Observation of the cosmic-ray shadow of the Moon with IceCube

Aartsen, M. G.; Abbasi, Rasha; Abdou, Y.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Altmann, D.; Auffenberg, J.; Bai, X.; Baker, M. D.; Barwick, S. W.; Baum, V.; Bay, R.; Beatty, J. J.; Bechet, S.; Tjus, J. Becker; Becker, K.-H.; Bell, Michael; Benabderrahmane, M. L.; BenZvi, S.; Berdermann, Jens; Berghaus, P.; Berley, D.; Bernardini, E.; Bernhard, A.; Bertrand, Daniel; Besson, D.; Binder, G.; Bindig, D.; Bissok, M.; Blaufuss, E.; Blumenthal, J.; Boersma, D. J.; Bohaichuk, S.; Böhm, C.; Bose, D.; Böser, S.; Botner, O.; Brayeur, L.; Bretz, H.-P.; Brown, A. M.; Bruijn, R.; Brünner, J.; Carson, M.; Casey, J.; Casier, M.; Chirkin, D.; Christov, A.; Christy, B.; Clark, K.; Clevermann, F.; Coenders, S.; Cohen, S.; Cowen, D. F.; Silva, A. H. Cruz; Danninger, M.; Daughhetee, J.; Davis, J.; Clercq, C. De; Ridder, S. De; Desiati, P.; DeYoung, T.; Díaz-Vélez, J. C.; Dunkman, M.; Eagan, R.; Eberhardt, B.; Eisch, J.; Ellsworth, R. W.; Euler, S.; Evenson, P. A.; Fadiran, O.; Fazely, A. R.; Fedynitch, Anatoli; Feintzeig, J.; Feusels, T.; Filimonov, K.; Finley, C.; Fischer-Wasels, T.; Flis, S.; Franckowiak, A.; Franke, Robert; Frantzen, K.; Fuchs, T.; Gaisser, T. K.; Gallagher, John S.; Gerhardt, L.; Gladstone, L.; Glüsenkamp, T.; Goldschmidt, A.; Golup, G.; González, J. G.; Goodman, J. A.; Góra, D.; Grandmont, D. T.; Grant, D.; Groß, A.; Ha, C.; Ismail, A. Haj; Hallen, P.; Hallgren, A.; Halzen, F.; Hanson, K.; Heereman, D.; Heinen, D.; Helbing, K.; Hellauer, R.; Hickford, S.; Hill, G. C.; Hoffman, K. D.; Hoffmann, R.; Homeier, A.; Hoshina, K.; Huelsnitz, W.; Hulth, P. O.; Hultqvist, K.; Hussain, Shahid; Ishihara, A.; Jacobi, E.; Jacobsen, J.; Jagielski, K.; Japaridze, G. S.; Jero, K.; Jlelati, O.; Kaminsky, B.; Kappes, A.; Karg, T.; Karle, A.; Kelley, J. L.; Kiryluk, J.; Kislat, Fabian; Kläs, J.; Klein, S. R.; Köhne, J. H.; Kohnen, G.; Kolanoski, H.; Köpke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Kowalski, M.; Krasberg, M.; Krings, K.; Kroll, G.; Kunnen, J.; Kurahashi, N.; Kuwabara, T.; Labare, M.; Landsman, H.; Larson, M. J.; Lesiak-Bzdak, M.; Leuermann, M.; Leute, J.; Lünemann, J.; Madsen, J.; Maruyama, R.; Mase, K.; Matis, H. S.; McNally, F.; Meagher, K.; Merck, M.; Mészáros, P.; Meures, T.; Miarecki, S.; Middell, E.; Milke, N.; Miller, J.; Mohrmann, L.; Montaruli, T.; Morse, R.; Nahnhauer, R.; Naumann, Uwe; Niederhausen, H.; Nowicki, S. C.; Nygren, D. R.; Obertacke, A.; Odrowski, S.; Olivas, A.; Olivo, M.; O’Murchadha, A.; Paul, Larissa; Pepper, J. A.; Heros, C. Pérez de los; Pfendner, C.; Pieloth, D.; Pinat, E.; Pirk, Norbert; Posselt, J.; Price, P. B.; Przybylski, G. T.; Rädel, L.; Rameez, M.; Rawlins, K.; Redl, P.; Reimann, R.; Resconi, E.; Rhode, W.; Ribordy, M.; Richman, M.; Riedel, Benedikt; Rodrigues, J. P.; Rott, C.; Ruhe, T.; Ruzybayev, B.; Ryckbosch, D.; Saba, S. M.; Salameh, T.; Sander, H. G.; Santander, M.; Sarkar, S.; Schatto, K.; Scheel, Mark A.; Scheriau, F.; Schmidt, T.; Schmitz, M.; Schoenen, S.; Schöneberg, S.; Schönwald, A.; Schukraft, A.; Schulte, L.; Schulz, O.; Seckel, D.; Sestayo, Y.; Seunarine, S.; Sheremata, C.; Smith, M. W. E.; Soldin, D.; Spiczak, G. M.; Spiering, C.; Stamatikos, M.; Stanev, T.; Stasik, A.; Stezelberger, T.; Stokstad, R. G.; Stößl, A.; Strahler, E. A.; Strom, Lars Rickard; Sullivan, G. W.; Taavola, H.; Taboada, I.; Tamburro, A.; Tepe, A.; Ter–Antonyan, S.; Tešić, G.; Tilav, S.; Toale, P. A.; Toscano, S.; Usner, M.; Drift, D. van der; Eijndhoven, N. van; Overloop, A. Van; Santen, J. V.; Vehring, M.; Vöge, M.; Vraeghe, M.; Walck, C.; Waldenmaier, T.; Wallraff, M.; Wasserman, R.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.; Wiebe, K.; Wiebusch, C. H.; Williams, D. R.; Wissing, H.; Wolf, M.; Wood, T. R.; Woschnagg, K.; Xu, C.; Xu, D. L.; Xu, X. W.; Yañez, J. P.; Yodh, G.; Yoshida, Shigeru; Zarzhitsky, P.; Ziemann, J.; Zierke, S.; Zoll, M.

doi:10.1103/physrevd.89.102004

Cited by 46 publications

(41 citation statements)

References 25 publications

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“…Compared with the Single Photo-Electron (SPE) fit, which only uses the arrival time of the first photon in each DOM, the MPE fit yields a slightly better angular resolution in highenergy range, indicated by simulation studies (Aartsen et al, 2014).…”

Section: Data Samplementioning

confidence: 99%

“…The trigger rate is dominated by muons produced by cosmic-rays interacting with the Earth's atmosphere. A deficit of cosmic-rays from the direction of the Moon and Sun is expected and was observed for the Moon in Aartsen et al (2014) with greater than 6σ .…”

Section: Introductionmentioning

confidence: 99%

“…For the detector configuration with 40 and 59 strings (IC40 and IC59) a Moon shadow analysis was done in Aartsen et al (2014). This work makes use of the data taken from detector configurations with 79 and 86 strings (IC79 and IC86-I).…”

Section: Data Samplementioning

confidence: 99%

“…A data selection for the IC40 and IC59 detector configuration is described in Aartsen et al (2014). At the South Pole Moon and Sun filters are enabled if the celestial body is at least 15 • above the horizon (Aartsen et al, 2014). The Moon reaches this threshold for at least 6 days each month.…”

Section: Data Samplementioning

confidence: 99%

“…Moreover, the second year (IC86-II) in which the detector was operating in its final configurations has been analyzed. A data selection for the IC40 and IC59 detector configuration is described in Aartsen et al (2014). At the South Pole Moon and Sun filters are enabled if the celestial body is at least 15 • above the horizon (Aartsen et al, 2014).…”

Section: Data Samplementioning

confidence: 99%

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Observation of the Cosmic-Ray Shadow of the Moon and Sun with IceCube

et al. 2015

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Abstract. Moon shadow analyses are standard methods to calibrate cosmic-ray detectors. We report on a threeyear observation of cosmic-ray Moon and Sun shadows in different detector configurations. The cosmic-ray Moon shadow was observed with high statistical significance ( > 6σ ) in previous analyses when the IceCube detector operated in a smaller configuration before it was completed in December 2010. This work shows first analyses of the cosmic-ray Sun shadow in IceCube. A binned analysis in one-dimension is used to measure the Moon and Sun shadow with high statistical significance greater than 12σ .

show abstract

Section: Data Samplementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Data Samplementioning

confidence: 99%

Section: Data Samplementioning

confidence: 99%

Section: Data Samplementioning

confidence: 99%

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Observation of the Cosmic-Ray Shadow of the Moon and Sun with IceCube

et al. 2015

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Investigation on the cosmic-ray shadow of planets and asteroids

Zhang

Huang

et al. 2022

Exp Astron

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The moon shadow and sun shadow of cosmic rays are commonly used to calibrate the angular resolution of the instrument in extensive air shower experiments, measure the proton-antiproton ratio, and study the interplanetary magnetic field (IMF). The shadow effect of planets and asteroids in the solar system, on the other hand, has received little attention. If considerable shadow effects can be observed, a novel approach may be developed to calibrate the point spread function and investigate the IMF. In this work, we calculate the sensitivity of observing the shadow effects of planets and asteroids in the next hundred years using LHAASO's instrumental response as an example. The result shows that the blocking impact of these celestial bodies is minimal; thus, their influence on the direction distribution of cosmic rays is negligible.

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Characterization of the atmospheric muon flux in IceCube

Aartsen¹,

Abraham²,

Ackermann³

et al. 2016

Astroparticle Physics

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101

117

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Muons produced in atmospheric cosmic ray showers account for the by far dominant part of the event yield in large-volume underground particle detectors. The IceCube detector, with an instrumented volume of about a cubic kilometer, has the potential to conduct unique investigations on atmospheric muons by exploiting the large collection area and the possibility to track particles over a long distance. Through detailed reconstruction of energy deposition along the tracks, the characteristics of muon bundles can be quantified, and individual particles of exceptionally high energy identified. The data can then be used to constrain the cosmic ray primary flux and the contribution to atmospheric lepton fluxes from prompt decays of short-lived hadrons.In this paper, techniques for the extraction of physical measurements from atmospheric muon events are described and first results are presented. The multiplicity spectrum of TeV muons in cosmic ray air showers for primaries in the energy range from the knee to the ankle is derived and found to be consistent with recent results from surface detectors. The single muon energy spectrum is determined up to PeV energies and shows a clear indication for the 2 emergence of a distinct spectral component from prompt decays of short-lived hadrons. The magnitude of the prompt flux, which should include a substantial contribution from light vector meson di-muon decays, is consistent with current theoretical predictions.The variety of measurements and high event statistics can also be exploited for the evaluation of systematic effects. In the course of this study, internal inconsistencies in the zenith angle distribution of events were found which indicate the presence of an unexplained effect outside the currently applied range of detector systematics. The underlying cause could be related to the hadronic interaction models used to describe muon production in air showers.

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Observation of the cosmic-ray shadow of the Moon with IceCube

Cited by 46 publications

References 25 publications

Observation of the Cosmic-Ray Shadow of the Moon and Sun with IceCube

Observation of the Cosmic-Ray Shadow of the Moon and Sun with IceCube

Investigation on the cosmic-ray shadow of planets and asteroids

Characterization of the atmospheric muon flux in IceCube

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