Atmospheric and astrophysical neutrinos above 1 TeV interacting in IceCube

Aartsen, M. G.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Ahrens, M.; Altmann, D.; Anderson, Tyler; Argüelles, C.; Arlen, T. C.; Auffenberg, J.; Bai, X.; 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.; Binder, G.; Bindig, D.; Bissok, M.; Blaufuss, E.; Blumenthal, J.; Boersma, D. J.; Böhm, 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.; Cowen, D. F.; Silva, A. H. Cruz; Danninger, M.; Daughhetee, J.; Davis, J.; Day, M.; André, J. P. A. M. de; Clercq, C. De; Ridder, S. De; Desiati, P.; Vries, Krijn de; DeYoung, T.; Díaz-Vélez, J. C.; Dunkman, M.; Eagan, R.; Eberhardt, B.; Eichmann, B.; Eisch, J.; Euler, S.; Evenson, P. A.; Fadiran, O.; Fazely, A. R.; Fedynitch, Anatoli; Feintzeig, J.; Felde, J.; Feusels, T.; Filimonov, K.; Finley, C.; Fischer-Wasels, T.; Flis, S.; Franckowiak, A.; Frantzen, K.; Fuchs, T.; Gaisser, T. K.; Gaïor, R.; Gallagher, J.; Gerhardt, L.; Gier, D.; Gladstone, L.; Glüsenkamp, T.; Goldschmidt, A.; Golup, G.; González, J. G.; Goodman, J. A.; Góra, Dariusz; Grant, D.; Gretskov, P.; Groh, J. C.; Groß, A.; Ha, C.; Haack, Christian; Ismail, A. Haj; Hallen, P.; Hallgren, A.; Halzen, F.; Hanson, K.; Hebecker, D.; Heereman, D.; Heinen, D.; Helbing, K.; Hellauer, R.; Hellwig, D.; Hickford, S.; Hill, G. C.; Hoffman, K. D.; Hoffmann, R.; Homeier, A.; Hoshina, K.; Huang, F.; Huelsnitz, W.; Hulth, P. O.; Hultqvist, K.; Hussain, Safeer; Ishihara, A.; Jacobi, E.; Jacobsen, J.; Jagielski, K.; Japaridze, G. S.; Jero, K.; Jlelati, O.; Jurković, M.; Kaminsky, B.; Kappes, A.; Karg, T.; Karle, A.; Kauer, M.; Keivani, A.; Kelley, J. L.; Kheirandish, Ali; 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.; Kriesten, A.; Krings, K.; Kroll, G.; Kroll, M.; Kunnen, J.; Kurahashi, N.; Kuwabara, T.; Labare, M.; Larsen, D.; Larson, M. J.; Lesiak-Bzdak, M.; Leuermann, M.; Leute, J.; Lünemann, J.; Madsen, J.; Maggi, G.; 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.; Morse, R.; Nahnhauer, R.; Naumann, Uwe; Niederhausen, H.; Nowicki, S. C.; Nygren, D. R.; Obertacke, A.; Odrowski, S.; Olivas, A.; Omairat, A.; O’Murchadha, A.; Palczewski, T.; Paul, Larissa; Penek, Ö.; Pepper, J. A.; Heros, C. Pérez de los; Pfendner, C.; Pieloth, D.; Pinat, E.; 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, Benedikt; Robertson, S.; Rodrigues, J. P.; Rongen, Martin; Rott, C.; Ruhe, T.; Ruzybayev, B.; Ryckbosch, D.; Saba, S. M.; Sander, H. G.; Sandroos, J.; 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.; Shanidze, R.; Smith, M. W. E.; Soldin, D.; Spiczak, G. M.; Spiering, C.; Stamatikos, M.; Stanev, T.; Stanisha, N. A.; Stasik, A.; Stezelberger, T.; Stokstad, R. G.; Stößl, A.; Strahler, E. A.; Strom, Lars Rickard; Strotjohann, N. L.; Sullivan, G. W.; Taavola, H.; Taboada, I.; Tamburro, A.; Tepe, A.; Ter–Antonyan, S.; Terliuk, A.; Tešić, G.; Tilav, S.; Toale, P. A.; Tobin, M. N.; Tosi, D.; Tselengidou, M.; Unger, E.; Usner, M.; Vallecorsa, S.; Eijndhoven, N. van; Vandenbroucke, J.; Santen, J. V.; Vehring, M.; Vöge, 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.; 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.91.022001

Cited by 264 publications

(250 citation statements)

References 78 publications

(88 reference statements)

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“…Our results should be compared with the recent IceCube discovery of high-energy neutrinos [43] (blue line in Fig. 7), whose sources are still unknown as well as with the unsuccessfull searches on GRBs from the IceCube telescope [16][17][18][19][20].…”

Section: Expected Diffuse Background and Uncertainties On The Local Rmentioning

confidence: 98%

“…However, h γp = 10 −5 would give a diffuse neutrino flux above the current IceCube observed flux. We therefore chose our canonical value in such a way to boost the neutrino emission with respect to the photon one without violating the IceCube current bounds [43]. We stress, however, that this parameter is currently unconstrained and scalings of the LL-GRB intensity with respect to the one presented here are not excluded yet.…”

Section: Expected Diffuse Background and Uncertainties On The Jet Parmentioning

confidence: 99%

See 1 more Smart Citation

Diffuse emission of high-energy neutrinos from gamma-ray burst fireballs

Tamborra

Ando

2015

J. Cosmol. Astropart. Phys.

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Abstract. Gamma-ray bursts (GRBs) have been suggested as possible sources of the highenergy neutrino flux recently detected by the IceCube telescope. We revisit the fireball emission model and elaborate an analytical prescription to estimate the high-energy neutrino prompt emission from pion and kaon decays, assuming that the leading mechanism for the neutrino production is lepto-hadronic. To this purpose, we include hadronic, radiative and adiabatic cooling effects and discuss their relevance for long-(including high-and lowluminosity) and short-duration GRBs. The expected diffuse neutrino background is derived, by requiring that the GRB high-energy neutrino counterparts follow up-to-date gamma-ray luminosity functions and redshift evolutions of the long and short GRBs. Although dedicated stacking searches have been unsuccessful up to now, we find that GRBs could contribute up to a few % to the observed IceCube high-energy neutrino flux for sub-PeV energies, assuming that the latter has a diffuse origin. Gamma-ray bursts, especially low-luminosity ones, could however be the main sources of the IceCube high-energy neutrino flux in the PeV range. While high-luminosity and low-luminosity GRBs have comparable intensities, the contribution from the short-duration component is significantly smaller. Our findings confirm the most-recent IceCube results on the GRB searches and suggest that larger exposure is mandatory to detect high-energy neutrinos from high-luminosity GRBs in the near future.

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Section: Expected Diffuse Background and Uncertainties On The Local Rmentioning

confidence: 98%

Section: Expected Diffuse Background and Uncertainties On The Jet Parmentioning

confidence: 99%

Diffuse emission of high-energy neutrinos from gamma-ray burst fireballs

Tamborra

Ando

2015

J. Cosmol. Astropart. Phys.

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“…Also we would like to comment on the new IceCube veto-based technique developed to study the neutrino spectrum between 10 and 100 TeV [48]. Using this new method they JHEP02(2015)189 were able to better understand their background at lower energies.…”

Section: Jhep02(2015)189mentioning

confidence: 99%

Possible interpretations of IceCube high-energy neutrino events

Fong

Minakata

Panes

et al. 2015

J. High Energ. Phys.

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Abstract:We discuss possible interpretations of the 37 high energy neutrino events observed by the IceCube experiment in the South Pole. We examine the possibility to explain the observed neutrino spectrum exclusively by the decays of a heavy long-lived particle of mass in the PeV range. We compare this with the standard scenario, namely, a single power-law spectrum related to neutrinos produced by astrophysical sources and a viable hybrid situation where the spectrum is a product of two components: a power-law and the long-lived particle decays. We present a simple extension of the Standard Model that could account for the heavy particle decays that are needed in order to explain the data. We show that the current data equally supports all above scenarios and try to evaluate the exposure needed in order to falsify them in the future.

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“…Accordingly, a number of models have been developed which explain the high-energy neutrino flux with DM [7,. Generally these models seek to explain the highest energy neutrinos observed by IceCube -the so-called High Energy Starting Events (HESE)-however some also deal with a putative excess in the lower energy Medium Energy Starting Events (MESE) [45], which has been discussed in the context of DM [46] and astrophysics [47][48][49]. Nevertheless, in these models the DM decays will generically also produce photons which can be searched for in other experiments.…”

Section: Jcap02(2018)049mentioning

confidence: 99%

A search for dark matter in the Galactic halo with HAWC

Abeysekara

Albert

Alfaro

et al. 2018

J. Cosmol. Astropart. Phys.

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Abstract. The High Altitude Water Cherenkov (HAWC) gamma-ray observatory is a wide field-of-view observatory sensitive to 500 GeV -100 TeV gamma rays and cosmic rays. With its observations over 2/3 of the sky every day, the HAWC observatory is sensitive to a wide variety of astrophysical sources, including possible gamma rays from dark matter. Dark matter annihilation and decay in the Milky Way Galaxy should produce gamma-ray signals across many degrees on the sky. The HAWC instantaneous field-of-view of 2 sr enables observations of extended regions on the sky, such as those from dark matter in the Galactic halo. Here we show limits on the dark matter annihilation cross-section and decay lifetime from HAWC observations of the Galactic halo with 15 months of data. These are some of the most robust limits on TeV and PeV dark matter, largely insensitive to the dark matter morphology. These limits begin to constrain models in which PeV IceCube neutrinos are explained by dark matter which primarily decays into hadrons.

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Atmospheric and astrophysical neutrinos above 1 TeV interacting in IceCube

Cited by 264 publications

References 78 publications

Diffuse emission of high-energy neutrinos from gamma-ray burst fireballs

Diffuse emission of high-energy neutrinos from gamma-ray burst fireballs

Possible interpretations of IceCube high-energy neutrino events

A search for dark matter in the Galactic halo with HAWC

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