -H., Lee, W. H., Lefèvre, J. -P., Leich, H., de Oliveira, M. A. Leigui, Lelas, D., Lenain, J. -P., Leoni, R., Leopold, D. J., Lerch, T., Lessio, L., Leto, G., Lieunard, B., Lieunard, S., Lindemann, R., Lindfors, E., Liolios, A., Lipniacka, A., Lockart, H., Lohse, T., Lombardi, S., Longo, F., Lopatin, A., Lopez, M., López-Coto, R., López-Oramas, A., Lorca, A., Lorenz, E., Louis, F., Lubinski, P., Lucarelli, F., Lüdecke, H., Ludwin, J., Luque-Escamilla, P. L., Lustermann, W., Luz, O., Lyard, E., Maccarone, M. C., Maccarone, T. J., Madejski, G. M., Madhavan, A., Mahabir, M., Maier, G., Majumdar, P., Malaguti, G., Malaspina, G., Maltezos, S., Manalaysay, A., Mancilla, A., Mandat, D., Maneva, G., Mangano, A., Manigot, P., Mannheim, K., Manthos, I., Maragos, N., Marcowith, A., Mariotti, M., Marisaldi, M., Markoff, S., Marszałek, A., Martens, C., Martí, J., Martin, J. -M., Martin, P., Martínez, G., Martínez, F., Martínez, M., Massaro, F., Masserot, A., Mastichiadis, A., Mathieu, A., Matsumoto, H., Mattana, F., Mattiazzo, S., Maurer, A., Maurin, G., Maxfield, S., Maya, J., Mazin, D., Comb, L. Mc, McCann, A., McCubbin, N., McHardy, I., McKay, R., Meagher, K., Medina, C., Melioli, C., Melkumyan, D., Melo, D., Mereghetti, S., Mertsch, P., Meucci, M., Meyer, M., Michałowski, J., Micolon, P., Mihailidis, A., Mineo, T., Minuti, M., Mirabal, N., Mirabel, F., Miranda, J. M., Mirzoyan, R., Mistò, A., Mizuno, T., Moal, B., Moderski, R., Mognet, I., Molinari, E., Molinaro, M., Montaruli, T., Monte, C., Monteiro, I., Moore, P., Olaizola, A. Moralejo, Mordalska, M., Morello, C., Mori, K., Morlino, G., Morselli, A., Mottez, F., Moudden, Y., Moulin, E., Mrusek, I., Mukherjee, R., Munar-Adrover, P., Muraishi, H., Murase, K., Murphy, A. StJ., Nagataki, S., Naito, T., Nakajima, D., Nakamori, T., Nakayama, K., Naumann, C., Naumann, D., Naumann-Godo, M., Nayman, P., Nedbal, D., Neise, D., Nellen, L., Neronov, A., Neustroev, V., Neyroud, N., Nicastro, L., Nicolau-Kukliński, J., Niedźwiecki, A., Niemiec, J., Nieto, D., Nikolaidis, A., Nishijima, K., Nishikawa, K. -I., Noda, K., Nolan, S., Northrop, R., Nosek, D., Nowak, N., Nozato, A., Oakes, L., O'Brien, P. T., Ohira, Y., Ohishi, M., Ohm, S., Ohoka, H., Okuda, T., Okumura, A., Olive, J. -F., Ong, R. A., Orito, R., Orr, M., Osborne, J. P., Ostrowski, M., Otero, L. A., Otte, N., Ovcharov, E., Oya, I., Ozieblo, A., Padilla, L., Pagano, I., Paiano, S., Paillot, D., Paizis, A., Palanque, S., Palatka, M., Pallota, J., Palatiello, M., Panagiotidis, K., Panazol, J. -L., Paneque, D., Panter, M., Panzera, M. R., Paoletti, R., Papayannis, A., Papyan, G., Paredes, J. M., Pareschi, G., Parraud, J. -M., Parsons, D., Pauletta, G., Arribas, M. Paz, Pech, M., Pedaletti, G., Pelassa, V., Pelat, D., Perez, M. d. C., Persic, M., Petrucci, P. -O., Peyaud, B., Pichel, A., Pieloth, D., Pierre, E., Pita, S., Pivato, G., Pizzolato, F., Platino, M., Platos, Ł., Platzer, R., Podkladkin, S., Pogosyan, L., Pohl, M., Pojmanski, G., Ponz, J. D., Potter, W., Poutanen, J., Prandini, E., Prast, J., Preece, R., Profeti, F., Prokoph, H., Prouza, M., Proyetti, M., Puerto-Giménez, I., Pühlhofer, G., Puljak, I., Punch, M., Pyzioł, R., Quel, E. J., Quesada, J., Quinn, J., Quirrenbach, A., Racero, E., Rainò, S., Rajda, P. J., Rameez, M., Ramon, P., Rando, R., Rannot, R. C., Rataj, M., Raue, M., Ravignani, D., Reardon, P., Reimann, O., Reimer, A., Reimer, O., Reitberger, K., Renaud, M., Renner, S., Reville, B., Rhode, W., Ribó, M., Ribordy, M., Richards, G., Richer, M. G., Rico, J., Ridky, J., Rieger, F., Ringegni, P., Ripken, J., Ristori, P. R., Rivière, A., Rivoire, S., Rob, L., Rodeghiero, G., Roeser, U., Rohlfs, R., Rojas, G., Romano, P., Romaszkan, W., Romero, G. E., Rosen, S. R., Lees, S. Rosier, Ross, D., Rouaix, G., Rousselle, J., Rousselle, S., Rovero, A. C., Roy, F., Royer, S., Rudak, B., Rulten, C., Rupiński, M., Russo, F., Ryde, F., Saavedra, O., Sacco, B., Saemann, E. O., Saggion, A., Sahakian, V., Saito, K., Saito, T., Saito, Y., Sakaki, N., Sakonaka, R., Salini, A., Sanchez, F., Sanchez-Conde, M., Sandoval, A., Sandaker, H., Sant'Ambrogio, E., Santangelo, A., Santos, E. 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C., Stawarz, Ł., Steenkamp, R., Stegmann, C., Steiner, S., Stella, C., Stergioulas, N., Sternberger, R., Sterzel, M., Stinzing, F., Stodulski, M., Stolarczyk, Th., Straumann, U., Strazzeri, E., Stringhetti, L., Suarez, A., Suchenek, M., Sugawara, R., Sulanke, K. -H., Sun, S., Supanitsky, A. D., Suric, T., Sutcliffe, P., Sykes, J. M., Szanecki, M., Szepieniec, T., Szostek, A., Tagliaferri, G., Tajima, H., Takahashi, H., Takahashi, K., Takalo, L., Takami, H., Talbot, G., Tammi, J., Tanaka, M., Tanaka, S., Tasan, J., Tavani, M., Tavernet, J. -P., Tejedor, L. A., Telezhinsky, I., Temnikov, P., Tenzer, C., Terada, Y., Terrier, R., Teshima, M., Testa, V., Tezier, D., Thayer, J., Thuermann, D., Tibaldo, L., Tibolla, O., Tiengo, A., Timpanaro, M. C., Tluczykont, M., Peixoto, C. J. Todero, Tokanai, F., Tokarz, M., Toma, K., Tonachini, A., Torii, K., Tornikoski, M., Torres, D. F., Torres, M., Toscano, S., Toso, G., Tosti, G., Totani, T., Toussenel, F., Tovmassian, G., Travnicek, P., Treves, A., Trifoglio, M., Troyano, I., Tsinganos, K., Ueno, H., Umana, G., Umehara, K., Upadhya, S. S., Usher, T., Uslenghi, M., Vagnetti, F., Valdes-Galicia, J. F., Vallania, P., Vallejo, G., van Driel, W., van Eldik, C., Vandenbrouke, J., Vanderwalt, J., Vankov, H., Vasileiadis, G., Vassiliev, V., Veberic, D., Vegas, I., Vercellone, S., Vergani, S., Verzi, V., Vettolani, G. P., Veyssière, C., Vialle, J. P., Viana, A., Videla, M., Vigorito, C., Vincent, P., Vincent, S., Vink, J., Vlahakis, N., Vlahos, L., Vogler, P., Voisin, V., Vollhardt, A., von Gunten, H. -P., Vorobiov, S., Vuerli, C., Waegebaert, V., Wagner, R., Wagner, R. G., Wagner, S., Wakely, S. P., Walter, R., Walther, T., Warda, K., Warwick, R. S., Wawer, P., Wawrzaszek, R., Webb, N., Wegner, P., Weinstein, A., Weitzel, Q., Welsing, R., Werner, M., Wetteskind, H., White, R. J., Wierzcholska, A., Wiesand, S., Wilhelm, A., Wilkinson, M. I., Williams, D. A., Willingale, R., Winde, M., Winiarski, K., Wischnewski, R., Wiśniewski, Ł., Wojcik, P., Wood, M., Wörnlein, A., Xiong, Q., Yadav, K. K., Yamamoto, H., Yamamoto, T., Yamazaki, R., Yanagita, S., Yebras, J. M., Yelos, D., Yoshida, A., Yoshida, T., Yoshikoshi, T., Yu, P., Zabalza, V., Zacharias, M., Zajczyk, A., Zampieri, L., Zanin, R., Zdziarski, A., Zech, A., Zhao, A., Zhou, X., Zietara, K., Ziolkowski, J., Ziółkowski, P., Zitelli, V., Zurbach, C., and Zychowski, P.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, High Energy Physics - Experiment
Abstract

Compilation of CTA contributions to the proceedings of the 33rd International Cosmic Ray Conference (ICRC2013), which took place in 2-9 July, 2013, in Rio de Janeiro, Brazil, Comment: Index of CTA conference proceedings at the ICRC2013, Rio de Janeiro (Brazil). v1: placeholder with no arXiv links yet, to be replaced once individual contributions have been all submitted. v2: final with arXiv links to all CTA contributions and full author list

Published
2013

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

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., D’Ettorre Piazzoli, B., Di Girolamo, T., Di Sciascio, G., Feng, C.F., Feng, Zhaoyang, Feng, Zhenyong, Gou, Q.B., Guo, Y.Q., He, H.H., Hu, Haibing, Hu, Hongbo, Iacovacci, M., Iuppa, R., Jia, H.Y., Labaciren, Li, H.J., Liguori, G., Liu, C., Liu, J., Liu, M.Y., Lu, H., Ma, L.L., Ma, X.H., Mancarella, G., Mari, S.M., Marsella, G., Martello, D., Mastroianni, S., Montini, P., Ning, C.C., Panareo, M., Perrone, L., Pistilli, P., Ruggieri, F., Salvini, P., Santonico, R., Shen, P.R., Sheng, X.D., Shi, F., Surdo, A., Tan, Y.H., Vallania, P., Vernetto, S., Vigorito, C., Wang, H., Wu, C.Y., Wu, H.R., Xue, L., Yang, Q.Y., Yang, X.C., Yao, Z.G., Yuan, A.F., Zha, M., Zhang, H.M., Zhang, L., Zhang, X.Y., Zhang, Y., Zhao, J., Zhaxiciren, Zhaxisangzhu, Zhou, X.X., Zhu, F.R., Zhu, Q.Q., and Zizzi, G.

Published
2019
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45. ARGO-YBJ: Status and Highlights

Author

Di Sciascio, G.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract

The ARGO-YBJ experiment is in stable data taking since November 2007 at the YangBaJing Cosmic Ray Laboratory (Tibet, P.R. China, 4300 m a.s.l., 606 g/cm$^2$). ARGO-YBJ is facing open problems in Cosmic Ray (CR) physics in different ways. The search for CR sources is carried out by the observation of TeV gamma-ray sources both galactic and extra-galactic. The CR spectrum, composition and anisotropy are measured in a wide energy range (TeV - PeV) thus overlapping for the first time direct measurements. In this paper we summarize the current status of the experiment and describe some of the scientific highlights since 2007., Comment: Invited contribution to the Workshop "Frontier Objects in Astrophysics and Particle Physics", Vulcano (Italy) 28 May - 2 June 2012

Published
2012

46. 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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47. Measurement of Cosmic Ray spectrum and Anisotropy with ARGO-YBJ

Author

DI SCIASCIO, G.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract

In this paper we report on the observation of the anisotropy of cosmic ray arrival direction at different angular scales with ARGO-YBJ. Evidence of new few-degree excesses throughout the sky region 195$^{\circ}\leq$ R.A. $\leq$ 315$^{\circ}$ is presented for the first time. We report also on the measurement of the light-component (p+He) spectrum of primary cosmic rays in the range 5 - 200 TeV., Comment: Invited talk to the 3rd Galileo - Xu Guangqi meeting, October 11-15, 2011 Beijing (China)

Published
2012
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48. 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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49. Measurement of Cosmic Ray antiproton/proton flux ratio at TeV energies with ARGO-YBJ

Author

Di Sciascio, G., Iuppa, R., and collaboration, the ARGO-YBJ

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract

Cosmic ray antiprotons provide an important probe for the study of cosmic-ray propagation in the interstellar space and to investigate the existence of Galactic dark matter. The ARGO-YBJ experiment, located at the Yangbajing Cosmic Ray Laboratory (Tibet, P.R. China, 4300 m a.s.l., 606 g/cm$^2$), is the only experiment exploiting the full coverage approach at very high altitude presently at work. The ARGO-YBJ experiment is particularly effective in measuring the cosmic ray antimatter content via the observation of the cosmic rays Moon shadowing effect. Based on all the data recorded during the period from July 2006 through November 2009 and a full Monte Carlo simulation, we searched for the existence of the shadow produced by antiprotons at the few-TeV energy region. No evidence of the existence of antiprotons was found in this energy region. Upper limits to the antip/p flux ratio are set to 5 % at a median energy of 2 TeV and 6 % at 5 TeV with a confidence level of 90 %. In the few-TeV energy range this result is the lowest available., Comment: 4 pages, Contribution to the 32nd ICRC, August 11-18, 2011, Beijing (P.R. China)

Published
2011
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50. Observation of the Cosmic Ray Moon shadowing effect with the ARGO-YBJ experiment

Author

Di Sciascio, G. and Iuppa, R.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract

Cosmic rays are hampered by the Moon and a deficit in its direction is expected (the so-called \emph{Moon shadow}). The Moon shadow is an important tool to determine the performance of an air shower array. In fact, the displacement of the shadow center, due to the bending effect of the Geomagnetic field on the propagation of cosmic rays, allows to set the energy scale of the primary particles inducing the showers observed by the detector. The shape of the shadow permits to determine the detector point spread function. The position of the deficit at high energy allows evaluating its pointing accuracy. Here we present the observation of the cosmic ray Moon shadowing effect carried out by the ARGO-YBJ experiment (Yangbajing Cosmic Ray Laboratory, Tibet, P.R. China, 4300 m a.s.l., 606 g/cm$^2$) in the multi-TeV energy region with high statistical significance (70 standard deviations). By means of an accurate Monte Carlo simulation of the cosmic rays propagation in the Earth-Moon system we have studied the role of the Geomagnetic field and of the detector point spread function on the observed shadow., Comment: Contribution to the 32nd ICRC, August 11-18 2011, Beijing (P.R. China)

Published
2011
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