A search for flaring very-high-energy cosmic γ-ray sources with the L3+C muon spectrometer

Achard, P.; Адриани, О.; Aguilar-Benı́tez, M.; Akker, M. van den; Alcaraz, J.; Alemanni, G.; Allaby, J.; Aloisio, A.; Alviggi, M. G.; Anderhub, H.; Andreev, V.; Anselmo, F.; Arefiev, A.; Azemoon, T.; Aziz, T.; Bagnaia, P.; Bajo, A.; Baksay, G.; Baksay, L.; Bähr, J.; Baldew, S.V.; Banerjee, S.; Barczyk, A.; Barillère, R.; Bartalini, P.; Basile, M.; Batalova, N.; Battiston, R.; Bay, A.; Becattini, F.; Becker, U.; Behner, F.; Bellucci, L.; Berbeco, R.; Berdugo, J.; Berges, P.; Bertucci, B.; Betev, B. L.; Biasini, M.; Biglietti, M.; Biland, A.; Blaising, J. J.; Blyth, S.; Bobbink, G. J.; Böhm, A.; Boldizsár, L.; Borgia, B.; Bottai, S.; Bourilkov, D.; Bourquin, M.; Braccini, S.; Branson, J. G.; Brochu, F. M.; Bürger, J.; Burger, W. J.; Cai, Xudong; Capell, M.; Romeo, G.; Carlino, G.; Cartacci, A. M.; Casaus, J.; Cavallari, F.; Cavallo, N.; Cecchi, C.; Cerrada, M.; Chamizo, M.; Chang, Y. H.; Chemarin, M.; Chen, A.; Chen, G.; Chen, G.M.; Chen, H.F.; Chen, H.S.; Chiarusi, T.; Chiefari, G.; Cifarelli, L.; Cindolo, F.; Clare, I.; Clare, R.; Coignet, G.; Colino, N.; Costantini, S.; Cruz, B. De La; Cucciarelli, S.; Asmundis, R. de; Déglon, P.; Debreczeni, J.; Degré, A.; Dehmelt, K.; Deiters, K.; Volpe, D. della; Delmeire, E.; Denes, P.; DeNotaristefani, F.; Salvo, A. De; Diemoz, M.; Dierckxsens, M.; Ding, L. K.; Dionisi, C.; Dittmar, M.; Doria, A.; Dova, M. T.; Duchesneau, D.; Duda, Michał; Durán, I.; Echenard, B.; Eline, A.; Hage, A. El; Mamouni, H. El; Engler, A.; Eppling, Frederic J.; Extermann, P.; Faber, G.; Falagán, M. A.; Falciano, S.; Favara, A.; Fay, Jonathan; Fedin, O. L.; Felcini, M.; Ferguson, T.; Fesefeldt, H.; Fiandrini, E.; Field, J. H.; Filthaut, F.; Fisher, P. H.; Fisher, Wade Cameron; Fisk, I.; Forconì, G.; Freudenreich, K.; Furetta, C.; Galaktionov, Yu.; Ganguli, S. N.; Garcı́a-Abia, P.; Gataullin, M.; Gentile, S.; Giagu, S.; Gong, Z. F.; Grabosch, H. J.; Grenier, G. J.; Grimm, O.; Groenstege, H.; Gruenewald, M. W.; Guida, M.; Guo, Y.N.; Gupta, Sunil; Gupta, V. K.; Gurtu, A.; Gutay, L.; Haas, D.; Haller, C.; Hatzifotiadou, D.; Hayashi, Y.; He, Zhi-Guo; Hebbeker, T.; Hervé, A. E.; Hirschfelder, J.; Hofer, H.; Hohlmann, M.; Holzner, G.; Hou, Shaocong; Huo, A. X.; Ito, N.; Jin, B. N.; Jindal, P.; Jing, C. L.; Jones, L. W.; Jong, P. de; Josa-Mutuberrı́a, I.; Kantserov, V. A.; Kaur, M.; Kawakami, Satoshi; Kienzle‐Focacci, M. N.; Kim, J.K.; Kirkby, J.; Kittel, W.; Klimentov, A.; König, A. C.; Kok, E.; Korn, A.; Kopál, M.; Koutsenko, V.; Kräber, M.; Kuang, H.H.; Kraemer, R.W.; Krüger, A.; Kuijpers, J.; Kunin, A.; Guevara, P. Ladrón de; Laktineh, I. B.; Landi, G.; Lebeau, M.; Lebedev, A. P.; Lebrun, P.; Lecomte, P.; Lecoq, P.; Coultre, P. Le; Goff, J. M. Le; Lei, Y. J.; Leich, H.; Leiste, R.; Levtchenko, M.; Levtchenko, P.; Li, C.; Li, L.; Li, Z.C.; Likhoded, S.; Lin, Chao-Hung; Lin, Weikang; Linde, F.; Lista, L.; Liu, Z.A.; Lohmann, W.; Longo, E.; Lu, Y. S.; Luci, C.; Luminari, L.; Lustermann, W.; Wen-Gan, Ma; Ma, Xiaohua; Ma, Yuqian; Malgeri, L.; Малинин, А.; Mañá, C.; Mans, J.; Martín, J. P.; Marzano, F.; Mazumdar, K.; McNeil, R. R.; Mele, S.; Meng, X.; Merola, L.; Meschini, M.; Metzger, W. J.; Mihul, A.; Mil, A. van; Milcent, H.; Mirabelli, G.; Mnich, J.; Mohanty, G. B.; Monteleoni, B.; Muanza, G. S.; Muijs, A. J.M.; Musicar, B.; Musy, M.; Nagy, S.; Nahnhauer, R.; Naumov, Vadim A.; Natale, Sonia; Napolitano, M.; Nessi‐Tedaldi, F.; Newman, H. B.; Nisati, A.; Novák, T.; Nowak, H.; Ofierzynski, R. A.; Organtini, G.; Pal, I.; Palomares, C.; Paolucci, P.; Paramatti, R.; Parriaud, J.-F.; Passaleva, G.; Patricelli, S.; Paul, T.; Pauluzzi, M.; Paus, C.; Pauß, F.; Pedace, M.; Pensotti, S.; Perret-Gallix, D.; Petersen, B. A.; Piccolo, D.; Pierella, F.; Pieri, M.; Pioppí, M.; Piroué, P.; Pistolesi, E.; Plyaskin, V.; Pohl, M.; Pojidaev, V.; Pothier, J.; Prokofiev, D.; Quartieri, J.; Cheng-Rui, Qing; Rahal-Callot, G.; Rahaman, M. A.; Raics, P.; Raja, N.; Ramelli, R.; Rancoita, P.G.; Ranieri, R.; Raspereza, A.; Ravindran, K.; Razis, P. A.; Ren, D.; Rescigno, M.; Reucroft, S.; Rewiersma, P.; Riemann, S.; Riles, K.; Roe, B.P.; Rojkov, A.; Romero, L.; Rosca, A.; Rosemann, C.; Rosenbleck, C.; Rosier‐Lees, S.; Roth, Stefan; Rubio, Juan Antonio; Ruggiero, G.; Rykaczewski, H.; Saidi, R.; Sakharov, A.; Saremi, S.; Sarkar, S.; Salicio, J.; Sánchez, E.; Schäfer, C.; Schegelsky, V. A.; Schmitt, V.; Schoeneich, B.; Schopper, H.; Schotanus, D. J.; Sciacca, C.; Servoli, L.; Shen, C.; Shevchenko, S.; Shivarov, N.; Shoutko, V.; Shumilov, E.; Shvorob, A.; Son, D.; Souga, C.; Спиллантини, П.; Steuer, M.; Stickland, D.; Stoyanov, B.; Straessner, A.; Sudhakar, K.; Sulanke, H.; Sultanov, G.; Sun, L.; Sushkov, S.; Suter, H.; Swain, J. D.; Szillási, Z.; Tang, X. W.; Tarján, P.; Tauscher, L.; Taylor, L.; Tellili, B.; Teyssier, D.; Timmermans, C.; Ting, Samuel C.C.; Ting, Susan Marks; Tonwar, S. C.; Töth, J.; Trowitzsch, G.; Tully, C.; Tung, K. L.; Ulbricht, J.; Unger, Michael; Valente, E.; Verkooijen, H.; Walle, R. T. Van de; Vasquez, Raymond; Veszprémi, V.; Vesztergombi, G.; Vetlitsky, I.; Vicinanza, D.; Viertel, G.; Villa, S.; Vivargent, M.; Vlachos, S.; Vodopianov, I.; Vogel, H.; Vogt, H.; Vorobiev, I.; Vorobyov, A. A.; Wadhwa, M.; Wang, R.G.; Wang, Q.; Wang, X.L.; Wang, X.W.; Wang, Z.M.; Weber, M.; Wijk, R. van; Wijnen, T.; Wilkens, H. G.; Wynhoff, S.; Liu, Xia; Xu, Yupeng; Xu, J.; Xu, Z.; Yang, B. Z.; Yang, C.; Yang, H. J.; Yang, M.; Yang, Xinzheng; Yao, Z. G.; Yeh, S. C.; Yu, Zhao-Huan; Zalite, A.; Zalite, Y.; Zhang, C.; Zhang, F.; Zhang, J.; Zhang, S.; Zhang, Z.P.; Zhao, J.; Zhou, S.; Zhu, G. Y.; Zhu, Ruilin; Zhu, Q. Q.; Zhuang, H.L.; Zichichi, A.; Zimmermann, B.; Zöller, Margot; Zwart, A.

doi:10.1016/j.astropartphys.2006.03.007

Cited by 4 publications

(2 citation statements)

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“…The related conventional value for this observable is 3 11 R e + e − = 1.0461 +0.0015 −0.0008 [5]. Since there are experimental data for R e + e − up to center of mass energy 208 GeV [25] or even more, we do as well the required calculations in the McKeon et al approach, taking Λ MS = 210 +14 −14 M eV at the energy scales 42.5 and 56.5 GeV. What we obtain for 3 11 R e + e − at these energy scales are 1.0463 and 1.0441 respectively which are comparable with their experimental values, i.e.…”

Section: A Electron-positron Annihilation In Mckeon and At Al Approachmentioning

confidence: 99%

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Comparing optimized renormalization schemes for QCD observables

Akrami

Mirjalili

2020

Phys. Rev. D

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In this article based on the McKeon et al . approach, it can be shown that the renormalization group equation while it is related to the radiatively mass scale µ, operates to do a summation over QCD perturbative terms. Employing the full QCD β-function within this summation, all logarithmic corrections can be presented as the log-independent contributions. In another step of this approach , the renormalization scheme dependence for QCD observable which is characterised by Stevenson, can be examined by specifying the renormalization scheme in which the β-function beyond two-loop orders is utilized. In this regard two choices of renormalization schemes would be exposed. In one of them the QCD observable is expressed while involves two powers of running coupling constant such that the perturbative series contains just two terms. In another choice the perturbative series expansion is written as an infinite series in terms of two-loop running coupling which can be presented by Lambert W -function. In both cases the QCD observable involves parameters which are renormalization scheme invariant and the coupling constant which is independent of renormalization scale. We then consider the other approach which is called the complete renormalization group improvement (CORGI). In this approach, using the self consistency principle it is possible to reconstruct the conventional perturbative series in terms of scheme invariant quantities and the coupling constant as a function of Lambert-W function. It should be noted while in the renormalization group summation method of McKeon et al ., scheme dependence of observables is investigated separately from their scale dependence, in CORGI approach, through the principle of self consistency, both scale and scheme parameters are utilized together. In continuation we examine numerically these two approaches, considering two QCD observable. The first one is R e + e − ratio, investigated at three different colliding energies and the second observable is Higgs decay width to gluon-gluon. Comparison for R e + e − with the available experimental is done. The results based on the McKeon et al . approach are in better agreement with the experimental data.

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Section: A Electron-positron Annihilation In Mckeon and At Al Approachmentioning

confidence: 99%

“…(113) which can be done usingEqs. (108,111)where r i coefficients have been calculated in[25]. The results for these RS invariant quantities are as fo;;owing: GeV and Λ n f =5 QCD = 210 ± 10 M eV the numerical result for Higgs decay width would be: Γ(H → gg) = 0.393 ± 0.025 M eV.…”

mentioning

confidence: 96%

Comparing optimized renormalization schemes for QCD observables

Akrami

Mirjalili

2020

Phys. Rev. D

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Observation of a VHE cosmic-ray flare-signal with the L3+C muon spectrometer

Адриани

Akker

Aziz

et al. 2010

Astroparticle Physics

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a b s t r a c tThe data collected by the L3+C muon spectrometer at the CERN Large Electron-Positron collider, LEP, have been used to search for short duration signals emitted by cosmic point sources. A sky survey performed from July to November 1999 and from April to November 2000 has revealed one single flux enhancement ðchance probability ¼ 2:6 Â 10 À3 Þ between the 17th and 20th of August 2000 from a direction with a galactic longitude of (265.02 ± 0.42)°and latitude of (55.58 ± 0.24)°. The energy of the detected muons was above 15 GeV.

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L3+C: status of the data analysis

Yao

2008

Nuclear Physics B - Proceedings Supplements

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A search for flaring very-high-energy cosmic γ-ray sources with the L3+C muon spectrometer

Abstract: The L3+C muon detector at the CERN electron-positron collider, LEP, is used for the detection of very-high-energy cosmic γ-ray sources through the observation of muons of energies above 20, 30,

Cited by 4 publications

References 36 publications

Comparing optimized renormalization schemes for QCD observables

Comparing optimized renormalization schemes for QCD observables

Observation of a VHE cosmic-ray flare-signal with the L3+C muon spectrometer

L3+C: status of the data analysis

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