APS » Phys. Rev. D » Volume 75 » Issue 10

A. Achterberg,³¹ M. Ackermann,³³ J. Adams,¹¹ J. Ahrens,²¹ K. Andeen,²⁰ D. W. Atlee,²⁹ J. N. Bahcall,²⁵ X. Bai,²³ B. Baret,⁹ S. W. Barwick,¹⁶ R. Bay,⁵ K. Beattie,⁷ T. Becka,²¹ J. K. Becker,¹³ K.-H. Becker,³² P. Berghaus,⁸ D. Berley,¹² E. Bernardini,³³ D. Bertrand,⁸ D. Z. Besson,¹⁷ E. Blaufuss,¹² D. J. Boersma,²⁰ C. Bohm,²⁷ J. Bolmont,³³ S. Böser,³³ O. Botner,³⁰ A. Bouchta,³⁰ J. Braun,²⁰ C. Burgess,²⁷ T. Burgess,²⁷ T. Castermans,²² D. Chirkin,⁷ B. Christy,¹² J. Clem,²³ D. F. Cowen,^29,28 M. V. D'Agostino,⁵ A. Davour,³⁰ C. T. Day,⁷ C. De Clercq,⁹ L. Demirörs,²³ F. Descamps,¹⁴ P. Desiati,²⁰ T. DeYoung,²⁹ J. C. Diaz-Velez,²⁰ J. Dreyer,¹³ J. P. Dumm,²⁰ M. R. Duvoort,³¹ W. R. Edwards,⁷ R. Ehrlich,¹² J. Eisch,²⁶ R. W. Ellsworth,¹² P. A. Evenson,²³ O. Fadiran,³ A. R. Fazely,⁴ T. Feser,²¹ K. Filimonov,⁵ B. D. Fox,²⁹ T. K. Gaisser,²³ J. Gallagher,¹⁹ R. Ganugapati,²⁰ H. Geenen,³² L. Gerhardt,¹⁶ A. Goldschmidt,⁷ J. A. Goodman,¹² R. Gozzini,²¹ S. Grullon,²⁰ A. Groß,¹⁵ R. M. Gunasingha,⁴ M. Gurtner,³² A. Hallgren,³⁰ F. Halzen,²⁰ K. Han,¹¹ K. Hanson,²⁰ D. Hardtke,⁵ R. Hardtke,²⁶ T. Harenberg,³² J. E. Hart,²⁹ T. Hauschildt,²³ D. Hays,⁷ J. Heise,³¹ K. Helbing,³² M. Hellwig,²¹ P. Herquet,²² G. C. Hill,²⁰ J. Hodges,²⁰ K. D. Hoffman,¹² B. Hommez,¹⁴ K. Hoshina,²⁰ D. Hubert,⁹ B. Hughey,²⁰ P. O. Hulth,²⁷ K. Hultqvist,²⁷ S. Hundertmark,²⁷ J.-P. Hülß,³² A. Ishihara,¹⁰ J. Jacobsen,⁷ G. S. Japaridze,³ H. Johansson,²⁷ A. Jones,⁷ J. M. Joseph,⁷ K.-H. Kampert,³² A. Karle,²⁰ H. Kawai,¹⁰ J. L. Kelley,²⁰ M. Kestel,²⁹ N. Kitamura,²⁰ S. R. Klein,⁷ S. Klepser,³³ G. Kohnen,²² H. Kolanoski,⁶ M. Kowalski,⁶ L. Köpke,²¹ M. Krasberg,²⁰ K. Kuehn,¹⁶ H. Landsman,²⁰ H. Leich,³³ D. Leier,¹³ M. Leuthold,¹ I. Liubarsky,¹⁸ J. Lundberg,³⁰ J. Lünemann,¹³ J. Madsen,²⁶ K. Mase,¹⁰ H. S. Matis,⁷ T. McCauley,⁷ C. P. McParland,⁷ A. Meli,¹³ T. Messarius,¹³ P. Mészáros,^29,28 H. Miyamoto,¹⁰ A. Mokhtarani,⁷ T. Montaruli,²⁰ A. Morey,⁵ R. Morse,²⁰ S. M. Movit,²⁸ K. Münich,¹³ R. Nahnhauer,³³ J. W. Nam,¹⁶ P. Nießen,²³ D. R. Nygren,⁷ H. Ögelman,²⁰ A. Olivas,¹² S. Patton,⁷ C. Peña-Garay,²⁵ C. Pérez de los Heros,³⁰ A. Piegsa,²¹ D. Pieloth,³³ A. C. Pohl,³⁰ R. Porrata,⁵ J. Pretz,¹² P. B. Price,⁵ G. T. Przybylski,⁷ K. Rawlins,² S. Razzaque,^28,29 E. Resconi,¹⁵ W. Rhode,¹³ M. Ribordy,²² A. Rizzo,⁹ S. Robbins,³² P. Roth,¹² C. Rott,²⁹ D. Rutledge,²⁹ D. Ryckbosch,¹⁴ H.-G. Sander,²¹ S. Sarkar,²⁴ S. Schlenstedt,³³ T. Schmidt,¹² D. Schneider,²⁰ D. Seckel,²³ S. H. Seo,²⁹ S. Seunarine,¹¹ A. Silvestri,¹⁶ A. J. Smith,¹² M. Solarz,⁵ C. Song,²⁰ J. E. Sopher,⁷ G. M. Spiczak,²⁶ C. Spiering,³³ M. Stamatikos,²⁰ T. Stanev,²³ P. Steffen,³³ T. Stezelberger,⁷ R. G. Stokstad,⁷ M. C. Stoufer,⁷ S. Stoyanov,²³ E. A. Strahler,²⁰ T. Straszheim,¹² K.-H. Sulanke,³³ G. W. Sullivan,¹² T. J. Sumner,¹⁸ I. Taboada,⁵ O. Tarasova,³³ A. Tepe,³² L. Thollander,²⁷ S. Tilav,²³ M. Tluczykont,³³ P. A. Toale,²⁹ D. Turčan,¹² N. van Eijndhoven,³¹ J. Vandenbroucke,⁵ A. Van Overloop,¹⁴ B. Voigt,³³ W. Wagner,²⁹ C. Walck,²⁷ H. Waldmann,³³ M. Walter,³³ Y.-R. Wang,²⁰ C. Wendt,²⁰ C. H. Wiebusch,¹ G. Wikström,²⁷ D. R. Williams,²⁹ R. Wischnewski,³³ H. Wissing,¹ K. Woschnagg,⁵ X. W. Xu,²⁶ G. Yodh,¹⁶ S. Yoshida,¹⁰ and J. D. Zornoza^20
1III Physikalisches Institut, RWTH Aachen University, D-52056, Aachen, Germany
²Department of Physics and Astronomy, University of Alaska Anchorage, 3211 Providence Dr., Anchorage, Alaska 99508, USA
³CTSPS, Clark-Atlanta University, Atlanta, Georgia 30314, USA
⁴Department of Physics, Southern University, Baton Rouge, Louisiana 70813, USA
⁵Department of Physics, University of California, Berkeley, California 94720, USA
⁶Institut für Physik, Humboldt Universität zu Berlin, D-12489 Berlin, Germany
⁷Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
⁸Université Libre de Bruxelles, Science Faculty CP230, B-1050 Brussels, Belgium
⁹Vrije Universiteit Brussel, Dienst ELEM, B-1050 Brussels, Belgium
¹⁰Department of Physics, Chiba University, Chiba 263-8522 Japan
¹¹Department of Physics and Astronomy, University of Canterbury, Private Bag 4800, Christchurch, New Zealand
¹²Department of Physics, University of Maryland, College Park, Maryland 20742, USA
¹³Department of Physics, Universität Dortmund, D-44221 Dortmund, Germany
¹⁴Department of Subatomic and Radiation Physics, University of Gent, B-9000 Gent, Belgium
¹⁵Max-Planck-Institut für Kernphysik, D-69177 Heidelberg, Germany
¹⁶Department of Physics and Astronomy, University of California, Irvine, California 92697, USA
¹⁷Department of Physics and Astronomy, University of Kansas, Lawrence, Kansas 66045, USA
¹⁸Blackett Laboratory, Imperial College, London SW7 2BW, United Kingdom
¹⁹Department of Astronomy, University of Wisconsin, Madison, Wisconsin 53706, USA
²⁰Department of Physics, University of Wisconsin, Madison, Wisconsin 53706, USA
²¹Institute of Physics, University of Mainz, Staudinger Weg 7, D-55099 Mainz, Germany
²²University of Mons-Hainaut, 7000 Mons, Belgium
²³Bartol Research Institute, University of Delaware, Newark, Delaware 19716, USA
²⁴Department of Physics, University of Oxford, 1 Keble Road, Oxford OX1 3NP, United Kingdom
²⁵Institute for Advanced Study, Princeton, New Jersey 08540, USA
²⁶Department of Physics, University of Wisconsin, River Falls, Wisconsin 54022, USA
²⁷Department of Physics, Stockholm University, SE-10691 Stockholm, Sweden
²⁸Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, Pennsylvania 16802, USA
²⁹Department of Physics, Pennsylvania State University, University Park, Pennsylvania 16802, USA
³⁰Division of High Energy Physics, Uppsala University, S-75121 Uppsala, Sweden
³¹Department of Physics and Astronomy, Utrecht University/SRON, NL-3584 CC Utrecht, The Netherlands
³²Department of Physics, University of Wuppertal, D-42119 Wuppertal, Germany
³³DESY, D-15735 Zeuthen, Germany

We report the results of a five-year survey of the northern sky to search for point sources of high energy neutrinos. The search was performed on the data collected with the AMANDA-II neutrino telescope in the years 2000 to 2004, with a live time of 1001 days. The sample of selected events consists of 4282 upward going muon tracks with high reconstruction quality and an energy larger than about 100 GeV. We found no indication of point sources of neutrinos and set 90% confidence level flux upper limits for an all-sky search and also for a catalog of 32 selected sources. For the all-sky search, our average (over declination and right ascension) experimentally observed upper limit Phi⁰=((E/(1 TeV)))^gamma·((d Phi)/dE) to a point source flux of muon and tau neutrino (detected as muons arising from taus) is Phi_{nu[sub mu] + [overline nu ][sub mu]}⁰+Phi_{nu[sub tau] + [overline nu ][sub tau]}⁰=11.1×  10^-11 TeV^-1 cm^-2 s^-1, in the energy range between 1.6 TeV and 2.5 PeV for a flavor ratio Phi_{nu[sub mu] + [overline nu ][sub mu]}⁰/Phi_{nu[sub tau] + [overline nu ][sub tau]}⁰=1 and assuming a spectral index gamma=2. It should be noticed that this is the first time we set upper limits to the flux of muon and tau neutrinos. In previous papers we provided muon neutrino upper limits only neglecting the sensitivity to a signal from tau neutrinos, which improves the limits by 10% to 16%. The value of the average upper limit presented in this work corresponds to twice the limit on the muon neutrino flux Phi_{nu[sub mu] + [overline nu ][sub mu]}⁰=5.5×10^-11 TeV^-1 cm^-2 s^-1. A stacking analysis for preselected active galactic nuclei and a search based on the angular separation of the events were also performed. We report the most stringent flux upper limits to date, including the results of a detailed assessment of systematic uncertainties.

©2007 The American Physical Society

View Cart	Download Citation
MyScitation	Print View