Muon-induced background in the KATRIN main spectrometer

Altenmüller, K.; Arenz, M.; Baek, W.-J.; Beck, M.; Beglarian, A.; Behrens, J.; Bergmann, T.; Berlëv, A. I.; Besserer, U.; Blaum, Klaus; Bobien, S.; Bode, T.; Bornschein, B.; Bornschein, L.; Brunst, T.; Buzinsky, N.; Chilingaryan, S.; Choi, W.; Deffert, M.; Doe, P. J.; Dragoun, O.; Drexlin, G.; Dyba, S.; Edzards, F.; Eitel, K.; Ellinger, Enrico; Engel, R.; Enomoto, S.; Erhard, M.; Eversheim, D.; Fedkevych, M.; Formaggio, J. A.; Fränkle, F. M.; Franklin, G.; Friedel, F.; Fulst, A.; Gil, W.; Glück, F.; Ureña, A. Gonzalez; Grohmann, Steffen; Größle, Robin; Gumbsheimer, R.; Hackenjos, M.; Hannen, V.; Harms, F.; Haußmann, N.; Heizmann, F.; Helbing, K.; Herz, Werner; Hickford, S.; Hilk, D.; Hillesheimer, D.; Howe, M. A.; Huber, A.; Jansen, A.; Kellerer, J.; Kernert, N.; Kippenbrock, L.; Kleesiek, M.; Klein, Manuel; Kopmann, A.; Korzeczek, M.; Kovalı́k, A.; Krasch, B.; Kraus, M.; Kuckert, L.; Lasserre, T.; Lebeda, O.; Leiber, B.; Letnev, J.; Linek, J.; Lokhov, Alexey; Machatschek, M.; Marsteller, A.; Martín, E. L.; Mertens, S.; Mirz, Sebastian; Monreal, B.; Neumann, H.; Niemes, S.; Off, A.; Osipowicz, A.; Otten, E.; Parno, D. S.; Pollithy, A.; Poon, A. W. P.; Priester, F.; Ranitzsch, P. C.-O.; Rest, O.; Rink, R.; Robertson, R. G. H.; Roccati, F.; Rodenbeck, C.; Röllig, M.; Röttele, C.; Rovedo, P.; Ryšavý, M.; Sack, R.; Sáenz, Alejandro; Schimpf, L.; Schlösser, K.; Schlösser, M.; Schönung, K.; Schrank, M.; Seitz-Moskaliuk, H.; Sentkerestiová, J.; Sibille, V.; Slezák, M.; Steidl, M.; Steinbrink, N.; Sturm, M.; Suchopar, M.; Suesser, M.; Telle, Helmut H.; Thorne, L. A.; Thümmler, T.; Titov, N.; Tkachev, I.; Trost, N.; Valerius, K.; Vénos, D.; Vianden, R.; Hernández, A. P. Vizcaya; Wandkowsky, N.; Weber, M.; Weinheimer, C.; Weiss, C.; Welte, S.; Wendel, J.; Wilkerson, J. F.; Wolf, J.; Wüstling, S.; Zadoroghny, S.; Zeller, G. P.

doi:10.1016/j.astropartphys.2019.01.003

Cited by 19 publications

(19 citation statements)

References 36 publications

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“…Up to now, source-related backgrounds have not been observed, so that spectrometerrelated processes [39] dominate R bg apart from a small detector-related contribution [32]. Electrons generated at the spectrometer surface by cosmic muons and environmental gamma rays are inhibited from entering the inner flux tube by magnetic and electric barriers [40,41]. Thus, R bg originates from excited or unstable neutral atoms which can propagate freely in the UHVenvironment.…”

mentioning

confidence: 99%

Improved Upper Limit on the Neutrino Mass from a Direct Kinematic Method by KATRIN

Aker¹,

Altenmüller²,

Arenz³

et al. 2019

Phys. Rev. Lett.

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477

431

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mentioning

confidence: 99%

Improved Upper Limit on the Neutrino Mass from a Direct Kinematic Method by KATRIN

Aker¹,

Altenmüller²,

Arenz³

et al. 2019

Phys. Rev. Lett.

Self Cite

477

431

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“…The surface, however, is efficiently shielded by the approximately axisymmetric magnetic field and by the wire electrode system of the spectrometer. The lower limit for the suppression factor of the shielding is about 10 4 [18]. Assuming again that 10 8 electron-ion pairs are generated for each primary trapped electron and further assuming that each ion knocks out 10 electrons at the surface, there could be up to 10 5 electrons reaching the detector per primary trapped electron by this process.…”

Section: Inter-spectrometer Penning Trap Problem and Countermeasuresmentioning

confidence: 99%

Suppression of Penning discharges between the KATRIN spectrometers

et al. 2020

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The KArlsruhe TRItium Neutrino experiment (KATRIN) aims to determine the effective electron (anti)neutrino mass with a sensitivity of 0.2eV/c 2 by precisely measuring the endpoint region of the tritium β-decay spectrum. It uses a tandem of electrostatic spectrometers working as magnetic adiabatic collimation combined with an electrostatic (MAC-E) filters. In the space between the prespectrometer and the main spectrometer, creating a Penning trap is unavoidable when the superconducting magnet between the two spectrometers, biased at their respective nominal potentials, is energized. The electrons accumulated in this trap can lead to discharges, which create additional background electrons and endanger the spectrometer and detector section downstream. To counteract this problem, "electron catchers" were installed in the beamline inside the magnet bore between the two spectrometers. These catchers can be moved across the magnetic-flux tube and intercept on a sub-ms time scale the stored electrons along their magnetron motion paths. In this paper, we report on the design and the successful commissioning of the electron catchers and present results on their efficiency in reducing the experimental background.

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“…The energy spectrum for true-secondary electrons is treated independently of the primary particle energy; the shape of the spectrum is known not to vary significantly with respect to the incident photon energy [34,35]. The validity of these assumptions on the electrons' initial properties was shown in the context of the background analysis of cosmic-ray muons [7]. Using the 60 Co measurement, one finds Y= 3×10 −4 e − /γ.…”

Section: Secondary Electron Yieldmentioning

confidence: 99%

“…Background electrons produced in the main spectrometer (MS), the high-resolution MAC-E filter [4][5][6] that analyzes the energy of the β-particles, are of particular importance. Several sources of background in the MS have already been analyzed in detail, including cosmicray muons [7] and radon decays [8].…”

Section: Introductionmentioning

confidence: 99%