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Background studies for acoustic neutrino detection at the South Pole |
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| Institution: | a III. Physikalisches Institut, RWTH Aachen University, D-52056 Aachen, Germany b Dept. of Physics and Astronomy, University of Alabama, Tuscaloosa, AL 35487, USA c Dept. of Physics and Astronomy, University of Alaska Anchorage, 3211 Providence Dr., Anchorage, AK 99508, USA d CTSPS, Clark-Atlanta University, Atlanta, GA 30314, USA e School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, Atlanta, GA 30332, USA f Dept. of Physics, Southern University, Baton Rouge, LA 70813, USA g Dept. of Physics, University of California, Berkeley, CA 94720, USA h Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA i Institut für Physik, Humboldt-Universität zu Berlin, D-12489 Berlin, Germany j Fakultät für Physik & Astronomie, Ruhr-Universität Bochum, D-44780 Bochum, Germany k Physikalisches Institut, Universität Bonn, Nussallee 12, D-53115 Bonn, Germany l Dept. of Physics, University of the West Indies, Cave Hill Campus, Bridgetown BB11000, Barbados m Université Libre de Bruxelles, Science Faculty CP230, B-1050 Brussels, Belgium n Vrije Universiteit Brussel, Dienst ELEM, B-1050 Brussels, Belgium o Dept. of Physics, Chiba University, Chiba 263-8522, Japan p Dept. of Physics and Astronomy, University of Canterbury, Private Bag 4800, Christchurch, New Zealand q Dept. of Physics, University of Maryland, College Park, MD 20742, USA r Dept. of Physics and Center for Cosmology and Astro-Particle Physics, Ohio State University, Columbus, OH 43210, USA s Dept. of Astronomy, Ohio State University, Columbus, OH 43210, USA t Dept. of Physics, TU Dortmund University, D-44221 Dortmund, Germany u Dept. of Physics, University of Alberta, Edmonton, Alberta, Canada T6G 2G7 v Dept. of Physics and Astronomy, University of Gent, B-9000 Gent, Belgium w Max-Planck-Institut für Kernphysik, D-69177 Heidelberg, Germany x Dept. of Physics and Astronomy, University of California, Irvine, CA 92697, USA y Laboratory for High Energy Physics, École Polytechnique Fédérale, CH-1015 Lausanne, Switzerland z Dept. of Physics and Astronomy, University of Kansas, Lawrence, KS 66045, USA aa Dept. of Astronomy, University of Wisconsin, Madison, WI 53706, USA ab Dept. of Physics, University of Wisconsin, Madison, WI 53706, USA ac Institute of Physics, University of Mainz, Staudinger Weg 7, D-55099 Mainz, Germany ad Université de Mons, 7000 Mons, Belgium ae Bartol Research Institute and Department of Physics and Astronomy, University of Delaware, Newark, DE 19716, USA af Dept. of Physics, University of Oxford, 1 Keble Road, Oxford OX1 3NP, UK ag Dept. of Physics, University of Wisconsin, River Falls, WI 54022, USA ah Oskar Klein Centre and Dept. of Physics, Stockholm University, SE-10691 Stockholm, Sweden ai Dept. of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802, USA aj Dept. of Physics, Pennsylvania State University, University Park, PA 16802, USA ak Dept. of Physics and Astronomy, Uppsala University, Box 516, S-75120 Uppsala, Sweden al Dept. of Physics, University of Wuppertal, D-42119 Wuppertal, Germany am DESY, D-15735 Zeuthen, Germany |
| Abstract: | The detection of acoustic signals from ultra-high energy neutrino interactions is a promising method to measure the flux of cosmogenic neutrinos expected on Earth. The energy threshold for this process depends strongly on the absolute noise level in the target material. The South Pole Acoustic Test Setup (SPATS), deployed in the upper part of four boreholes of the IceCube Neutrino Observatory, has monitored the noise in Antarctic ice at the geographic South Pole for more than two years down to 500 m depth. The noise is very stable and Gaussian distributed. Lacking an in situ calibration up to now, laboratory measurements have been used to estimate the absolute noise level in the 10-50 kHz frequency range to be smaller than 20 mPa. Using a threshold trigger, sensors of the South Pole Acoustic Test Setup registered acoustic events in the IceCube detector volume and its vicinity. Acoustic signals from refreezing IceCube holes and from anthropogenic sources have been used to test the localization of acoustic events. An upper limit on the neutrino flux at energies Eν > 1011 GeV is derived from acoustic data taken over eight months. |
| Keywords: | Acoustic neutrino detection Absolute noise level Neutrino flux limit |
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