Flux limits on ultra high energy neutrinos with AMANDA-B10

被引：68

作者：

Ackermann, M

Ahrens, J

Albrecht, H

Atlee, D

Bai, X

Bay, R

Bartelt, M

Barwick, SW

Becka, T

Becker, KH

Becker, JK

Bernardini, E

Bertrand, D

Boersma, DJ

Böser, S

Botner, O

Bouchta, A

Bouhali, O

Braun, J

Burgess, C

Burgess, T

Castermans, T

Chirkin, D

Coarasa, T

Collin, B

Conrad, J

Cooley, J

Cowen, DF

Davour, A

De Clercq, C

DeYoung, T

Desiati, P

Ekström, P

Feser, T

Gaisser, TK

Ganugapati, R

Geenen, H

Gerhardt, L

Goldschmidt, A

Gross, A

Hallgren, A

Halzen, F

Hanson, K

Hardtke, D

Hardtke, R

Harenberg, T

Hauschildt, T

Helbing, K

Hellwig, M

Herquet, P

机构：

[1] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden

[2] DESY, D-15735 Zeuthen, Germany

[3] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany

[4] Penn State Univ, Dept Phys, University Pk, PA 16802 USA

[5] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA

[6] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[7] Berg Univ Wuppertal, Dept Phys, D-42097 Wuppertal, Germany

[8] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA

[9] Free Univ Brussels, Fac Sci CP230, B-1050 Brussels, Belgium

[10] Uppsala Univ, Div High Energy Phys, S-75121 Uppsala, Sweden

[11] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA

[12] Univ Mons, B-7000 Mons, Belgium

[13] Free Univ Brussels, Dienst ELEM, B-1050 Brussels, Belgium

[14] Univ Maryland, Dept Phys, College Pk, MD 20742 USA

[15] Lawrence Berkeley Lab, Berkeley, CA 94720 USA

[16] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA

[17] Univ Kalmar, Dept Chem & Biomed Sci, S-39182 Kalmar, Sweden

[18] Univ Simon Bolivar, Dept Phys, Caracas 1080, Venezuela

来源：

ASTROPARTICLE PHYSICS | 2005年 / 22卷 / 5-6期

基金：

美国国家科学基金会;

关键词：

neutrino telescopes; neutrino astronomy; UHE neutrinos; AMANDA;

D O I：

10.1016/j.astropartphys.2004.09.008

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Data taken during 1997 with the AMANDA-B10 detector are searched for a diffuse flux of neutrinos of all flavors with energies above 10(16) eV. At these energies the Earth is opaque to neutrinos, and thus neutrino induced events are concentrated at the horizon. The background are large muon bundles from down-going atmospheric air shower events. No excess events above the background expectation are observed and a neutrino flux following E-2, with an equal mix of all flavors, is limited to E(2)Phi(10(15) eV < E < 3 x 10(18) eV) less than or equal to 0.99 x 10(-6) GeV cm(-2) s(-1) sr(-1) at 90% confidence level. This is the most restrictive experimental bound placed by any neutrino detector at these energies. Bounds to specific extraterrestrial neutrino flux predictions are also presented. (C) 2004 Elsevier B.V. All rights reserved.

引用

页码：339 / 353

页数：15

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