Measurements of quasi-trapped electron and positron fluxes with PAMELA

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1 JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 114,, doi: /2009ja014660, 2009 Measurements of quasi-trapped electron and positron fluxes with PAMELA O. Adriani, 1,2 G. Barbarino, 3,4 G. A. Bazilevskaya, 5 R. Bellotti, 6,7 M. Boezio, 8,9 E. A. Bogomolov, 10 L. Bonechi, 1,2 M. Bongi, 1,2 V. Bonvicini, 8,9 S. V. Borisov, 11 S. Bottai, 1,2 A. Bruno, 6,7 F. S. Cafagna, 6,7 D. Campana, 3,4 R. Carbone, 3,4 P. Carlson, 12,13 M. Casolino, 14,15 G. Castellini, 16 L. Consiglio, 3,4 M. P. De Pascale, 14,15 C. De Santis, 14,15 N. De Simone, 14,15 V. Di Felice, 14,15 A. M. Galper, 11 W. Gillard, 12,13 L. A. Grishantseva, 11 G. Jerse, 8,9 P. Hofverberg, 12,13 A. V. Karelin, 11 S. V. Koldashov, 11 S. Y. Krutkov, 10 A. N. Kvashnin, 5 A. A. Leonov, 11 V. V. Malakhov, 11 V. Malvezzi, 14,15 L. Marcelli, 14,15 A. G. Mayorov, 11 W. Menn, 17 V. V. Mikhailov, 11 E. Mocchiutti, 8,9 A. Monaco, 6,7 N. Mori, 1,2 N. N. Nikonov, 10 G. Osteria, 3,4 P. Papini, 1,2 M. Pearce, 12,13 P. Picozza, 14,15 C. Pizzolotto, 8,9 M. Ricci, 18 S. B. Ricciarini, 1,2 L. Rossetto, 12,13 S. Ritabrata, 8,9 M. F. Runtso, 11 M. Simon, 17 R. Sparvoli, 14,15 P. Spillantini, 1,2 Y. I. Stozhkov, 5 A. Vacchi, 8,9 E. Vannuccini, 1,2 G. I. Vasilyev, 10 S. A. Voronov, 11 J. Wu, 12,13 Y. T. Yurkin, 11 G. Zampa, 8,9 N. Zampa, 8,9 and V. G. Zverev 11 Received 20 July 2009; revised 22 September 2009; accepted 3 November 2009; published 29 December [1] This paper presents precise measurements of the differential energy spectra of quasi-trapped secondary electrons and positrons and their ratio between 80 MeV and 10 GeV in the near-equatorial region (altitudes between 350 km and 600 km). Latitudinal dependences of the spectra are analyzed in detail. The results were obtained from July until November 2006 onboard the Resurs-DK satellite by the PAMELA spectrometer, a general purpose cosmic ray detector system built around a permanent magnet spectrometer and a silicon-tungsten calorimeter. Citation: Adriani, O., et al. (2009), Measurements of quasi-trapped electron and positron fluxes with PAMELA, J. Geophys. Res., 114,, doi: /2009ja Introduction [2] Interactions of primary cosmic rays with residual atmospheric nuclei produce secondary leptons through the p ± decay chain (p ±! m ±! e ± ). According to Grigorov [1977], the 1 Sezione di Florence, INFN, Florence, Italy. 2 Department of Physics, University of Florence, Florence, Italy. 3 Sezione di Naples, INFN, Naples, Italy. 4 Department of Physics, University of Naples Federico II, Naples, Italy. 5 Lebedev Physical Institute, Moscow, Russia. 6 Sezione di Bari, INFN, Bari, Italy. 7 Department of Physics, University of Bari, Bari, Italy. 8 Sezione di Trieste, INFN, Trieste, Italy. 9 Department of Physics, University of Trieste, Trieste, Italy. 10 Ioffe Physical Technical Institute, Russian Academy of Sciences, Saint Petersburg, Russia. 11 Moscow Engineering and Physics Institute, Moscow, Russia. 12 Department of Physics, KTH, Stockholm, Sweden. 13 Oskar Klein Centre for Cosmo Particle Physics, Stockholm University, Stockholm, Sweden. 14 Sezione di Rome, INFN, Rome, Italy. 15 Department of Physics, University of Rome Tor Vergata, Rome, Italy. 16 IFAC, Florence, Italy. 17 Department of Physics, University of Siegen, Siegen, Germany. 18 Laboratori Nazionali di Frascati, INFN, Frascati, Italy. Copyright 2009 by the American Geophysical Union /09/2009JA resulting electron and positrons are confined between magnetic mirror points within the vicinity of the Earth. Depending on the primary proton energy, the cross section for p + production is 1 2 times greater than for p, and so positrons are expected to dominate. In the work of Koldashov et al. [1995], secondary fluxes are calculated also considering pair production by gamma rays from neutral pion decays and Bremsstrahlung. The effect of these mechanisms can be significant especially for low energies (up to several hundreds of MeV). [3] As the particle energy increases the influence of the East-West asymmetry grows. Quasi-trapped leptons are produced mainly by protons and helium arriving from the West, and the secondary particles move in the same direction as the primary ones. Electrons with a large Larmor radius lose their energy through scattering in the atmosphere while positrons with the same energy turn in the opposite direction, reach a higher altitude (around 500 km) and can be intercepted in an orbiting instrument. A positron excess is therefore observed. Simulations performed in the work of Derome et al. [2001], Plyaskin [2008], and Lipari [2002] elucidated the nature of particle propagation in near-earth space and included important effects due to the East-West asymmetry of the geomagnetic cutoff. Gusev et al. [1985] discuss this effect in more detail. 1of7

2 (10 days flight in 1998, inclination 51.6 and altitude km) observed secondary positrons and electrons (>80 MeV). The equatorial quasi-trapped positron flux was found to be approximately 4 times that for electrons. The magnitude of the effect decreased with latitude, and for particles with a small trapping lifetime. [6] This paper reports a measurement of the quasi-trapped e + /e flux ratio between 80 MeV and 10 GeV. Section 2 describes the PAMELA instrument, in section 3 the data analysis procedure is described, and in section 4 the results are presented and discussed. Conclusions are presented in section 5. Figure 1. Schematic overview of the PAMELA apparatus which is approximately 1.3 m high. The magnetic field lines inside the spectrometer cavity are oriented along the y direction. [4] The main conclusions of these studies have been confirmed for total (electron plus positron) secondary particle fluxes obtained by several satellite experiments during the 1970s [Grigorov, 1977]. The first separate measurements for electron and positron fluxes ( MeV) were performed by the MARIA and MARIA-2 instruments onboard SALYUT-7 (inclination 51.6, altitude about 280 km) and MIR (inclination 51.6, altitude about 390 km) space stations, respectively, between 1985 and 1997 [Voronov et al., 1991, 1992, 1995]. An excess of quasi-trapped positrons over electrons was observed. The magnitude of the positron excess was found to be location-dependent, with the e + /e flux ratio spanning the range from 1 to 2. It was shown that the e + /e flux ratio varies in near-earth space due to both the action of the geomagnetic cutoff on the primary cosmic ray spectrum and differing drift effects for electrons and positrons generated in the Earth s atmosphere and subsequently trapped by the Earth s magnetic field. [5] The AMS-01 experiment [Alcaraz et al., 2000; Fiandrini et al., 2002] onboard Space Shuttle Discovery 2. PAMELA Instrument [7] The PAMELA instrument [Picozza et al., 2007] was developed in the framework of an international collaboration between Russian, Italian, Swedish and German institutions. PAMELA was launched onboard the Resurs-DK1 satellite on 15 June 2006 and inserted into a quasi-polar (70 inclination) elliptical orbit with an altitude varying between 350 and 600 km. The large accumulated statistics resulting from a relatively large acceptance and excellent particle identification power provides new opportunities for detailed studies of quasi-trapped electrons and positrons in near-earth space. [8] The PAMELA instrument consists of the following subdetectors, as shown in Figure 1: a time-of-flight system (TOF), an anticoincidence system (CAS, CARD, CAT), a magnetic spectrometer and an electromagnetic calorimeter. A shower tail catching scintillator (S4) and a neutron detector are also present, but are not used in this work. The TOF comprises 6 layers of segmented plastic scintillators arranged in three planes (S1, S2, and S3). The TOF system provides the main trigger for data acquisition, measures the absolute value of the particle charge and the flight time for traversal of the S1, S2, and S3 planes. The acceptance is about 21.5 cm 2 sr (for a S1, S2, and S3 trigger configuration). The particle rigidity (momentum divided by charge) is determined by the magnetic spectrometer which comprises a permanent magnet (mean bending field 0.43 T) and 6 planes of double-sided silicon microstrip planes. During flight the spatial resolution of the silicon planes is observed to be 3 mm, corresponding to a maximum detectable rigidity (MDR) exceeding 1 TV. Lepton-hadron separation is provided by the calorimeter which consists of 22 plates of tungsten absorber interleaved with 44 silicon sensor planes for a total thickness of 16.3 radiation lengths. Positrons (electrons) can be selected from a background of protons (antiprotons) by considering the energy deposition and interaction topology characteristics of the event. Particles not cleanly entering the PAMELA acceptance are rejected by the anticoincidence system. The instrument is approximately 120 cm high, has a mass of about 470 kg and a power consumption of 355 W. PAMELA is located inside a pressurized and temperature controlled vessel attached to the satellite. [9] All triggered events are stored in the PAMELA memory for subsequent transmission to ground. The attitude and geographical location of the satellite and PAMELA are determined onboard and recorded approximately once a 2of7

3 second. From this information the vertical geomagnetic cutoff is determined on an event-by-event basis. 3. Data Analysis [10] A subsample of all downlinked events were selected for further analysis. The following selection criteria were applied: [11] 1. A single reconstructed track was required in the magnetic spectrometer. [12] 2. The TOF information was required to be compatible with the expectation for a down-going particle. The time-of-flight resolution of 300 ps, compared with a timeof-flight between S1 and S3 of more than 3 ns, ensures that no contamination from upgoing particles remains in the selected sample. [13] 3. Particles arising from interactions above the magnetic spectrometer were rejected by requiring that no hit was recorded by either the CARD or CAT scintillators of the AC system. [14] From the resulting sample of events, electrons and positrons were identified using information from the magnetic spectrometer and the calorimeter. In the spectrometer, ionization energy losses were required to be compatible with the expectation for a singly charged minimum ionizing particle (mip). For the energy range considered in this paper, electrons and positrons develop well contained electromagnetic showers in the calorimeter. During positron selection the misidentification of protons is the largest source of background and can occur if electron- and proton-like interaction patterns are confused in the calorimeter data. Simulations show that particle identification based on the total measured energy and the starting point of the reconstructed shower in the calorimeter can be tuned to reject 99.9% of the protons, while selecting >95% of the electrons or positrons. The remaining proton contamination in the positron sample can be eliminated using additional topological information, including the lateral and longitudinal profile of the shower. This method was described in detail by Adriani et al. [2009]. Note that levels conditions are much lower in the equatorial region due to the cutoff in the proton flux. A similar procedure was followed to reject antiprotons from the electron sample. Examples of events identified in this way are shown in Figure 2. [15] Charged pions are a second source of background and affect the selection of both electrons and positrons. This contamination was addressed in three ways: (1) Pions produced from proton interactions in the pressure vessel or in the first TOF detector (S1) are rejected by the AC system. (2) Low-rigidity pions (up to several hundreds of MeV) are almost nonrelativistic, and can be separated from electrons and positrons using TOF velocity measurements. (3) Pions are strongly interacting particles like protons, and can be rejected in the same way, i.e., using the shower starting point and lateral and longitudinal profiles reconstructed in the calorimeter. Studies of ionization energy loss distributions for selected events showed that the final pion contamination was less than 1%. [16] The PAMELA acceptance points to zenith. This allows particles with pitch angles (the angle between the particle velocity and the geomagnetic field direction) of about to be measured in the equatorial region. Since the angle between PAMELA and the geomagnetic field direction decreases with latitude, smaller pitch angles are observed for increasing latitudes. Each event recorded by PAMELA can be characterized according to the registration time, geographical coordinates and the orientation of PAMELA. This allows the McIlvain geomagnetic coordinates based on the magnitude of the geomagnetic field (B) and the magnetic shell parameter (L) determined from an integral invariant for particle motion [McIlvain, 1961] to be calculated for each event. The dipole magnetic field L shell is determined as the distance from the Earth center to a given magnetic field line evaluated at Earth radius. For a geomagnetic latitude Q the parameter L is given by 1/L = cos 2 (Q). The IGRF 05 model of the Earth s magnetic field was assumed ( [17] Geographical distributions of selected electrons and positrons are presented in Figure 3, where each point represents an event. Different L shell ranges are separated using a color code. Events in regions with B < 0.23 G are plotted in grey, and correspond to the South Atlantic Anomaly (SAA). More positrons are observed in the equatorial region (L shell < 1.2) than at middle and high latitudes. The apparent deficit of events in the center of the SAA are due to a saturation of the instrument trigger rate because of the low-energy proton flux. In this paper, the electron and positron fluxes are studied mainly in the equatorial region (L shell < 1.2). The South Atlantic Anomaly was rejected by selecting B > 0.23 G. [18] Electron and positron spectra were calculated using the formula NðEÞ FE ð Þ ¼ DTDEGðEÞ ; where N(E) is the number of particles registered in a certain energy interval DE, DT denotes the exposure time of the satellite in the region of near-earth space under consideration and G(E) the geometrical acceptance, defined as Z Z GE ð Þ ¼ W S hðe; 8; qþds cosðþdw; q where ds (dw) is an area (solid angle) element, E, (8, q p ) are the energy and incidence angles, respectively, of the triggering particle and h(e, 8, q) is the corresponding detection efficiency. The exposure of PAMELA in each region of space considered was obtained using knowledge of the satellite orbit, taking into account the dead time of the spectrometer for each registered event. The acceptance was obtained using the official simulation software of the PAMELA collaboration which is based on GEANT ( Selection efficiencies were determined from simulations tuned with periodic in-flight calibrations. 4. Results and Discussion [19] Data recorded between July and November 2006 were used to determine the quasi-trapped e + /e flux ratio between 80 MeV and 8 GeV (L shell < 1.2, B > 0.23 G). The result is presented in Figure 4. The e + /e flux ratio is clearly energy-dependent and reaches a value of 5 in the ð1þ ð2þ 3of7

4 Figure 2. (left) A positron event with energy GeV (bending view). The particle crosses the TOF system (S1, S2, and S3 detectors) and the magnetic spectrometer before finally interacting in the calorimeter. (right) An electron event with energy GeV. Note the opposing reconstructed track curvatures which allow the particle sign of charge to be determined. Figure 3. Geographical distribution of (a) secondary positrons and (b) electrons. The color scale allows different L shell values to be distinguished. Grey points are for regions with B shell < 0.23 G, i.e., the South Atlantic Anomaly. 4of7

5 Figure 4. Measurements of the positron to electron flux ratio in the equatorial region (L shell < 1.2; B shell > 0.23 G). energy range 300 to 800 MeV. The PAMELA measurements are shown together with those published by the AMS Collaboration [Fiandrini et al., 2002] for energies >150 MeV. Low-energy results from the MARIA [Voronov et al., 1992] instrument are also shown. The statistical accuracy and wide energy range of the PAMELA data set is far superior to all previously published results. [20] As discussed in the introduction, the large value for the e + /e flux ratio observed for energies from 300 to 800 MeV can be explained by an East-West asymmetry of the geomagnetic cutoff. At lower energies, the Larmor radius of particles decreases and this effect becomes less important, yielding a flux ratio for energies <100 MeV of approximately unity due to increasing role of pair production by gamma rays from neutral pion decay and Bremsstrahlung [Koldashov et al., 1995; Derome et al., 2001]. The decrease in the ratio at high energies (several GeV) is caused by two effects. The first concerns a reduction in Figure 6. The differential energy spectrum of quasitrapped electrons. The PAMELA result is compared to other measurements and theoretical models. Model 1, Koldashov et al. [1995]; model 2, Derome et al. [2001]. the East-West asymmetry for high-energy protons that can produce electrons and positrons of energy equal to several GeV. The second cause is because at the equator the vertical cutoff rigidity is about GeV. In the energy region from several GeV up to vertical cutoff the so-called penumbra produces an increase in contamination from cosmic ray electrons and the e + /e flux ratio therefore decreases. [21] In Figure 5 the behavior of the e + /e flux ratio for different geomagnetic latitudes is presented. The magnitude of the flux ratio can be seen to decrease at high latitudes. It is shown clearly by Derome et al. [2001] that at high latitudes the East-West asymmetry is much weaker, so the electron and positron fluxes are about equal. [22] Differential energy spectra for quasi-trapped positrons and electrons are shown in Figures 6 and 7, respec- Figure 5. PAMELA measurements of the positron to electron flux ratio in the equatorial region (L shell < 1.2; B shell > 0.23 G) for different geomagnetic latitudes. Figure 7. The differential energy spectrum of quasitrapped positrons. The PAMELA result is compared to other measurements and theoretical models. Model 1, Koldashov et al. [1995]; model 2, Derome et al. [2001]. 5of7

6 Figure 8. The differential energy spectra of quasi-trapped electrons for a range of geomagnetic latitudes. tively. Measurements obtained by the MARIA and AMS instruments are also shown. At low energies (<0.5 GeV) the electron and positron fluxes measured by PAMELA are lower than those reported by AMS. This is thought to be due to the anisotropy of secondary lepton fluxes in this energy range combined with the larger acceptance of AMS which allows particles with large zenith angles to be registered. Predictions from Koldashov et al. [1995] (model 1) and Derome et al. [2001] (model 2) are also illustrated in Figures 6 and 7. The energy dependence of the spectra is not well reproduced, especially for positrons (Figure 7) where experimental data of PAMELA and AMS are systematically higher than the models. The precise results obtained by PAMELA can be used to further improve these models. [23] The latitude dependence of the electron and positron differential spectra was studied. The results are presented in Figures 8 and 9. An increasing contamination of cosmic ray electrons is evident especially for L1.4, where the value of vertical cutoff rigidity is 7.6 GeV. Spectra slopes also vary. Both the electron and positron spectra soften at high geomagnetic latitudes due to a decrease in the particle Figure 10. The latitudinal dependencies of electron and positron fluxes for particle energy 0.1 GeV. quasi-trapping limit [Grigorov, 1977]. Detailed dependencies of electron and positron fluxes on geomagnetic latitudes for two energies (0.1 GeV and 0.85 GeV) are presented in Figures 10 and 11. Note a different behavior of the electron and positron spectra for low energies (about 100 MeV). The electron flux becomes less with latitudes, while the positron flux does not change significantly. For higher energies both electron and positron fluxes decrease with latitudes. Probably this is due to a combination of the East-West asymmetry of the geomagnetic cutoff, forward peaking of the production cross section and atmospheric absorption of the produced leptons [Derome et al., 2001]. 5. Summary and Conclusions [24] The results presented in this paper show that the quasi-trapped electron and positron fluxes have a complex spatial structure caused by the Earth s geomagnetic field, the energy dependence of production cross sections and the atmospheric absorption of produced leptons. In spite of the fact that secondary particle generation and propagation processes are well known, nowadays experimental spectra Figure 9. The differential energy spectra of quasi-trapped positrons for a range of geomagnetic latitudes. Figure 11. The latitudinal dependencies of electron and positron fluxes for particle energy 0.85 GeV. 6of7

7 are not well reproduced by theoretical models, so the precision data set collected by PAMELA will allow empirical models of secondary particle production in near-earth space to be significantly improved. [25] Acknowledgments. We acknowledge support from the Russian Space Agency (Roscosmos), the Russian Foundation for Basic Research (grant a), the Italian Space Agency (ASI), Deutsches Zentrum für Luft- und Raumfahrt (DLR), the Swedish National Space Board, and the Swedish Research Council. [26] Zuyin Pu thanks Bernd Heber and another reviewer for their assistance in evaluating this paper. References Adriani, O., et al. (2009), An anomalous positron abundance in cosmic rays with energies GeV, Nature, 458, 607. Alcaraz, J., et al. (2000), Leptons in near-earth orbit, Phys. Lett. B, 484, 10. Derome, L., M. Buenerd, and Y. Liu (2001), Secondary electrons and positrons in near-earth orbit, Phys. Lett. B, 515, 1. Fiandrini, E., G. Esposito, B. Bertucci, B. Alpat, R. Battiston, W. J. Burger, G. Lamanna, and P. Zuccon (2002), Leptons with E > 200 MeV trapped in the Earth s radiation belt, J. Geophys. Res., 107(A6), 1067, doi: /2001ja Grigorov, N. L. (1977), On the possibility of the existence of a radiation belt formed by electrons with energies of 100 MeV and higher, Dokl. Acad. Sci. USSR, Earth Sci. Sect., Engl. Transl., 236, 810. Gusev, A. A., I. A. Efimov, K. Kudela, G. I. Pugacheva, and L. Iust (1985), The spatial distribution of albedo particles at altitudes of 500 km, Geomagn. Aeron., 25(4), 462. Koldashov, S. V., V. V. Mikhailov, and S. A. Voronov (1995), Electron and positron albedo spectra with energy more than 10 MeV, in International Cosmic Ray Conference 24th, Rome, vol. 4, pp , Int. Union of Pure and Appl. Phys., Rome. Lipari, P. (2002), The fluxes of sub-cutoff particles, detected by ams, cosmic ray albedo and athmospheric neutrinos, Astropart. Phys., 16, 295. McIlvain, C. E. (1961), Coordinates for mapping the disribution of magnetically trapped particles, J. Geophys. Res., 66, Picozza, P., et al. (2007), PAMELA: A payload antimatter matter exploration and light-nuclei astrophysics, Astropart. Phys., 27, 296. Plyaskin, V. (2008), Mapping Earth s radiation belts using data from STS91 mission of AMS, Astropart. Phys., 30, 18. Voronov, S. A., A. M. Galper, S. V. Koldashov, L. V. Maslennikov, V. V. Mikhailov, and A. V. Popov (1991), Energetic spectra of high energy electrons and positrons below the Earth s radiation belt, Cosmic Res., Engl. Transl., 33(5), 567. Voronov, S. A., A. M. Galper, S. V. Koldashov, L. V. Maslennikov, V. V. Mikhailov, and A. V. Popov (1992), Spatial distributions of high-energy electrons and positrons below the Earth s radiation belt, Cosmic Res., Engl. Transl., 34(1), 140. Voronov, S. A., S. V. Koldashov, and V. V. Mikhailov (1995), Spectra of albedo electrons and positrons with energy greater than 20 MeV, Cosmic Res., Engl. Transl., 33(3), 329. O. Adriani, L. Bonechi, M. Bongi, S. Bottai, N. Mori, P. Papini, S. B. Ricciarini, P. Spillantini, and E. Vannuccini, Department of Physics, University of Florence, I Sesto Fiorentino, Florence, Italy. G. Barbarino, D. Campana, R. Carbone, L. Consiglio, and G. Osteria, Department of Physics, University of Naples Federico II, I Naples, Italy. G. A. Bazilevskaya, A. N. Kvashnin, and Y. I. Stozhkov, Lebedev Physical Institute, Leninsky Prospekt 53, RU Moscow, Russia. R. Bellotti, A. Bruno, F. S. Cafagna, and A. Monaco, Department of Physics, University of Bari, I Bari, Italy. M. Boezio, V. Bonvicini, G. Jerse, E. Mocchiutti, C. Pizzolotto, S. Ritabrata, A. Vacchi, G. Zampa, and N. Zampa, Department of Physics, University of Trieste, I Trieste, Italy. E. A. Bogomolov, S. Y. Krutkov, N. N. Nikonov, and G. I. Vasilyev, Ioffe Physical Technical Institute, Russian Academy of Sciences, RU Saint Petersburg, Russia. S. V. Borisov, A. M. Galper, L. A. Grishantseva, A. V. Karelin, S. V. Koldashov, A. A. Leonov, V. V. Malakhov, A. G. Mayorov, V. V. Mikhailov, M. F. Runtso, S. A. Voronov, Y. T. Yurkin, and V. G. Zverev, Moscow Engineering and Physics Institute, RU Moscow, Russia. (lagrishantseva@mephi.ru) P. Carlson, W. Gillard, P. Hofverberg, M. Pearce, L. Rossetto, and J. Wu, Department of Physics, KTH, Stockholm University, SE Stockholm, Sweden. M. Casolino, M. P. De Pascale, C. De Santis, N. De Simone, V. Di Felice, V. Malvezzi, L. Marcelli, P. Picozza, and R. Sparvoli, Department of Physics, University of Rome Tor Vergata, I Rome, Italy. G. Castellini, IFAC, I Sesto Fiorentino, Florence, Italy. W. Menn and M. Simon, Department of Physics, Universitaet Siegen, D Siegen, Germany. M. Ricci, Laboratori Nazionali di Frascati, INFN, 1 Via Enrico Fermi 40, I Frascati, Italy. 7of7

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