SEARCHES FOR HIGH-ENERGY NEUTRINO EMISSION IN THE GALAXY WITH THE COMBINED ICECUBE-AMANDA DETECTORShow others and affiliations
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2013 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 763, article id 33Article in journal (Refereed) Published
Abstract [en]
We report on searches for neutrino sources at energies above 200 GeV in the Northern sky of the Galactic plane, using the data collected by the South Pole neutrino telescope, IceCube, and AMANDA. The Galactic region considered in this work includes the local arm toward the Cygnus region and our closest approach to the Perseus Arm. The searches are based on the data collected between 2007 and 2009. During this time AMANDA was an integrated part of IceCube, which was still under construction and operated with 22 strings (2007-2008) and 40 strings (2008-2009) of optical modules deployed in the ice. By combining the advantages of the larger IceCube detector with the lower energy threshold of the more compact AMANDA detector, we obtain an improved sensitivity at energies below similar to 10 TeV with respect to previous searches. The analyses presented here are a scan for point sources within the Galactic plane, a search optimized formultiple and extended sources in the Cygnus region, which might be below the sensitivity of the point source scan, and studies of seven pre-selected neutrino source candidates. For one of them, Cygnus X-3, a time-dependent search for neutrino emission in coincidence with observed radio and X-ray flares has been performed. No evidence of a signal is found, and upper limits are reported for each of the searches. We investigate neutrino spectra proportional to E-2 and E-3 in order to cover the entire range of possible neutrino spectra. The steeply falling E-3 neutrino spectrum can also be used to approximate neutrino energy spectra with energy cutoffs below 50 TeV since these result in a similar energy distribution of events in the detector. For the region of the Galactic plane visible in the Northern sky, the 90% confidence level muon neutrino flux upper limits are in the range E(3)dN/dE similar to 5.4-19.5 x 10(-11) TeV2 cm(-2) s(-1) for point-like neutrino sources in the energy region [180.0 GeV-20.5 TeV]. These represent the most stringent upper limits for soft-spectra neutrino sources within the Galaxy reported to date.
Place, publisher, year, edition, pages
2013. Vol. 763, article id 33
Keywords [en]
acceleration of particles cosmic rays neutrinos gamma-ray emission cosmic-rays crab-nebula statistical-analysis track reconstruction supernova remnant shock fronts cassiopeia-a cold media x-ray Astronomy & Astrophysics
Research subject
SWEDARP, IceCube
Identifiers
URN: urn:nbn:se:polar:diva-2008DOI: 10.1088/0004-637x/763/1/33OAI: oai:DiVA.org:polar-2008DiVA, id: diva2:812273
Note
ISI Document Delivery No.: 069SH Times Cited: 6 Cited Reference Count: 103 Abbasi, R. Abdou, Y. Ackermann, M. Adams, J. Aguilar, J. A. Ahlers, M. Altmann, D. Andeen, K. Auffenberg, J. Bai, X. Baker, M. Barwick, S. W. Baum, V. Bay, R. Beattie, K. Beatty, J. J. Bechet, S. Tjus, J. Becker Becker, K. -H. Bell, M. Benabderrahmane, M. L. BenZvi, S. Berdermann, J. Berghaus, P. Berley, D. Bernardini, E. Bertrand, D. Besson, D. Z. Bindig, D. Bissok, M. Blaufuss, E. Blumenthal, J. Boersma, D. J. Bohm, C. Bose, D. Boeser, S. Botner, O. Brayeur, L. Brown, A. M. Bruijn, R. Brunner, J. Buitink, S. Carson, M. Casey, J. Casier, M. Chirkin, D. Christy, B. Clevermann, F. Cohen, S. Cowen, D. F. Silva, A. H. Cruz Danninger, M. Daughhetee, J. Davis, J. C. De Clercq, C. Descamps, F. Desiati, P. de Vries-Uiterweerd, G. DeYoung, T. Diaz-Velez, J. C. Dreyer, J. Dumm, J. P. Dunkman, M. Eagan, R. Eisch, J. Ellsworth, R. W. Engdegard, O. Euler, S. Evenson, P. A. Fadiran, O. Fazely, A. R. Fedynitch, A. 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Beatty, James/D-9310-2011; Hallgren, Allan/A-8963-2013; Sarkar, Subir/G-5978-2011; Tjus, Julia/G-8145-2012; Wiebusch, Christopher/G-6490-2012; Auffenberg, Jan/D-3954-2014; Koskinen, David/G-3236-2014 Sarkar, Subir/0000-0002-3542-858X; Auffenberg, Jan/0000-0002-1185-9094; Koskinen, David/0000-0002-0514-5917 U.S. National Science Foundation-Office of Polar Programs; U.S. National Science Foundation-Physics Division, University of Wisconsin Alumni Research Foundation; Grid Laboratory of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin-Madison; Open Science Grid (OSG) infrastructure; U.S. Department of Energy, and National Energy Research Scientific Computing Center; Louisiana Optical Network Initiative (LONI) grid computing resources; National Science and Engineering Research Council of Canada; Swedish Research Council; Swedish Polar Research Secretariat; Swedish National Infrastructure for Computing (SNIC); Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF); Helmholtz Alliance for Astroparticle Physics (HAP); Deutsche Forschungsgemeinschaft (DFG); Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO Odysseus programme; Flanders Institute to encourage scientific and technological research in industry (IWT); Belgian Federal Science Policy Office (Belspo); University of Oxford, UK; Marsden Fund, New Zealand; Australian Research Council; Japan Society for the Promotion of Science (JSPS); Swiss National Science Foundation (SNSF), Switzerland We acknowledge support from the following agencies: the U.S. National Science Foundation-Office of Polar Programs, the U.S. National Science Foundation-Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin-Madison, the Open Science Grid (OSG) infrastructure; the U.S. Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; the National Science and Engineering Research Council of Canada; the Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; the German Ministry for Education and Research (BMBF), Helmholtz Alliance for Astroparticle Physics (HAP), Deutsche Forschungsgemeinschaft (DFG), Research Department of Plasmas with Complex Interactions (Bochum), Germany; the Fund for Scientific Research (FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); the University of Oxford, UK; the Marsden Fund, New Zealand; the Australian Research Council; the Japan Society for the Promotion of Science (JSPS); and the Swiss National Science Foundation (SNSF), Switzerland. 6 Iop publishing ltd Bristol Astronomy & Astrophysics
2015-05-182015-05-132017-12-04Bibliographically approved