IceCube-Gen2: A Vision for the Future of Neutrino Astronomy in Antarctica

Aartsen, M. G.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Ahrens, M.; Altmann, D.; Anderson, T.; Anton, G.; Arguelles, C.; Arlen, T. C.; Auffenberg, J.; Axani, S.; Bai, X.; Bartos, I.; Barwick, S. W.; Baum, V.; Bay, R.; Beatty, J. J.; Tjus, J. Becker; Becker, K. -H.; BenZvi, S.; Berghaus, P.; Berley, D.; Bernardini, E.; Bernhard, A.; Besson, D. Z.; Binder, G.; Bindig, D.; Bissok, M.; Blaufuss, E.; Blumenthal, J.; Boersma, D. J.; Bohm, C.; Bos, F.; Bose, D.; Böser, S.; Botner, O.; Brayeur, L.; Bretz, H. -P.; Brown, A. M.; Buzinsky, N.; Casey, J.; Casier, M.; Cheung, E.; Chirkin, D.; Christov, A.; Christy, B.; Clark, K.; Classen, L.; Clevermann, F.; Coenders, S.; Collin, G. H.; Conrad, J. M.; Cowen, D. F.; Silva, A. H. Cruz; Daughhetee, J.; Davis, J. C.; Day, M.; de André, J. P. A. M.; De Clercq, C.; De Ridder, S.; Desiati, P.; de Vries, K. D.; de With, M.; DeYoung, T.; andaz-Vélez, J. C. Dí; Dunkman, M.; Eagan, R.; Eberhardt, B.; Ehrhardt, T.; Eichmann, B.; Eisch, J.; Euler, S.; Evans, J. J.; Evenson, P. A.; Fadiran, O.; Fazely, A. R.; Fedynitch, A.; Feintzeig, J.; Felde, J.; Filimonov, K.; Finley, C.; Fischer-Wasels, T.; Flis, S.; Frantzen, K.; Fuchs, T.; Gaisser, T. K.; Gaior, R.; Gallagher, J.; Gerhardt, L.; Gier, D.; Gladstone, L.; Glüsenkamp, T.; Goldschmidt, A.; Golup, G.; Gonzalez, J. G.; Goodman, J. A.; Góra, D.; Grant, D.; Gretskov, P.; Groh, J. C.; Groß, A.; Ha, C.; Haack, C.; Ismail, A. Haj; Hallen, P.; Hallgren, A.; Halzen, F.; Hanson, K.; Haugen, J.; Hebecker, D.; Heereman, D.; Heinen, D.; Helbing, K.; Hellauer, R.; Hellwig, D.; Hickford, S.; Hignight, J.; Hill, G. C.; Hoffman, K. D.; Hoffmann, R.; Homeier, A.; Hoshina, K.; Huang, F.; Huelsnitz, W.; Hulth, P. O.; Hultqvist, K.; Ishihara, A.; Jacobi, E.; Jacobsen, J.; Japaridze, G. S.; Jero, K.; Jlelati, O.; Jones, B. J. P.; Jurkovic, M.; Kalekin, O.; Kappes, A.; Karg, T.; Karle, A.; Katori, T.; Katz, U. F.; Kauer, M.; Keivani, A.; Kelley, J. L.; Kheirandish, A.; Kiryluk, J.; Kläs, J.; Klein, S. R.; Köhne, J. -H.; Kohnen, G.; Kolanoski, H.; Koob, A.; Köpke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Kowalski, M.; Krauss, C. B.; Kriesten, A.; Krings, K.; Kroll, G.; Kroll, M.; Kunnen, J.; Kurahashi, N.; Kuwabara, T.; Labare, M.; Lanfranchi, J. L.; Larsen, D. T.; Larson, M. J.; Lesiak-Bzdak, M.; Leuermann, M.; LoSecco, J.; Lünemann, J.; Madsen, J.; Maggi, G.; Mahn, K. B. M.; Marka, S.; Marka, Z.; Maruyama, R.; Mase, K.; Matis, H. S.; Maunu, R.; McNally, F.; Meagher, K.; Medici, M.; Meli, A.; Meures, T.; Miarecki, S.; Middell, E.; Middlemas, E.; Milke, N.; Miller, J.; Mohrmann, L.; Montaruli, T.; Moore, R. W.; Morse, R.; Nahnhauer, R.; Naumann, U.; Niederhausen, H.; Nowicki, S. C.; Nygren, D. R.; Obertacke, A.; Odrowski, S.; Olivas, A.; Omairat, A.; O'Murchadha, A.; Palczewski, T.; Paul, L.; Penek, Ö.; Pepper, J. A.; Heros, C. Pérez de los; Pfendner, C.; Pieloth, D.; Pinat, E.; Pinfold, J. L.; Posselt, J.; Price, P. B.; Przybylski, G. T.; Pütz, J.; Quinnan, M.; Rädel, L.; Rameez, M.; Rawlins, K.; Redl, P.; Rees, I.; Reimann, R.; Relich, M.; Resconi, E.; Rhode, W.; Richman, M.; Riedel, B.; Robertson, S.; Rodrigues, J. P.; Rongen, M.; Rott, C.; Ruhe, T.; Ruzybayev, B.; Ryckbosch, D.; Saba, S. M.; Sander, H. -G.; Sandroos, J.; Sandstrom, P.; Santander, M.; Sarkar, S.; Schatto, K.; Scheriau, F.; Schmidt, T.; Schmitz, M.; Schoenen, S.; Schöneberg, S.; Schönwald, A.; Schukraft, A.; Schulte, L.; Schulz, O.; Seckel, D.; Sestayo, Y.; Seunarine, S.; Shaevitz, M. H.; Shanidze, R.; Smith, M. W. E.; Soldin, D.; Söldner-Rembold, S.; Spiczak, G. M.; Spiering, C.; Stamatikos, M.; Stanev, T.; Stanisha, N. A.; Stasik, A.; Stezelberger, T.; Stokstad, R. G.; andl, A. Stöß; Strahler, E. A.; Ström, R.; Strotjohann, N. L.; Sullivan, G. W.; Taavola, H.; Taboada, I.; Taketa, A.; Tamburro, A.; Tanaka, H. K. M.; Tepe, A.; Ter-Antonyan, S.; Terliuk, A.; Teš, G.; Tilav, S.; Toale, P. A.; Tobin, M. N.; Tosi, D.; Tselengidou, M.; Unger, E.; Usner, M.; Vallecorsa, S.; van Eijndhoven, N.; Vandenbroucke, J.; van Santen, J.; Vanheule, S.; Vehring, M.; Voge, M.; Vraeghe, M.; Walck, C.; Wallraff, M.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whelan, B. J.; Whitehorn, N.; Wichary, C.; Wiebe, K.; Wiebusch, C. H.; Williams, D. R.; Wissing, H.; Wolf, M.; Wood, T. R.; Woschnagg, K.; Wren, S.; Xu, D. L.; Xu, X. W.; Xu, Y.; Yanez, J. P.; Yodh, G.; Yoshida, S.; Zarzhitsky, P.; Ziemann, J.; Zoll, M.

doi:10.48550/arxiv.1412.5106

Cited by 159 publications

(222 citation statements)

References 146 publications

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“…Although we would ideally incorporate early pulses for CC and NC background rejection, there are several technical challenges that this can pose, including full resimulations of the MC sets that include systematic uncertainties of the hadronic interaction models. Such studies are under way, and inclusion of this information will be especially important for IceCube-Gen2 [21], which, owing to its much larger effective area, will record many more events at the Glashow resonance.…”

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confidence: 99%

“…already inconsistent with the result presented here because such sources produce no electron antineutrinos. With just one event, pp source models cannot be constrained, but the planned IceCube Gen2 experiment [21] will increase the instrumented volume by an order of magnitude. The statistics collected by such a detector should allow us to differentiate between pp and idealized pγ models at a high significance level.…”

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confidence: 99%

See 1 more Smart Citation

Detection of a particle shower at the Glashow resonance with IceCube

Aartsen¹,

Abbasi²,

Ackermann³

et al. 2021

Nature

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139

107

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The Glashow resonance describes the resonant formation of a W − boson during the interaction of a highenergy electron antineutrino with an electron [1], peaking at an antineutrino energy of 6.3 petaelectronvolts (PeV) in the rest frame of the electron. Whereas this energy scale is out of reach for currently operating and future planned particle accelerators, natural astrophysical phenomena are expected to produce antineutrinos with energies beyond the PeV scale. Here we report the detection by the IceCube neutrino observatory of a cascade of high-energy particles (a particle shower) consistent with being created at the Glashow resonance. A shower with an energy of 6.05 ± 0.72 PeV (determined from Cherenkov radiation in the Antarctic Ice Sheet) was measured. Features consistent with the production of secondary muons in the particle shower indicate the hadronic decay of a resonant W − boson, confirm that the source is astrophysical and provide improved directional localization. The evidence of the Glashow resonance suggests the presence of electron antineutrinos in the astrophysical flux, while also providing further validation of the standard model of particle physics. Its unique signature indicates a method of distinguishing neutrinos from antineutrinos, thus providing a way to identify astronomical accelerators that produce neutrinos via hadronuclear or photohadronic interactions, with or without strong magnetic fields. As such, knowledge of both the flavour (that is, electron, muon or tau neutrinos) and charge (neutrino or antineutrino) will facilitate the advancement of neutrino astronomy.

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mentioning

confidence: 99%

mentioning

confidence: 99%

Detection of a particle shower at the Glashow resonance with IceCube

Aartsen¹,

Abbasi²,

Ackermann³

et al. 2021

Nature

Self Cite

139

107

View full text Add to dashboard Cite

show abstract

“…At energies 1 TeV, atmospheric backgrounds are negligible, though the IceCube flux is much smaller, so that multiple events are unlikely at present. IceCube-Gen2 is proposed to be an order of magnitude larger than IceCube, though with string spacing aimed more at the > ∼ 10 TeV range [138]. Scaling our > ∼ 10 TeV shower rate from §III by a factor of 10, the burst rates would somewhat exceed those in Fig.…”

Section: Discussionmentioning

confidence: 90%

Peeking into the Origins of IceCube Neutrinos: I. Buried Transient TeV Miniburst Rates

Kistler,

Yuksel

2017

Preprint

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Any interpretation of the astrophysical neutrinos discovered by IceCube must accommodate a variety of multimessenger constraints. We address implications of these neutrinos being produced in transient sources, principally if buried within supernovae so that gamma rays are absorbed by the star. This would alleviate tension with the isotropic Fermi GeV background that > ∼ 10 TeV neutrinos rival in detected energy flux. We find that IceCube data constrain transient properties, implying buried GeV-TeV electromagnetic emission near or exceeding canonical SN explosion energies of ∼ 10 51 erg, indicative of an origin within superluminous SNe. TeV neutrino bursts with dozens of IceCube events -which would be of great use for understanding r-process nucleosynthesis and more -may be just around the corner if they are a primary component of the flux.

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“…With the advent of higher-precision neutrino measurements [68], it will be necessary to account for nuclear effects in cross section and tomography measurements. This need will only increase in larger, next-generation neutrino observatories [69][70][71]. The introduction of large (order 100 km 3 ) radio-pulse-based neutrino telescopes, with energy thresholds above 10 7 GeV will also open the door to cross section measurements at higher energies [67,72], provided that good angular resolution is achieved for near-horizontal events.…”

Section: Discussionmentioning

confidence: 99%

Nuclear effects in high-energy neutrino interactions

Klein,

Robertson,

Vogt

2020

Preprint

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Neutrino telescopes like IceCube, KM3NeT and Baikal-GVD offer physicists the opportunity to study neutrinos with energies far beyond the reach of terrestrial accelerators. These neutrinos are used to study high-energy neutrino interactions and to probe the Earth through absorption tomography. Current studies of TeV neutrinos use cross sections which are calculated for free nucleons with targets which are assumed to contain equal numbers of protons and neutrons.Here we consider modifications of high-energy neutrino interactions due to two nuclear effects: modifications of the parton densities in the nucleus, referred to here as shadowing, and the effect of non-isoscalar targets, with unequal numbers of neutrons and protons. Both these effects depend on the interaction medium. Because shadowing is larger for heavier nuclei, such as iron, found in the Earth's core, it introduces a zenith-angle dependent change in the absorption cross section. These modifications increase the cross sections by 1-2% at energies below 100 TeV (antishadowing), and reduce it by 3-4% at higher energies (shadowing).Nuclear effects also alter the inelasticity distribution of neutrino interactions in water/ice by increasing the number of low inelasticity interactions, with a larger effect for ν than ν. These effects are particularly large in the energy range below a few TeV. These effects could alter the cross sections inferred from events with tracks originating within the active detector volume as well as the ratio ν/ν inferred from inelasticity measurements.The uncertainties in these nuclear effects are larger than the uncertainties on the free-proton cross sections and will thus limit the systematic precision of future high-precision measurements at neutrino telescopes.

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IceCube-Gen2: A Vision for the Future of Neutrino Astronomy in Antarctica

Cited by 159 publications

References 146 publications

Detection of a particle shower at the Glashow resonance with IceCube

Detection of a particle shower at the Glashow resonance with IceCube

Peeking into the Origins of IceCube Neutrinos: I. Buried Transient TeV Miniburst Rates

Nuclear effects in high-energy neutrino interactions

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