Search for neutrino-induced cascades with five years of AMANDA data
We report on the search for electromagnetic and hadronic showers ("cascades") produced by a diffuse flux of extraterrestrial neutrinos in the AMANDA neutrino telescope. Data for this analysis were recorded during 1001 days of detector livetime in the years 2000-2004. The observed event rat...
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creator | Abbasi, R. Abdou, Y. Abu-Zayyad, T. Actis, O. Adams, J. Aguilar, J. A. Ahlers, M. Andeen, K. Auffenberg, J. Bai, X. Baker, Mark D. Barwick, S. W. Bay, R. Bazo Alba, J. L. Beattie, K. Beatty, J. J. Bechet, S. Becker, J. K. Becker, K.-H. Benabderrahmane, M. L. Berdermann, J. Berghaus, P. Berley, D. Bernardini, E. Bertrand, D. Besson, D. Z. Bissok, M. Blaufuss, E. Boersma, D. J. Bohm, C. Böser, S. Botner, O. Bradley, L. Braun, J. Buitink, S. Carson, M. Chirkin, D. Christy, B. Clem, J. Clevermann, F. Cohen, S. Colnard, C. Cowen, D. F. d'Agostino, M. V. Danninger, M. Davis, J. C. de Clercq, C. Demirörs, L. Depaepe, O. Descamps, F. Desiati, P. de Vries-Uiterweerd, G. Deyoung, T. Díaz-Vélez, J. C. Dreyer, J. Dumm, J. P. Duvoort, M. R. Ehrlich, R. Eisch, J. Ellsworth, R. W. Engdegård, O. Euler, S. Evenson, P. A. Fadiran, O. Fazely, A. R. Feusels, T. Filimonov, K. Finley, C. Foerster, M. M. Fox, B. D. Franckowiak, A. Franke, R. Gaisser, T. K. Gallagher, J. Ganugapati, R. Geisler, M. Gerhardt, L. Gladstone, L. Glüsenkamp, T. Goldschmidt, A. Goodman, J. A. Grant, D. Griesel, T. Gross, A. Grullon, S. Gunasingha, R. M. Gurtner, M. Ha, C. Hallgren, A. Halzen, F. Han, K. Hanson, K. Helbing, K. Herquet, P. Hickford, S. Hill, G. C. Hoffman, K. D. Homeier, A. Hoshina, K. Hubert, D. |
description | We report on the search for electromagnetic and hadronic showers ("cascades") produced by a diffuse flux of extraterrestrial neutrinos in the AMANDA neutrino telescope. Data for this analysis were recorded during 1001 days of detector livetime in the years 2000-2004. The observed event rates are consistent with the background expectation from atmospheric neutrinos and muons. An upper limit is derived for the diffuse flux of neutrinos of all flavors assuming a flavor ratio of νe:νμ:ντ = 1:1:1 at the detection site. The all-flavor flux of neutrinos with an energy spectrum Φ ∝ E-2 is less than 5.0 × 10-7 GeV s-1 sr-1 cm-2 at a 90% C.L. Here, 90% of the simulated signal would fall within the energy range 40 TeV to 9 PeV. We discuss flux limits in the context of several specific models of extraterrestrial and prompt atmospheric neutrino production. |
doi_str_mv | 10.1016/J.ASTROPARTPHYS.2010.10.007 |
format | Article |
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A. ; Ahlers, M. ; Andeen, K. ; Auffenberg, J. ; Bai, X. ; Baker, Mark D. ; Barwick, S. W. ; Bay, R. ; Bazo Alba, J. L. ; Beattie, K. ; Beatty, J. J. ; Bechet, S. ; Becker, J. K. ; Becker, K.-H. ; Benabderrahmane, M. L. ; Berdermann, J. ; Berghaus, P. ; Berley, D. ; Bernardini, E. ; Bertrand, D. ; Besson, D. Z. ; Bissok, M. ; Blaufuss, E. ; Boersma, D. J. ; Bohm, C. ; Böser, S. ; Botner, O. ; Bradley, L. ; Braun, J. ; Buitink, S. ; Carson, M. ; Chirkin, D. ; Christy, B. ; Clem, J. ; Clevermann, F. ; Cohen, S. ; Colnard, C. ; Cowen, D. F. ; d'Agostino, M. V. ; Danninger, M. ; Davis, J. C. ; de Clercq, C. ; Demirörs, L. ; Depaepe, O. ; Descamps, F. ; Desiati, P. ; de Vries-Uiterweerd, G. ; Deyoung, T. ; Díaz-Vélez, J. C. ; Dreyer, J. ; Dumm, J. P. ; Duvoort, M. R. ; Ehrlich, R. ; Eisch, J. ; Ellsworth, R. W. ; Engdegård, O. ; Euler, S. ; Evenson, P. A. ; Fadiran, O. ; Fazely, A. R. ; Feusels, T. ; Filimonov, K. ; Finley, C. ; Foerster, M. M. ; Fox, B. D. ; Franckowiak, A. ; Franke, R. ; Gaisser, T. K. ; Gallagher, J. ; Ganugapati, R. ; Geisler, M. ; Gerhardt, L. ; Gladstone, L. ; Glüsenkamp, T. ; Goldschmidt, A. ; Goodman, J. A. ; Grant, D. ; Griesel, T. ; Gross, A. ; Grullon, S. ; Gunasingha, R. M. ; Gurtner, M. ; Ha, C. ; Hallgren, A. ; Halzen, F. ; Han, K. ; Hanson, K. ; Helbing, K. ; Herquet, P. ; Hickford, S. ; Hill, G. C. ; Hoffman, K. D. ; Homeier, A. ; Hoshina, K. ; Hubert, D.</creator><creatorcontrib>Abbasi, R. ; Abdou, Y. ; Abu-Zayyad, T. ; Actis, O. ; Adams, J. ; Aguilar, J. A. ; Ahlers, M. ; Andeen, K. ; Auffenberg, J. ; Bai, X. ; Baker, Mark D. ; Barwick, S. W. ; Bay, R. ; Bazo Alba, J. L. ; Beattie, K. ; Beatty, J. J. ; Bechet, S. ; Becker, J. K. ; Becker, K.-H. ; Benabderrahmane, M. L. ; Berdermann, J. ; Berghaus, P. ; Berley, D. ; Bernardini, E. ; Bertrand, D. ; Besson, D. Z. ; Bissok, M. ; Blaufuss, E. ; Boersma, D. J. ; Bohm, C. ; Böser, S. ; Botner, O. ; Bradley, L. ; Braun, J. ; Buitink, S. ; Carson, M. ; Chirkin, D. ; Christy, B. ; Clem, J. ; Clevermann, F. ; Cohen, S. ; Colnard, C. ; Cowen, D. F. ; d'Agostino, M. V. ; Danninger, M. ; Davis, J. C. ; de Clercq, C. ; Demirörs, L. ; Depaepe, O. ; Descamps, F. ; Desiati, P. ; de Vries-Uiterweerd, G. ; Deyoung, T. ; Díaz-Vélez, J. C. ; Dreyer, J. ; Dumm, J. P. ; Duvoort, M. R. ; Ehrlich, R. ; Eisch, J. ; Ellsworth, R. W. ; Engdegård, O. ; Euler, S. ; Evenson, P. A. ; Fadiran, O. ; Fazely, A. R. ; Feusels, T. ; Filimonov, K. ; Finley, C. ; Foerster, M. M. ; Fox, B. D. ; Franckowiak, A. ; Franke, R. ; Gaisser, T. K. ; Gallagher, J. ; Ganugapati, R. ; Geisler, M. ; Gerhardt, L. ; Gladstone, L. ; Glüsenkamp, T. ; Goldschmidt, A. ; Goodman, J. A. ; Grant, D. ; Griesel, T. ; Gross, A. ; Grullon, S. ; Gunasingha, R. M. ; Gurtner, M. ; Ha, C. ; Hallgren, A. ; Halzen, F. ; Han, K. ; Hanson, K. ; Helbing, K. ; Herquet, P. ; Hickford, S. ; Hill, G. C. ; Hoffman, K. D. ; Homeier, A. ; Hoshina, K. ; Hubert, D.</creatorcontrib><description>We report on the search for electromagnetic and hadronic showers ("cascades") produced by a diffuse flux of extraterrestrial neutrinos in the AMANDA neutrino telescope. Data for this analysis were recorded during 1001 days of detector livetime in the years 2000-2004. The observed event rates are consistent with the background expectation from atmospheric neutrinos and muons. An upper limit is derived for the diffuse flux of neutrinos of all flavors assuming a flavor ratio of νe:νμ:ντ = 1:1:1 at the detection site. The all-flavor flux of neutrinos with an energy spectrum Φ ∝ E-2 is less than 5.0 × 10-7 GeV s-1 sr-1 cm-2 at a 90% C.L. Here, 90% of the simulated signal would fall within the energy range 40 TeV to 9 PeV. 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M.</creatorcontrib><creatorcontrib>Gurtner, M.</creatorcontrib><creatorcontrib>Ha, C.</creatorcontrib><creatorcontrib>Hallgren, A.</creatorcontrib><creatorcontrib>Halzen, F.</creatorcontrib><creatorcontrib>Han, K.</creatorcontrib><creatorcontrib>Hanson, K.</creatorcontrib><creatorcontrib>Helbing, K.</creatorcontrib><creatorcontrib>Herquet, P.</creatorcontrib><creatorcontrib>Hickford, S.</creatorcontrib><creatorcontrib>Hill, G. C.</creatorcontrib><creatorcontrib>Hoffman, K. D.</creatorcontrib><creatorcontrib>Homeier, A.</creatorcontrib><creatorcontrib>Hoshina, K.</creatorcontrib><creatorcontrib>Hubert, D.</creatorcontrib><title>Search for neutrino-induced cascades with five years of AMANDA data</title><title>Astroparticle physics</title><description>We report on the search for electromagnetic and hadronic showers ("cascades") produced by a diffuse flux of extraterrestrial neutrinos in the AMANDA neutrino telescope. Data for this analysis were recorded during 1001 days of detector livetime in the years 2000-2004. The observed event rates are consistent with the background expectation from atmospheric neutrinos and muons. An upper limit is derived for the diffuse flux of neutrinos of all flavors assuming a flavor ratio of νe:νμ:ντ = 1:1:1 at the detection site. The all-flavor flux of neutrinos with an energy spectrum Φ ∝ E-2 is less than 5.0 × 10-7 GeV s-1 sr-1 cm-2 at a 90% C.L. Here, 90% of the simulated signal would fall within the energy range 40 TeV to 9 PeV. We discuss flux limits in the context of several specific models of extraterrestrial and prompt atmospheric neutrino production.</description><subject>Astrophysics</subject><subject>Cosmology and Extra-Galactic Astrophysics</subject><subject>High Energy Astrophysical Phenomena</subject><subject>Physics</subject><subject>Sciences of the Universe</subject><issn>0927-6505</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2011</creationdate><recordtype>article</recordtype><recordid>eNqVzssKgkAYhuFZFGSHexhoGdo_WorLoQMSnUg3rYYfHXGiVGa06O6T6AZafYv3WXyETBk4DJg_3zk8Ti6nM78k5-gaOy58iwMQ9IgFoRvY_hKWAzI05gbAFuAtLLKKJeq0oHmlaSnbRquyslWZtanMaIomxUwa-lJNR9RT0nfHDa1yyg_8uOY0wwbHpJ_j3cjJb0dktt0kq8gu8C5qrR6o36JCJSK-F6p0a090p8APwX8y7z_9AR9LRbg</recordid><startdate>201101</startdate><enddate>201101</enddate><creator>Abbasi, R.</creator><creator>Abdou, Y.</creator><creator>Abu-Zayyad, T.</creator><creator>Actis, O.</creator><creator>Adams, J.</creator><creator>Aguilar, J. 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A. ; Ahlers, M. ; Andeen, K. ; Auffenberg, J. ; Bai, X. ; Baker, Mark D. ; Barwick, S. W. ; Bay, R. ; Bazo Alba, J. L. ; Beattie, K. ; Beatty, J. J. ; Bechet, S. ; Becker, J. K. ; Becker, K.-H. ; Benabderrahmane, M. L. ; Berdermann, J. ; Berghaus, P. ; Berley, D. ; Bernardini, E. ; Bertrand, D. ; Besson, D. Z. ; Bissok, M. ; Blaufuss, E. ; Boersma, D. J. ; Bohm, C. ; Böser, S. ; Botner, O. ; Bradley, L. ; Braun, J. ; Buitink, S. ; Carson, M. ; Chirkin, D. ; Christy, B. ; Clem, J. ; Clevermann, F. ; Cohen, S. ; Colnard, C. ; Cowen, D. F. ; d'Agostino, M. V. ; Danninger, M. ; Davis, J. C. ; de Clercq, C. ; Demirörs, L. ; Depaepe, O. ; Descamps, F. ; Desiati, P. ; de Vries-Uiterweerd, G. ; Deyoung, T. ; Díaz-Vélez, J. C. ; Dreyer, J. ; Dumm, J. P. ; Duvoort, M. R. ; Ehrlich, R. ; Eisch, J. ; Ellsworth, R. W. ; Engdegård, O. ; Euler, S. ; Evenson, P. A. ; Fadiran, O. ; Fazely, A. R. ; Feusels, T. ; Filimonov, K. ; Finley, C. ; Foerster, M. M. ; Fox, B. D. ; Franckowiak, A. ; Franke, R. ; Gaisser, T. K. ; Gallagher, J. ; Ganugapati, R. ; Geisler, M. ; Gerhardt, L. ; Gladstone, L. ; Glüsenkamp, T. ; Goldschmidt, A. ; Goodman, J. A. ; Grant, D. ; Griesel, T. ; Gross, A. ; Grullon, S. ; Gunasingha, R. M. ; Gurtner, M. ; Ha, C. ; Hallgren, A. ; Halzen, F. ; Han, K. ; Hanson, K. ; Helbing, K. ; Herquet, P. ; Hickford, S. ; Hill, G. C. ; Hoffman, K. D. ; Homeier, A. ; Hoshina, K. ; Hubert, D.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-hal_primary_oai_HAL_in2p3_00706906v13</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2011</creationdate><topic>Astrophysics</topic><topic>Cosmology and Extra-Galactic Astrophysics</topic><topic>High Energy Astrophysical Phenomena</topic><topic>Physics</topic><topic>Sciences of the Universe</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Abbasi, R.</creatorcontrib><creatorcontrib>Abdou, Y.</creatorcontrib><creatorcontrib>Abu-Zayyad, T.</creatorcontrib><creatorcontrib>Actis, O.</creatorcontrib><creatorcontrib>Adams, J.</creatorcontrib><creatorcontrib>Aguilar, J. A.</creatorcontrib><creatorcontrib>Ahlers, M.</creatorcontrib><creatorcontrib>Andeen, K.</creatorcontrib><creatorcontrib>Auffenberg, J.</creatorcontrib><creatorcontrib>Bai, X.</creatorcontrib><creatorcontrib>Baker, Mark D.</creatorcontrib><creatorcontrib>Barwick, S. W.</creatorcontrib><creatorcontrib>Bay, R.</creatorcontrib><creatorcontrib>Bazo Alba, J. L.</creatorcontrib><creatorcontrib>Beattie, K.</creatorcontrib><creatorcontrib>Beatty, J. J.</creatorcontrib><creatorcontrib>Bechet, S.</creatorcontrib><creatorcontrib>Becker, J. K.</creatorcontrib><creatorcontrib>Becker, K.-H.</creatorcontrib><creatorcontrib>Benabderrahmane, M. L.</creatorcontrib><creatorcontrib>Berdermann, J.</creatorcontrib><creatorcontrib>Berghaus, P.</creatorcontrib><creatorcontrib>Berley, D.</creatorcontrib><creatorcontrib>Bernardini, E.</creatorcontrib><creatorcontrib>Bertrand, D.</creatorcontrib><creatorcontrib>Besson, D. Z.</creatorcontrib><creatorcontrib>Bissok, M.</creatorcontrib><creatorcontrib>Blaufuss, E.</creatorcontrib><creatorcontrib>Boersma, D. J.</creatorcontrib><creatorcontrib>Bohm, C.</creatorcontrib><creatorcontrib>Böser, S.</creatorcontrib><creatorcontrib>Botner, O.</creatorcontrib><creatorcontrib>Bradley, L.</creatorcontrib><creatorcontrib>Braun, J.</creatorcontrib><creatorcontrib>Buitink, S.</creatorcontrib><creatorcontrib>Carson, M.</creatorcontrib><creatorcontrib>Chirkin, D.</creatorcontrib><creatorcontrib>Christy, B.</creatorcontrib><creatorcontrib>Clem, J.</creatorcontrib><creatorcontrib>Clevermann, F.</creatorcontrib><creatorcontrib>Cohen, S.</creatorcontrib><creatorcontrib>Colnard, C.</creatorcontrib><creatorcontrib>Cowen, D. F.</creatorcontrib><creatorcontrib>d'Agostino, M. V.</creatorcontrib><creatorcontrib>Danninger, M.</creatorcontrib><creatorcontrib>Davis, J. C.</creatorcontrib><creatorcontrib>de Clercq, C.</creatorcontrib><creatorcontrib>Demirörs, L.</creatorcontrib><creatorcontrib>Depaepe, O.</creatorcontrib><creatorcontrib>Descamps, F.</creatorcontrib><creatorcontrib>Desiati, P.</creatorcontrib><creatorcontrib>de Vries-Uiterweerd, G.</creatorcontrib><creatorcontrib>Deyoung, T.</creatorcontrib><creatorcontrib>Díaz-Vélez, J. C.</creatorcontrib><creatorcontrib>Dreyer, J.</creatorcontrib><creatorcontrib>Dumm, J. P.</creatorcontrib><creatorcontrib>Duvoort, M. R.</creatorcontrib><creatorcontrib>Ehrlich, R.</creatorcontrib><creatorcontrib>Eisch, J.</creatorcontrib><creatorcontrib>Ellsworth, R. W.</creatorcontrib><creatorcontrib>Engdegård, O.</creatorcontrib><creatorcontrib>Euler, S.</creatorcontrib><creatorcontrib>Evenson, P. A.</creatorcontrib><creatorcontrib>Fadiran, O.</creatorcontrib><creatorcontrib>Fazely, A. R.</creatorcontrib><creatorcontrib>Feusels, T.</creatorcontrib><creatorcontrib>Filimonov, K.</creatorcontrib><creatorcontrib>Finley, C.</creatorcontrib><creatorcontrib>Foerster, M. M.</creatorcontrib><creatorcontrib>Fox, B. D.</creatorcontrib><creatorcontrib>Franckowiak, A.</creatorcontrib><creatorcontrib>Franke, R.</creatorcontrib><creatorcontrib>Gaisser, T. K.</creatorcontrib><creatorcontrib>Gallagher, J.</creatorcontrib><creatorcontrib>Ganugapati, R.</creatorcontrib><creatorcontrib>Geisler, M.</creatorcontrib><creatorcontrib>Gerhardt, L.</creatorcontrib><creatorcontrib>Gladstone, L.</creatorcontrib><creatorcontrib>Glüsenkamp, T.</creatorcontrib><creatorcontrib>Goldschmidt, A.</creatorcontrib><creatorcontrib>Goodman, J. A.</creatorcontrib><creatorcontrib>Grant, D.</creatorcontrib><creatorcontrib>Griesel, T.</creatorcontrib><creatorcontrib>Gross, A.</creatorcontrib><creatorcontrib>Grullon, S.</creatorcontrib><creatorcontrib>Gunasingha, R. M.</creatorcontrib><creatorcontrib>Gurtner, M.</creatorcontrib><creatorcontrib>Ha, C.</creatorcontrib><creatorcontrib>Hallgren, A.</creatorcontrib><creatorcontrib>Halzen, F.</creatorcontrib><creatorcontrib>Han, K.</creatorcontrib><creatorcontrib>Hanson, K.</creatorcontrib><creatorcontrib>Helbing, K.</creatorcontrib><creatorcontrib>Herquet, P.</creatorcontrib><creatorcontrib>Hickford, S.</creatorcontrib><creatorcontrib>Hill, G. C.</creatorcontrib><creatorcontrib>Hoffman, K. D.</creatorcontrib><creatorcontrib>Homeier, A.</creatorcontrib><creatorcontrib>Hoshina, K.</creatorcontrib><creatorcontrib>Hubert, D.</creatorcontrib><collection>Hyper Article en Ligne (HAL)</collection><jtitle>Astroparticle physics</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Abbasi, R.</au><au>Abdou, Y.</au><au>Abu-Zayyad, T.</au><au>Actis, O.</au><au>Adams, J.</au><au>Aguilar, J. A.</au><au>Ahlers, M.</au><au>Andeen, K.</au><au>Auffenberg, J.</au><au>Bai, X.</au><au>Baker, Mark D.</au><au>Barwick, S. W.</au><au>Bay, R.</au><au>Bazo Alba, J. L.</au><au>Beattie, K.</au><au>Beatty, J. J.</au><au>Bechet, S.</au><au>Becker, J. K.</au><au>Becker, K.-H.</au><au>Benabderrahmane, M. L.</au><au>Berdermann, J.</au><au>Berghaus, P.</au><au>Berley, D.</au><au>Bernardini, E.</au><au>Bertrand, D.</au><au>Besson, D. Z.</au><au>Bissok, M.</au><au>Blaufuss, E.</au><au>Boersma, D. J.</au><au>Bohm, C.</au><au>Böser, S.</au><au>Botner, O.</au><au>Bradley, L.</au><au>Braun, J.</au><au>Buitink, S.</au><au>Carson, M.</au><au>Chirkin, D.</au><au>Christy, B.</au><au>Clem, J.</au><au>Clevermann, F.</au><au>Cohen, S.</au><au>Colnard, C.</au><au>Cowen, D. F.</au><au>d'Agostino, M. V.</au><au>Danninger, M.</au><au>Davis, J. C.</au><au>de Clercq, C.</au><au>Demirörs, L.</au><au>Depaepe, O.</au><au>Descamps, F.</au><au>Desiati, P.</au><au>de Vries-Uiterweerd, G.</au><au>Deyoung, T.</au><au>Díaz-Vélez, J. C.</au><au>Dreyer, J.</au><au>Dumm, J. P.</au><au>Duvoort, M. R.</au><au>Ehrlich, R.</au><au>Eisch, J.</au><au>Ellsworth, R. W.</au><au>Engdegård, O.</au><au>Euler, S.</au><au>Evenson, P. A.</au><au>Fadiran, O.</au><au>Fazely, A. R.</au><au>Feusels, T.</au><au>Filimonov, K.</au><au>Finley, C.</au><au>Foerster, M. M.</au><au>Fox, B. D.</au><au>Franckowiak, A.</au><au>Franke, R.</au><au>Gaisser, T. K.</au><au>Gallagher, J.</au><au>Ganugapati, R.</au><au>Geisler, M.</au><au>Gerhardt, L.</au><au>Gladstone, L.</au><au>Glüsenkamp, T.</au><au>Goldschmidt, A.</au><au>Goodman, J. A.</au><au>Grant, D.</au><au>Griesel, T.</au><au>Gross, A.</au><au>Grullon, S.</au><au>Gunasingha, R. M.</au><au>Gurtner, M.</au><au>Ha, C.</au><au>Hallgren, A.</au><au>Halzen, F.</au><au>Han, K.</au><au>Hanson, K.</au><au>Helbing, K.</au><au>Herquet, P.</au><au>Hickford, S.</au><au>Hill, G. C.</au><au>Hoffman, K. D.</au><au>Homeier, A.</au><au>Hoshina, K.</au><au>Hubert, D.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Search for neutrino-induced cascades with five years of AMANDA data</atitle><jtitle>Astroparticle physics</jtitle><date>2011-01</date><risdate>2011</risdate><volume>34</volume><spage>420</spage><epage>430</epage><pages>420-430</pages><issn>0927-6505</issn><abstract>We report on the search for electromagnetic and hadronic showers ("cascades") produced by a diffuse flux of extraterrestrial neutrinos in the AMANDA neutrino telescope. Data for this analysis were recorded during 1001 days of detector livetime in the years 2000-2004. The observed event rates are consistent with the background expectation from atmospheric neutrinos and muons. An upper limit is derived for the diffuse flux of neutrinos of all flavors assuming a flavor ratio of νe:νμ:ντ = 1:1:1 at the detection site. The all-flavor flux of neutrinos with an energy spectrum Φ ∝ E-2 is less than 5.0 × 10-7 GeV s-1 sr-1 cm-2 at a 90% C.L. Here, 90% of the simulated signal would fall within the energy range 40 TeV to 9 PeV. We discuss flux limits in the context of several specific models of extraterrestrial and prompt atmospheric neutrino production.</abstract><pub>Elsevier</pub><doi>10.1016/J.ASTROPARTPHYS.2010.10.007</doi><orcidid>https://orcid.org/0000-0003-3108-1141</orcidid><orcidid>https://orcid.org/0000-0003-2636-5000</orcidid><orcidid>https://orcid.org/0000-0001-5634-0766</orcidid><orcidid>https://orcid.org/0000-0002-5481-5040</orcidid><orcidid>https://orcid.org/0000-0003-3108-1141</orcidid></addata></record> |
fulltext | fulltext |
identifier | ISSN: 0927-6505 |
ispartof | Astroparticle physics, 2011-01, Vol.34, p.420-430 |
issn | 0927-6505 |
language | eng |
recordid | cdi_hal_primary_oai_HAL_in2p3_00706906v1 |
source | ScienceDirect Journals (5 years ago - present) |
subjects | Astrophysics Cosmology and Extra-Galactic Astrophysics High Energy Astrophysical Phenomena Physics Sciences of the Universe |
title | Search for neutrino-induced cascades with five years of AMANDA data |
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