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000293156 0247_ $$2doi$$a10.1016/j.astropartphys.2015.01.001
000293156 0247_ $$2ISSN$$a0927-6505
000293156 0247_ $$2ISSN$$a1873-2852
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000293156 037__ $$aPUBDB-2016-00321
000293156 082__ $$a540
000293156 1001_ $$aAartsen, M. G.$$b0
000293156 245__ $$aSearches for small-scale anisotropies from neutrino point sources with three years of IceCube data
000293156 260__ $$aAmsterdam [u.a.]$$bElsevier Science$$c2015
000293156 3367_ $$2DRIVER$$aarticle
000293156 3367_ $$2DataCite$$aOutput Types/Journal article
000293156 3367_ $$0PUB:(DE-HGF)16$$2PUB:(DE-HGF)$$aJournal Article$$bjournal$$mjournal$$s1472050580_23487
000293156 3367_ $$2BibTeX$$aARTICLE
000293156 3367_ $$2ORCID$$aJOURNAL_ARTICLE
000293156 3367_ $$00$$2EndNote$$aJournal Article
000293156 500__ $$a(c) Elsevier B.V. Post referee full text in progress.
000293156 520__ $$aRecently, IceCube found evidence for a diffuse signal of astrophysical neutrinos in an energy range of $/sim$ 60TeV to the PeV-scale [1]. The origin of those events, being a key to understanding the origin of cosmic rays, is still an unsolved question. So far, analyses have not succeeded to resolve the diffuse signal into point-like sources. Searches including a maximum-likelihood-ratio test, based on the reconstructed directions and energies of the detected down- and up-going neutrino candidates, were also performed on IceCube data leading to the exclusion of bright point sources. In this paper, we present two methods to search for faint neutrino point sources in three years of IceCube data, taken between 2008 and 2011. The first method is an autocorrelation test, applied separately to the northern and southern sky. The second method is a multipole analysis, which expands the measured data in the northern hemisphere into spherical harmonics and uses the resulting expansion coefficients to separate signal from background. With both methods, the results are consistent with the background expectation with a slightly more sparse spatial distribution, corresponding to an underfluctuation. Depending on the assumed number of sources, the resulting upper limit on the flux per source in the northern hemisphere for an $E^{-2}$ energy spectrum ranges from $∼1.5\cdot10^{-8} GeV/cm^{2} s^{−1}$, in the case of one assumed source, to $∼4\cdot10^{-10} GeV/cm^{2} s^{−1}$, in the case of 3500 assumed sources.
000293156 536__ $$0G:(DE-HGF)POF3-613$$a613 - Matter and Radiation from the Universe (POF3-613)$$cPOF3-613$$fPOF III$$x0
000293156 588__ $$aDataset connected to CrossRef
000293156 693__ $$0EXP:(DE-H253)IceCube-20150101$$5EXP:(DE-H253)IceCube-20150101$$eIceCube South Pole Neutrino Observatory$$x0
000293156 7001_ $$0P:(DE-H253)PIP1014130$$aAckermann, M.$$b1
000293156 7001_ $$aAdams, J.$$b2
000293156 7001_ $$aAguilar, J. A.$$b3
000293156 7001_ $$aAhlers, M.$$b4
000293156 7001_ $$aAhrens, M.$$b5
000293156 7001_ $$aAltmann, D.$$b6
000293156 7001_ $$aAnderson, T.$$b7
000293156 7001_ $$aArguelles, C.$$b8
000293156 7001_ $$aArlen, T. C.$$b9
000293156 7001_ $$aAuffenberg, J.$$b10
000293156 7001_ $$aBai, X.$$b11
000293156 7001_ $$aBarwick, S. W.$$b12
000293156 7001_ $$aBaum, V.$$b13
000293156 7001_ $$aBeatty, J. J.$$b14
000293156 7001_ $$aBecker Tjus, J.$$b15
000293156 7001_ $$aBecker, K.-H.$$b16
000293156 7001_ $$aBenZvi, S.$$b17
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000293156 7001_ $$aBerley, D.$$b19
000293156 7001_ $$0P:(DE-H253)PIP1003794$$aBernardini, E.$$b20
000293156 7001_ $$0P:(DE-HGF)0$$aBernhard, A.$$b21$$eCorresponding author
000293156 7001_ $$aBesson, D. Z.$$b22
000293156 7001_ $$aBinder, G.$$b23
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000293156 7001_ $$aBissok, M.$$b25
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000293156 7001_ $$0P:(DE-HGF)0$$aLeuermann, M.$$b159$$eCorresponding author
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