SEARCHES FOR HIGH-ENERGY NEUTRINO EMISSION IN THE GALAXY WITH THE COMBINED ICECUBE-AMANDA DETECTOR

被引：8

作者：

Abbasi, R. ^{[1
,2
]}

Abdou, Y. ^{[3
]}

Ackermann, M. ^{[4
]}

Adams, J. ^{[5
]}

Aguilar, J. A. ^{[6
]}

Ahlers, M. ^{[1
,2
]}

Altmann, D. ^{[7
]}

Andeen, K. ^{[1
,2
]}

Auffenberg, J. ^{[1
,2
]}

Bai, X. ^{[8
,9
,10
]}

Baker, M. ^{[1
,2
]}

Barwick, S. W. ^{[11
]}

Baum, V. ^{[12
]}

Bay, R. ^{[13
]}

Beattie, K. ^{[14
]}

Beatty, J. J. ^{[15
,16
,17
]}

Bechet, S. ^{[18
]}

Tjus, J. Becker ^{[19
]}

Becker, K. -H. ^{[20
]}

Bell, M. ^{[21
]}

Benabderrahmane, M. L. ^{[4
]}

BenZvi, S. ^{[1
,2
]}

Berdermann, J. ^{[4
]}

Berghaus, P. ^{[4
]}

Berley, D. ^{[22
]}

Bernardini, E. ^{[4
]}

Bertrand, D. ^{[18
]}

Besson, D. Z. ^{[23
]}

Bindig, D. ^{[20
]}

Bissok, M. ^{[24
]}

Blaufuss, E. ^{[22
]}

Blumenthal, J. ^{[24
]}

Boersma, D. J. ^{[24
]}

Bohm, C. ^{[25
,26
]}

Bose, D. ^{[27
]}

Boeser, S. ^{[28
]}

Botner, O. ^{[29
]}

Brayeur, L. ^{[27
]}

Brown, A. M. ^{[5
]}

Bruijn, R. ^{[30
]}

Brunner, J. ^{[4
]}

Buitink, S. ^{[27
]}

Carson, M. ^{[3
]}

Casey, J. ^{[31
,32
]}

Casier, M. ^{[27
]}

Chirkin, D. ^{[1
,2
]}

Christy, B. ^{[22
]}

Clevermann, F. ^{[33
]}

Cohen, S. ^{[30
]}

Cowen, D. F. ^{[21
,34
]}

机构：

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

[2] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA

[3] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium

[4] DESY, D-15735 Zeuthen, Germany

[5] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand

[6] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland

[7] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany

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

[9] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA

[10] S Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA

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

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

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

[14] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA

[15] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA

[16] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA

[17] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA

[18] Univ Libre Bruxelles, Sci Fac CP230, B-1050 Brussels, Belgium

[19] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany

[20] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany

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

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

[23] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA

[24] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany

[25] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden

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

[27] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium

[28] Univ Bonn, Inst Phys, D-53115 Bonn, Germany

[29] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden

[30] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland

[31] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA

[32] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA

[33] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany

[34] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA

[35] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA

[36] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA

[37] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada

[38] Tech Univ Munich, D-85748 Garching, Germany

[39] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia

[40] Los Alamos Natl Lab, Los Alamos, NM 87545 USA

[41] Chiba Univ, Dept Phys, Chiba 2638522, Japan

[42] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA

[43] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA

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

[45] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA

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

[47] Dipartimento Fis, Sez INFN, I-70126 Bari, Italy

[48] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA

[49] Univ Oxford, Dept Phys, Oxford OX1 3NP, England

[50] Univ W Indies, Dept Phys, BB-11000 Bridgetown, Barbados

来源：

ASTROPHYSICAL JOURNAL | 2013年 / 763卷 / 01期

基金：

澳大利亚研究理事会; 美国国家科学基金会; 日本学术振兴会; 瑞士国家科学基金会; 瑞典研究理事会;

关键词：

acceleration of particles; cosmic rays; neutrinos; GAMMA-RAY EMISSION; COSMIC-RAYS; CRAB-NEBULA; STATISTICAL-ANALYSIS; TRACK RECONSTRUCTION; SUPERNOVA REMNANT; CASSIOPEIA-A; X-RAY; ACCELERATION; TEV;

D O I：

10.1088/0004-637X/763/1/33

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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.

引用

页数：18

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