Neutrino interferometry for high-precision tests of Lorentz symmetry with IceCube

,; Aartsen, M. G.; Hill, G. C.; Kyriacou, A.; Robertson, S.; Wallace, A.; Whelan, B. J.; Ackermann, M.; Bernardini, E.; Blot, S.; Bradascio, F.; Bretz, H.-P.; Brostean-Kaiser, J.; Franckowiak, A.; Jacobi, E.; Karg, T.; Kintscher, T.; Kunwar, S.; Nahnhauer, R.; Satalecka, K.; Spiering, C.; Stachurska, J.; Stasik, A.; Strotjohann, N. L.; Terliuk, A.; Usner, M.; van Santen, J.; Adams, J.; Bagherpour, H.; Aguilar, J. A.; Ansseau, I.; Heereman, D.; Meagher, K.; Meures, T.; O’Murchadha, A.; Pinat, E.; Raab, C.; Ahlers, M.; Bourbeau, E.; Koskinen, D. J.; Larson, M. J.; Medici, M.; Rameez, M.; Stuttard, T.; Ahrens, M.; Bohm, C.; Dumm, J. P.; Finley, C.; Flis, S.; Hultqvist, K.; Walck, C.; Zoll, M.; Al Samarai, I.; Bron, S.; Carver, T.; Christov, A.; Montaruli, T.; Altmann, D.; Anton, G.; Glüsenkamp, T.; Katz, U.; Kittler, T.; Tselengidou, M.; Andeen, K.; Plum, M.; Anderson, T.; DeLaunay, J. J.; Dunkman, M.; Eller, P.; Huang, F.; Keivani, A.; Lanfranchi, J. L.; Pankova, D. V.; Tešić, G.; Turley, C. F.; Weiss, M. J.; Argüelles, C.; Axani, S.; Collin, G. H.; Conrad, J. M.; Moulai, M.; Auffenberg, J.; Brenzke, M.; Glauch, T.; Haack, C.; Kalaczynski, P.; Koschinsky, J. P.; Leuermann, M.; Rädel, L.; Reimann, R.; Rongen, M.; Sälzer, T.; Schoenen, S.; Schumacher, L.; Stettner, J.; Vehring, M.; Vogel, E.; Wallraff, M.; Waza, A.; Wiebusch, C. H.; Bai, X.; Dvorak, E.; Barron, J. P.; Giang, W.; Grant, D.; Kopper, C.; Moore, R. W.; Nowicki, S. C.; Sanchez Herrera, S. E.; Sarkar, S.; Wandler, F. D.; Weaver, C.; Wood, T. R.; Woolsey, E.; Yanez, J. P.; Barwick, S. W.; Yodh, G.; Baum, V.; Böser, S.; di Lorenzo, V.; Eberhardt, B.; Ehrhardt, T.; Köpke, L.; Krückl, G.; Momenté, G.; Peiffer, P.; Sandroos, J.; Steuer, A.; Wiebe, K.; Bay, R.; Filimonov, K.; Price, P. B.; Woschnagg, K.; Beatty, J. J.; Becker Tjus, J.; Bos, F.; Eichmann, B.; Kroll, M.; Schöneberg, S.; Tenholt, F.; Becker, K.-H.; Bindig, D.; Helbing, K.; Hickford, S.; Hoffmann, R.; Lauber, F.; Naumann, U.; Obertacke Pollmann, A.; Soldin, D.; BenZvi, S.; Cross, R.; Berley, D.; Blaufuss, E.; Cheung, E.; Felde, J.; Friedman, E.; Hellauer, R.; Hoffman, K. D.; Maunu, R.; Olivas, A.; Schmidt, T.; Song, M.; Sullivan, G. W.; Besson, D. Z.; Binder, G.; Klein, S. R.; Miarecki, S.; Palczewski, T.; Tatar, J.; Börner, M.; Fuchs, T.; Hünnefeld, M.; Meier, M.; Menne, T.; Pieloth, D.; Rhode, W.; Ruhe, T.; Sandrock, A.; Schlunder, P.; Soedingrekso, J.; Werthebach, J.; Bose, D.; Dujmovic, H.; In, S.; Jeong, M.; Kang, W.; Kim, J.; Rott, C.; Botner, O.; Burgman, A.; Hallgren, A.; Pérez de los Heros, C.; Unger, E.; Bourbeau, J.; Braun, J.; Casey, J.; Chirkin, D.; Day, M.; Desiati, P.; Díaz-Vélez, J. C.; Fahey, S.; Ghorbani, K.; Griffith, Z.; Halzen, F.; Hanson, K.; Hokanson-Fasig, B.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; Liu, Q. R.; Luszczak, W.; Mancina, S.; McNally, F.; Merino, G.; Schneider, A.; Tobin, M. N.; Tosi, D.; Ty, B.; Vandenbroucke, J.; Wandkowsky, N.; Wendt, C.; Westerhoff, S.; Wille, L.; Wolf, M.; Wood, J.; Xu, D. L.; Yuan, T.; Brayeur, L.; Casier, M.; De Clercq, C.; de Vries, K. D.; de Wasseige, G.; Kunnen, J.; Lünemann, J.; Maggi, G.; Toscano, S.; van Eijndhoven, N.; Clark, K.; Classen, L.; Kappes, A.; Coenders, S.; Huber, M.; Krings, K.; Rea, I. C.; Resconi, E.; Turcati, A.; Cowen, D. F.; de André, J. P. A. M.; DeYoung, T.; Hignight, J.; Mahn, K. B. M.; Micallef, J.; Neer, G.; Rysewyk, D.; Dembinski, H.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Koirala, R.; Pandya, H.; Seckel, D.; Stanev, T.; Tilav, S.; De Ridder, S.; Labare, M.; Ryckbosch, D.; Van Driessche, W.; Vanheule, S.; Vraeghe, M.; de With, M.; Hebecker, D.; Kolanoski, H.; Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.; Gallagher, J.; Gerhardt, L.; Goldschmidt, A.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.; Hoshina, K.; Ishihara, A.; Kim, M.; Kuwabara, T.; Lu, L.; Mase, K.; Relich, M.; Stößl, A.; Yoshida, S.; Japaridze, G. S.; Jones, B. J. P.; Katori, T.; Mandalia, S.; Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.; Xu, Y.; Kohnen, G.; Kopper, S.; Nakarmi, P.; Pepper, J. A.; Santander, M.; Toale, P. A.; Williams, D. R.; Kowalski, M.; Kurahashi, N.; Relethford, B.; Richman, M.; Wills, L.; Madsen, J.; Seunarine, S.; Spiczak, G. M.; Maruyama, R.; Rawlins, K.; Sarkar, S.; Stamatikos, M.; Sutherland, M.; Taboada, I.; Tung, C. F.

doi:10.1038/s41567-018-0172-2

Cited by 99 publications

(90 citation statements)

References 77 publications

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“…Indeed, this effective potential has already been (locally) constrained by IceCube, using atmospheric neutrinos with energies 1 TeV. The limit on constant couplings of dimension-three operators is 10 −24 GeV [56], as could be expected from the vacuum oscillations term, ∆m 2 /(2 E ν ) = 5 × 10 −25 GeV (∆m 2 /10 −3 eV 2 ) (1 TeV/E ν ). Note that the effective interaction in the rest frame of the DM background has the Lorentz structure of a mass term, ν † ν, so similarly to the standard scenario, the lower the neutrino energy the more suppressed matter effects are.…”

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confidence: 93%

Flavor of cosmic neutrinos preserved by ultralight dark matter

Farzan

Palomares‐Ruiz

2019

Phys. Rev. D

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Within the standard propagation scenario, the flavor ratios of high-energy cosmic neutrinos at neutrino telescopes are expected to be around the democratic benchmark resulting from hadronic sources, (1 : 1 : 1) ⊕ . We show how the coupling of neutrinos to an ultralight dark matter complex scalar field would induce an effective neutrino mass that could lead to adiabatic neutrino propagation. This would result in the preservation at the detector of the production flavor composition of neutrinos at sources. This effect could lead to flavor ratios at detectors well outside the range predicted by the standard scenario of averaged oscillations. We also present an electroweak-invariant model that would lead to the required effective interaction between neutrinos and dark matter.Introduction.-Although cosmological observations have determined the contribution of dark matter (DM) to the energy budget of the Universe with an outstanding precision, the nature of the particles making up this component of the Universe is still unknown. In particular, the mass, spin and couplings of DM particles have not been determined yet. A lower bound on the mass (m DM ) comes from the de Broglie wavelength of the DM particle, λ dB = 2π/(m DM v), which is required to be smaller than the size of dwarf galaxies. Ultralight bosonic DM with a mass close to this bound, ∼ 10 −22 −10 −21 eV, has gained popularity (see, e.g., Refs. [1-6] for reviews), as it can address the small structure problems that the canonical cold DM scenario suffers from [7][8][9]. Recent studies of rotation curves of nearby galaxies [10], of dwarf galaxies [11][12][13], the comparison between the predictions of hydrodynamical simulations and Lyman-α observations [14][15][16][17], and analyses of cosmological data [18][19][20] have set lower bounds of ∼ 10 −21 eV on m DM .As long as the de Broglie wavelength, λ dB , is much larger than the average distance between DM particles (∼ n

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confidence: 93%

Flavor of cosmic neutrinos preserved by ultralight dark matter

Farzan

Palomares‐Ruiz

2019

Phys. Rev. D

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“…Lorentz violation can also induce time variability of the neutrino oscillation [349]. Effects could be observed in short and long baseline neutrino oscillation experiments which ought to provide strong constraints lower-dimensional operators [347,[349][350][351][352][353][354][355][356][357][358][359].…”

Section: Lorentz Violationmentioning

confidence: 99%

White Paper on New Opportunities at the Next-Generation Neutrino Experiments (Part 1: BSM Neutrino Physics and Dark Matter)

Argüelles

Aurisano

Batell

et al. 2019

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The authors of this paper primarily consist of those who participated in the New Opportunities at Next-Generation Neutrino Experiments workshop held on the campus of the University of Texas at Arlington. Given the anticipated and growing importance of BSM topics that can be explored in the next-generation neutrino experiments, the authors of this white paper are strong advocates of these topics and aim to become a de facto working group for the upcoming decadal study of the APS Division of Particles and Fields. This white paper is the first step to accomplish these goals, and provides a benchmark for ourselves to check progress toward making BSM physics a primary, yet complementary, topical area to precision neutrino oscillation parameter measurements. The authors plan to follow up this white paper and workshop with the subsequent series to ensure continued improvement and broadening of the BSM topics accessible to neutrino experiments, and to draw increasing attention to this field throughout the future. New Opportunities at the Next-Generation Neutrino Experiments White Paper New Opportunities at the Next-Generation Neutrino Experiments White Paper

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“…The subtraction of P ð0Þ in RðtÞ made the fit insensitive to the isotropic amplitude ðCÞcd, whose coefficients can be extracted by analyzing the time-independent energy and baseline dependencies of the oscillation probability. These effects have been constrained by atmospheric neutrino data [20,21] well beyond the reach of Daya Bay. Without ðCÞcd, a total of nine different coefficients are contained in the amplitudes ðA s Þcd; ðA c Þcd; ðB s Þcd and ðB c Þcd, as shown in Eq.…”

Section: Analysis On Lv-cptv Coefficientsmentioning

confidence: 99%

“…The SME also predicts deviations from the standard L=E oscillation behavior. The oscillated neutrino energy spectrum of atmospheric neutrinos has been examined for such a distortion both in the Super Kamiokande [20] and IceCube [21] experiments. No positive LV or CPTV signal has yet been observed, and neutrino oscillation experiments have set some of the most stringent limits on the violation of these fundamental symmetries of nature, down to the level of 10 −28 [21].…”

Section: Introductionmentioning

confidence: 99%

Search for a time-varying electron antineutrino signal at Daya Bay

Adey¹,

An²,

Balantekin³

et al. 2018

Phys. Rev. D

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A search for a time-varyingν e signal was performed with 621 days of data acquired by the Daya Bay Reactor Neutrino Experiment over 704 calendar days. The time spectrum of the measuredν e flux normalized to its prediction was analyzed with a Lomb-Scargle periodogram, which yielded no significant signal for periods ranging from 2 hours to nearly 2 years. The normalized time spectrum was also fit for a sidereal modulation under the Standard Model Extension (SME) framework to search for Lorentz and CPT violation (LV-CPTV). Limits were obtained for all six flavor pairsēμ;ēτ,μτ,ēē;μμ andττ by fitting them one at a time, constituting the first experimental constraints on the latter three. Daya Bay's high statistics and unique layout of multiple directions from three pairs of reactors to three experimental halls allowed the simultaneous constraint of individual SME LV-CPTV coefficients without assuming others contribute negligibly, a first for a neutrino experiment.

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Neutrino interferometry for high-precision tests of Lorentz symmetry with IceCube

Cited by 99 publications

References 77 publications

Flavor of cosmic neutrinos preserved by ultralight dark matter

Flavor of cosmic neutrinos preserved by ultralight dark matter

White Paper on New Opportunities at the Next-Generation Neutrino Experiments (Part 1: BSM Neutrino Physics and Dark Matter)

Search for a time-varying electron antineutrino signal at Daya Bay

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