Search for excited electrons using the ZEUS detector

Derrick, M.; Krakauer, D.; Magill, S.; Musgrave, B.; Repond, J.; Repond, S.; Stanek, R. W.; Talaga, R. L.; Thron, J. L.; Arzarello, F.; Ayad, R.; Bari, G.; Basile, M.; Bellagamba, L.; Boscherini, D.; Bruni, A.; Bruni, G.; Bruni, P.; Romeo, G. Cara; Castellini, G.; Chiarini, M.; Cifarelli, L.; Cindolo, F.; Ciralli, F.; Contin, A.; D’Auria, S.; Papa, C. Del; Frasconi, F.; Giusti, P.; Iacobucci, G.; Laurenti, G.; Levi, G.; Lin, Q.; Lisowski, B.; Maccarrone, G.; Margotti, A.; Massam, T.; Nania, R.; Memoz, C.; Palmonari, F.; Sartorelli, G.; Timellini, R.; Garcia, Y. Zamora; Zichichi, A.; Bargende, A.; Crittenden, J.; Dabbous, H.; Desch, K.; Diekmann, B.; Doeker, T.; Geerts, M.; Geitz, G.; Hartmann, H.; Haun, Daniel B. M.; Héinloth, K.; Hilger, E.; Jakob, H.‐P.; Kramarczyk, S.; Kückes, M.; Mass, A.; Mengel, S.; Mollen, J.; Monaldi, Daniela; Müsch, H.; Paul, E.; Schattevoy, R.; Schneider, J.-L.; Schramm, David N.; Wedemeyer, R.; Cassidy, A.; Cussans, D.; Dyce, N.; Foster, B.; Gilmore, R.; Heath, G. P.; Heath, H. F.; Lancaster, M.; Llewellyn, T.J.; Malos, J.; Morgado, Cjs; Tapper, R. J.; Wilson, Stephen; Yoshida, R.; Rau, R. R.; Arneodo, M.; Barillari, T.; Schioppa, M.; Susinno, G.; Bernstein, Adam; Caldwell, A.; Gialas, I.; Parsons, J. A.; Ritz, S.; Sciulli, F.; Straub, P.B.; Wai, L.; Yang, S.; Chwastowski, J. J.; Dwuraźny, A.; Eskreys, A.; Jakubowski, Z.; Niziol, B.; Piotrzkowski, K.; Zachara, M.; Zawiejski, L.; Bednarek, B.; Borzemski, P.; Eskreys, K.; Jeleń, K.; Kisielewska, D.; Kowalski, T.; Rulikowska-Zarȩbska, E.; Suszycki, L.; Zając, Józef; Kȩdzierski, T.; Kotański, A.; Przybycień, M.; Bauerdick, L. A. T.; Behrens, U.; Bienlein, J. K.; Böttcher, S.; Coldewey, C.; Dannemann, A.; Drews, G.; Erhard, P.; Flasiński, Mariusz; Fleck, I.; Gläser, R.; Göttlicher, P.; Gutjahr, B.; Haas, T.; Hagge, Lars; Hain, W.; Hasell, D.; Hultschig, H.; Jahnen, G.; Joos, P.; Kasemann, M.; Klanner, R.; Koch, W.; Köpke, L.; Kötz, U.; Kowalski, H.; Krüger, J.; Labs, J.; Ladage, A.; Löhr, B.; Löwe, M.; Lüke, D.; Mainusch, J.; Mańczak, O.; Momayezi, M.; Ng, J. S. T.; Nickel, Stefan; Notz, D.; Pösnecker, K. U.; Rohde, M.; Roldán, J.; Ros, E.; Schneekloth, U.; Schroeder, J.; Schulz, W.; Selonke, F.; Stiliaris, E.; Tscheslog, E.; Tsurugai, T.; Vogel, W.; Wolf, G.; Youngman, C.; Grabosch, H. J.; Leich, A.; Meyer, Andreas Bernhard; Rethfeldt, C.; Schlenstedt, S.; Barbagli, G.; Francescato, A.; Nuti, Marco; Pelfer, P. G.; Anzivino, G.; Casaccia, R.; Pasquale, S. De; Qian, S. J.; Votano, L.; Bamberger, A.; Freidhof, A.; Kröger, W.; Poser, T.; Söldner-Rembold, S.; Theisen, G.; Trefzger, T.; Brook, N. H.; Bussey, P.; Doyle, A. T.; Forbes, J.R.; Jamieson, V.A.; Raine, C.; Saxon, D. H.; Brückmann, H.; Gloth, G.; Holm, U.; Kammerlocher, H.; Krebs, B.; Neumann, T.; Wick, K.; Fürtjes, A.; Lohrmann, E.; Milewski, J.; Nakahata, M.; Pavel, N.; Poelz, G.; Schott, W.; Terrón, J.; Zetsche, Frank; Bacon, T. C.; Beuselinck, R.; Butterworth, I.; Gallo, E.; Harris, V. L.; Miller, D. B.; Prinias, A.; Sedgbeer, J. K.; Vorvolakos, A.; Whitfield, A. F.; Bienz, T.; Kreutzmann, H.; Mallik, U.; McCliment, E.; Roco, M.; Wang, M.-Z.; Cloth, P.; Filges, P.; An, S. H.; Hong, S.; Kim, C.O.; Kim, T.Y.; Nam, S.; Park, S.K.; Suh, M. H.; Yon, S. H.; Imlay, R.; Kartik, S.; Kim, H.-J.; McNeil, R. R.; Metcalf, W.; Nadendla, V. K.; Barreiro, F.; Cases, G.; Hervás, L.; Labarga, L.; Peso, J. Del; Trocóniz, J. F. de; Ikraiam, F.; Mayer, J.; Smith, G. R.; Corriveau, F.; Gilkinson, D. J.; Hanna, D.; Hartmann, J.; Hung, L. W.; Lim, J.; Drees, R. Meijer; Mitchell, J. W.; Patel, P. M.; Sinclair, L.E.; Stairs, D. G.; St.Laurent, M.; Ullmann, R.; Bashindzhagyan, G. L.; Ermolov, P.; Gladilin, L. K.; Golubkov, Yu. A.; Kuzmin, V. A.; Kuznetsov, E.; Savin, A.A.; Voronin, A.; Zotov, N. P.; Bentvelsen, S.; Botje, M.; Dake, A.; Engelen, J.; Jong, P. de; Kamps, Marc de; Kooijman, P.; Kruse, A.; Lugt, H. van der; O’Dell, V.; Tenner, A.; Tiecke, H.; Uijterwaal, H.; Vreeswijk, M.; Wiggers, L.; Wolf, E. de; Woudenberg, R. van; Bylsma, B.; Durkin, L. S.; Honscheid, K.; Li, C.; Ling, T. Y.; McLean, K. W.; Murray, W. N.; Park, I.H.; Romanowski, T. A.; Seidlein, R.; Blair, G.A.; Byrne, A.; Cashmore, R. J.; Cooper-Sarkar, A. M.; Devenish, R.C.E.; Gingrich, D. M.; Hallam-Baker, Phillip; Harnew, N.; Khatri, T.; Long, K.; Luffman, P.; McArthur, I.; Morawitz, P.; Nash, J.A.; Smith, S.J.P.; Roocroft, N.C.; Wilson, F. F.; Abbiendi, G.; Brugnera, R.; Carlin, R.; Corso, F. Dal; Giorgi, M. De; Dosselli, U.; Gasparini, F.; Limentani, S.; Morandin, M.; Posocco, M.; Stančo, L.; Stroili, R.; Voci, C.; Butterworth, J. M.; Bulmahn, J.; Feild, G.; Oh, B.Y.; Whitmore, J. J.; Contino, U.; D’Agostini, G.; Guida, M.; Iori, M.; Mari, S. M.; Marini, G.; Mattioli, M.; Nigro, A.; Hart, J. C.; McCubbin, N. A.; Prytz, Kjell; Shah, T.; Short, T.L.; Barberis, E.; Cartiglia, N.; Heusch, C. A.; Hubbard, B.; Leslie, J. R.; Lockman, W. S.; O’Shaughnessy, K.; Sadronzinski, H. F. W.; Seiden, A.; Zer-Zion, D.; Badura, E.; Biltzinger, J.; Seifert, R. J.; Walenta, A.H.; Zech, G.; Dagan, S.; Levy, A.; Hasegawa, T.; Hazumi, M.; Ishii, T.; Kasai, S.; Kuze, M.; Nagasawa, Yutaka; Nakao, M.; Okuno, Hiroshi; Tokushuku, K.; Watanabe, Takayuki; Yamada, Shoichi; Chiba, M.; Hamatsu, R.; Hirose, T.; Kitamura, S.; Nagayama, S.; Nakamitsu, Y.; Cirio, R.; Costa, M.; Ferrero, M. I.; Lamberti, Luciano; Maselli, S.; Peroni, C.; Solano, A.; Staiano, A.; Dardo, M.; Bailey, D. C.; Bandyopadhyay, Debades; Bénard, F.; Bhadra, S.; Brkić, M.; Burow, B.D.; Chlebana, F.; Crombie, M.B.; Hartner, G.; Levman, G.; Martin, J. F.; Orr, R. S.; Prentice, J. D.; Sampson, C. R.; Stairs, G.G.; Teuscher, R. J.; Yoon, T. S.; Bullock, F. W.; Catterall, C. D.; Giddings, J. Calvin; Jones, T. W.; Khan, A.; Lane, J.B.; Makkar, P.L.; Shaw, D.; Shulman, J.; Blankenship, Kevin; Kochocki, J.; Lu, B.; Mo, L. W.; Charchuła, K.; Ciborowski, J.; Gajewski, J.; Grzelak, G.; Kasprzak, M.; Krzyżanowski, M.; Muchorowski, K.; Nowak, R. J.; Pawlak, J. M.; Stopczyński, Andrzej; Tymieniecka, T.; Walczak, R.; Wróblewski, A.; Zakrzewski, J.; Żarnecki, Aleksander Filip; Adamus, M.; Abramowicz, H.; Eisenberg, Y.; Glasman, C.; Karshon, U.; Montag, A.; Revel, D.; Shapira, A.; Foudas, C.; Fordham, C.; Loveless, R.; Goussiou, A. G.; Ali, I.; Behrens, B. H.; Dasu, S.; Reeder, D.D.; Smith, W. H.; Silverstein, S.; Frisken, W. R.; Furutani, K.M.; Iga, Y.

doi:10.1016/0370-2693(93)90680-g

Cited by 37 publications

(49 citation statements)

References 52 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In fact, in [1,2,3] non-steep (valencelike) initial distributions xf (x, µ 2 ) at some low scale µ ≈ 0.6 GeV were suggested in order to predict, purely dynamically, the rise of xq and xg in the above range of x and Q 2 . This prediction was subsequently confirmed by the measurements of F p 2 (x, Q 2 ) and xg(x, Q 2 ) at HERA [4,5]. As was stated in [2,3], the available pre-HERA data at x > 10 −2 utilized to fix the valence-like input distributions still allowed for a slight, typically O(10%), variation (increase) of µ which did not affect F 2 (x > 10 −2 , Q 2 ) but resulted in an about 10% (20%) uncertainty of the radiative predictions at x = 10 −3 (10 −4 ).…”

Section: Introductionsupporting

confidence: 52%

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Dynamical parton distributions revisited

1998

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Dynamical parton densities, generated radiatively from valence-like inputs at some low resolution scale, are confronted with recent small-x data on deep inelastic and other hard scattering processes. It is shown that within theoretical uncertainties our previous (1994) dynamical/radiative parton distributions are compatible with most recent data and still applicable within the restricted accuracy margins of the presently available next-to-leading order calculations. Due to recent high precision measurements we also present an updated, more accurate, version of our (valence-like) dynamical input distributions. Furthermore, our perturbatively stable parameter-free dynamical predictions are extended to the extremely small-x region, 10 −8 < ∼ x < ∼ 10 −5 , relevant to questions concerning ultra-high-energy cosmic ray and neutrino astronomy.

show abstract

Section: Introductionsupporting

confidence: 52%

“…Fig. 7 Comparison of our LO and NLO fits with fixed-target F p 2 data [17,18,19,20,21] in the Q 2 ≥ 4 GeV 2 , W 2 ≥ 10 GeV 2 region which were used for determining the valence and valence-like gluon and sea input in (5) and (6). The data sets are shown with their normalization factors as obtained in the fit.…”

Section: Discussion and Summarymentioning

confidence: 99%

Dynamical parton distributions revisited

1998

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“…The minimum estimated flux may be beyond the reach of the current generation of neutrino detectors mentioned above. I have reassessed the detectability of a wide range of flux predictions using calculations of the neutrino cross sections based on nucleon structure function parameterizations [18,19] (parton distributions) derived from recent accelerator experiments [20,21,22,23]. Use of the new parton distributions leads to higher cross sections and a corresponding increased probability of a detectable muon being produced in the rock surrounding a detector.…”

Section: Introductionmentioning

confidence: 99%

Detecting neutrinos from AGN: New fluxes and cross sections

Hill¹

1997

Astroparticle Physics

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New information on the structure of the nucleon from the HERA ep collider leads to higher neutrino cross sections for the processes ν µ (ν µ ) + N → µ − (µ + ) + X needed to calculate the expected rates of astrophysical neutrino induced muons in large detectors either under construction, or in the design stage. These higher cross sections lead to higher muon rates for arrival angles where neutrino attenuation in the earth is less important. On the other hand, new estimates of AGN neutrino fluxes suggest that the expected muon rates in these detectors may be much lower than previously calculated. I use the new cross sections to calculate the expected muon rates and angular distributions in large detectors for a variety of AGN models and compare these rates with the atmospheric neutrino backrounds (from both conventional decay channels and the 'prompt' charmed meson decay channels). If the lowest flux estimates are correct, there may be diffculties in determining the origin of a small excess of muons, due to the large uncertainty in the rate of the charmed meson neutrino production channel. However, the more optimistic AGN neutrino fluxes should be detectable in proposed detectors, such as DUMAND-II, AMANDA, NESTOR and Lake Baikal.

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“…The measurement of the proton structure function F 2 is one of the major achievements of HERA. Several measurements have been performed taking advantage of the increasing luminosity and improved detectors and reconstruction methods [5][6][7][8][9][11][12][13][14]. The results shown here are preliminary results from the H1 collaboration.…”

Section: Results From Deep Inelastic Scatteringmentioning

confidence: 99%

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Bornheim

Herbeck

1998

Small Business Economics

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Measurements of the total cross section for real and virtual photons on protons at center-of-mass energies in the range from 20 GeV to 270 GeV with photon virtualities up to 5000 GeV 2 are presented. For real photons this cross section can be described by Regge-motivated models while for virtual photons perturbative QCD can be applied. The measurements of the two HERA collider experiments ZEUS and H1 open the possibility to investigate the interplay between the two theoretical approaches in the transition region as well as the high-energy behavior of the cross sections. The results of total cross section measurements are discussed in the above context.Contribution to the proceedings of the

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Search for excited electrons using the ZEUS detector

Cited by 37 publications

References 52 publications

Dynamical parton distributions revisited

Dynamical parton distributions revisited

Detecting neutrinos from AGN: New fluxes and cross sections

Untitled

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