Search for Extraterrestrial Point Sources of Neutrinos with AMANDA-II

Ahrens, J.; Bai, X.; Barwick, S. W.; Becka, T.; Becker, J. K.; Bernardini, E.; Bertrand, Daniel; Binon, Freddy; Biron, A.; Boersma, D. J.; Böser, S.; Botner, O.; Bouchta, A.; Bouhali, O.; Burgess, T.; Carius, Staffan; Castermans, T.; Chen, A.; Chirkin, D.; Collin, Bertrand; Conrad, J.; Cooley, J.; Cowen, D. F.; Davour, Anna; Clercq, C. De; DeYoung, T.; Desiati, P.; Dewulf, J. P.; Ekström, P.; Feser, T.; Gaisser, T. K.; Ganugapati, R.; Gaug, M.; Geenen, H.; Gerhardt, L.; Goldschmidt, A.; Groß, A.; Hallgren, A.; Halzen, F.; Hanson, K.; Hardtke, R.; Harenberg, T.; Hauschildt, T.; Helbing, K.; Hellwig, M.; Herquet, P.; Hill, G. C.; Hubert, D.; Hughey, B.; Hulth, P. O.; Hultqvist, K.; Hundertmark, S.; Jacobsen, J.; Karle, A.; Kestel, M.; Köpke, L.; Kowalski, M.; Kuêhn, K.; Lamoureux, J.I.; Leich, H.; Leuthold, M.; Lindahl, P.; Liubarsky, I.; Madsen, J.; Mandli, Kyle T.; Marciniewski, P.; Matis, H. S.; McParland, C.; Messarius, T.; Minaeva, Y.; Miočinović, P.; Morse, R.; Münich, K.; Nahnhauer, R.; Neunhöffer, T.; Nießen, P.; Nygren, D. R.; Öğelman, H.; Olbrechts, Ph.; Heros, C. Pérez de los; Pohl, A. C.; Porrata, R.; Price, P. B.; Przybylski, G. T.; Rawlins, K.; Resconi, E.; Rhode, W.; Ribordy, M.; Richter, S.; Martino, J. Rodrı́guez; Sander, H. G.; Schinarakis, K.; Schlenstedt, S.; Schmidt, T.; Schneider, D.; Schwarz, R.; Silvestri, A.; Solarz, M.; Spiczak, G. M.; Spiering, Christian; Stamatikos, M.; Steele, D.; Steffen, P.; Stokstad, R. G.; Sulanke, K.-H.; Taboada, I.; Thollander, L.; Tilav, S.; Wagner, Wolfgang; Walck, C.; Wang, Y. R.; Wiebusch, C. H.; Wiedemann, C.; Wischnewski, R.; Wissing, H.; Woschnagg, K.; Yodh, G.

doi:10.1103/physrevlett.92.071102

Cited by 73 publications

(30 citation statements)

References 17 publications

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“…Neutrino time delay might therefore be a very precise probe of even n > 3 dispersion corrections. Of course, first an identifiable GRB neutrino flux must be detected, which has not happened yet [5]. Assuming that a flux is seen and able to be correlated on the sky with a GRB, one must still disentangle the signal.…”

Section: Astrophysical Constraints On Lorentz Violationmentioning

confidence: 99%

Modern Tests of Lorentz Invariance

Mattingly

2005

Living Rev. Relativ.

1,051

1,284

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Motivated by ideas about quantum gravity, a tremendous amount of effort over the past decade has gone into testing Lorentz invariance in various regimes. This review summarizes both the theoretical frameworks for tests of Lorentz invariance and experimental advances that have made new high precision tests possible. The current constraints on Lorentz violating effects from both terrestrial experiments and astrophysical observations are presented.

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Section: Astrophysical Constraints On Lorentz Violationmentioning

confidence: 99%

Modern Tests of Lorentz Invariance

Mattingly

2005

Living Rev. Relativ.

1,051

1,284

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“…Most of these models predict neutrino fluxes that should be easily detectable by a 1-km 2 neutrino detector of the IceCube type and in some cases by the detectors of the present AMANDA II type. Recent searches of the discrete neutrino sources by the AMANDA II detector, which are based on the analysis of the three-year experimental data (Ahrens et al 2004;Ackermann et al 2005), show no clear evidence of a significant neutrino flux excess above the background. E-mail: bednar@fizwe4.fic.uni.lodz.pl…”

Section: Introductionmentioning

confidence: 99%

GeV gamma-rays and TeV neutrinos from very massive compact binary systems: the case of WR 20a

Bednarek

2005

Monthly Notices of the Royal Astronomical Society: Letters

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Massive Wolf–Rayet stars in a compact binary system are characterized by very strong winds which collide, creating a shock wave. If the wind nuclei, from helium up to oxygen, accelerated at the shock can reach large enough energies, they suffer disintegration in collisions with soft thermal radiation from the massive stars injecting relativistic protons and neutrons. Protons collide with the matter of the wind and a fraction of neutrons collide with the massive stars producing γ‐rays and neutrinos via decay of pions. We calculate γ‐ray fluxes from inverse Compton e± pair cascades initiated by primary γ‐rays and leptons, which are produced by protons, and the neutrino fluxes, produced by protons and neutrons, for the example compact massive binary WR 20a. From normalization of these cascade γ‐ray spectra to the fluxes of the EGRET sources 2EG J1021 − 5835 and 2EG J1049 − 5847 observed in the direction of WR 20a, we conclude that this massive binary can be detected by the IceCube type of neutrino detector. The estimated muon neutrino event rate inside the 1‐km2 detector during 1 year is between a few and a few tens, depending on the spectrum of accelerated nuclei.

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“…To summarize, this work suggests that pulsars are unlikely to be strong sources of TeV neutrinos. The non-detection of any statistically significant excess from the direction of any pulsar by the Antarctic Muon and Neutrino Detector Array (AMANDA)-II telescope (Ahrens et al 2004;Ackermann et al 2005Ackermann et al , 2008 is thus as per expectations.…”

Section: O N C L U S I O Nmentioning

confidence: 74%

TeV neutrinos and gamma-rays from pulsars

Bhadra¹,

Dey²

2009

Monthly Notices of the Royal Astronomical Society

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Recent studies suggest that pulsars could be strong sources of TeV muon neutrinos provided positive ions are accelerated by pulsar polar caps to PeV energies. In such a situation, muon neutrinos are produced through the Δ‐resonance in interactions of pulsar‐accelerated ions with its thermal radiation field. High‐energy gamma‐rays should also be produced simultaneously in pulsar environment as both charged and neutral pions are generated in the interactions of energetic hadrons with the ambient photon fields. Here, we estimate TeV gamma‐ray flux at the Earth from a few nearby young pulsars. When compared with the observations, we find that proper consideration of the effect of polar cap geometry in flux calculation is important. Incorporating such an effect, we obtain the (revised) event rates at the Earth due to a few potential nearby pulsars. The results suggest that pulsars are unlikely to be detected by the upcoming neutrino telescopes. We also estimate TeV gamma‐ray and neutrino fluxes from pulsar nebulae for the adopted model of particle acceleration.

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Search for Extraterrestrial Point Sources of Neutrinos with AMANDA-II

Cited by 73 publications

References 17 publications

Modern Tests of Lorentz Invariance

Modern Tests of Lorentz Invariance

GeV gamma-rays and TeV neutrinos from very massive compact binary systems: the case of WR 20a

TeV neutrinos and gamma-rays from pulsars

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