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@ARTICLE{Aartsen:293156,
author = {Aartsen, M. G. and Ackermann, M. and Adams, J. and Aguilar,
J. A. and Ahlers, M. and Ahrens, M. and Altmann, D. and
Anderson, T. and Arguelles, C. and Arlen, T. C. and
Auffenberg, J. and Bai, X. and Barwick, S. W. and Baum, V.
and Beatty, J. J. and Becker Tjus, J. and Becker, K.-H. and
BenZvi, S. and Berghaus, P. and Berley, D. and Bernardini,
E. and Bernhard, A. and Besson, D. Z. and Binder, G. and
Bindig, D. and Bissok, M. and Blaufuss, E. and Blumenthal,
J. and Boersma, D. J. and Bohm, C. and Bos, F. and Bose, D.
and Böser, S. and Botner, O. and Brayeur, L. and Bretz,
H.-P. and Brown, A. M. and Casey, J. and Casier, M. and
Cheung, E. and Chirkin, D. and Christov, A. and Christy, B.
and Clark, K. and Classen, L. and Clevermann, F. and
Coenders, S. and Cowen, D. F. and Cruz Silva, A. H. and
Danninger, M. and Daughhetee, J. and Davis, J. C. and Day,
M. and de André, J. P. A. M. and De Clercq, C. and De
Ridder, S. and Desiati, P. and de Vries, K. D. and de With,
M. and DeYoung, T. and Díaz-Vélez, J. C. and Dunkman, M.
and Eagan, R. and Eberhardt, B. and Eichmann, B. and Eisch,
J. and Euler, S. and Evenson, P. A. and Fadiran, O. and
Fazely, A. R. and Fedynitch, A. and Feintzeig, J. and Felde,
J. and Feusels, T. and Filimonov, K. and Finley, C. and
Fischer-Wasels, T. and Flis, S. and Franckowiak, A. and
Frantzen, K. and Fuchs, T. and Gaisser, T. K. and Gaior, R.
and Gallagher, J. and Gerhardt, L. and Gier, D. and
Gladstone, L. and Glüsenkamp, T. and Goldschmidt, A. and
Golup, G. and Gonzalez, J. G. and Goodman, J. A. and Góra,
D. and Grant, D. and Gretskov, P. and Groh, J. C. and Groß,
A. and Ha, C. and Haack, C. and Haj Ismail, A. and Hallen,
P. and Hallgren, A. and Halzen, F. and Hanson, K. and
Hebecker, D. and Heereman, D. and Heinen, D. and Helbing, K.
and Hellauer, R. and Hellwig, D. and Hickford, S. and Hill,
G. C. and Hoffman, K. D. and Hoffmann, R. and Homeier, A.
and Hoshina, K. and Huang, F. and Huelsnitz, W. and Hulth,
P. O. and Hultqvist, K. and Hussain, S. and Ishihara, A. and
Jacobi, E. and Jacobsen, J. and Jagielski, K. and Japaridze,
G. S. and Jero, K. and Jlelati, O. and Jurkovic, M. and
Kaminsky, B. and Kappes, A. and Karg, T. and Karle, A. and
Kauer, M. and Kelley, J. L. and Kheirandish, A. and Kiryluk,
J. and Kläs, J. and Klein, S. R. and Köhne, J.-H. and
Kohnen, G. and Kolanoski, H. and Koob, A. and Köpke, L. and
Kopper, C. and Kopper, S. and Koskinen, D. J. and Kowalski,
M. and Kriesten, A. and Krings, K. and Kroll, G. and Kroll,
M. and Kunnen, J. and Kurahashi, N. and Kuwabara, T. and
Labare, M. and Larsen, D. T. and Larson, M. J. and
Lesiak-Bzdak, M. and Leuermann, M. and Leute, J. and
Lünemann, J. and Madsen, J. and Maggi, G. and Maruyama, R.
and Mase, K. and Matis, H. S. and Maunu, R. and McNally, F.
and Meagher, K. and Medici, M. and Meli, A. and Meures, T.
and Miarecki, S. and Middell, E. and Middlemas, E. and
Milke, N. and Miller, J. and Mohrmann, L. and Montaruli, T.
and Morse, R. and Nahnhauer, R. and Naumann, U. and
Niederhausen, H. and Nowicki, S. C. and Nygren, D. R. and
Obertacke, A. and Odrowski, S. and Olivas, A. and Omairat,
A. and O’Murchadha, A. and Palczewski, T. and Paul, L. and
Penek, Ö. and Pepper, J. A. and Pérez de los Heros, C. and
Pfendner, C. and Pieloth, D. and Pinat, E. and Posselt, J.
and Price, P. B. and Przybylski, G. T. and Pütz, J. and
Quinnan, M. and Rädel, L. and Rameez, M. and Rawlins, K.
and Redl, P. and Rees, I. and Reimann, R. and Relich, M. and
Resconi, E. and Rhode, W. and Richman, M. and Riedel, B. and
Robertson, S. and Rodrigues, J. P. and Rongen, M. and Rott,
C. and Ruhe, T. and Ruzybayev, B. and Ryckbosch, D. and
Saba, S. M. and Sander, H.-G. and Sandroos, J. and
Santander, M. and Sarkar, S. and Schatto, K. and Scheriau,
F. and Schmidt, T. and Schmitz, M. and Schoenen, S. and
Schöneberg, S. and Schönwald, A. and Schukraft, A. and
Schulte, L. and Schulz, O. and Seckel, D. and Sestayo, Y.
and Seunarine, S. and Shanidze, R. and Smith, M. W. E. and
Soldin, D. and Spiczak, G. M. and Spiering, C. and
Stamatikos, M. and Stanev, T. and Stanisha, N. A. and
Stasik, A. and Stezelberger, T. and Stokstad, R. G. and
Stößl, A. and Strahler, E. A. and Ström, R. and
Strotjohann, N. L. and Sullivan, G. W. and Taavola, H. and
Taboada, I. and Tamburro, A. and Tepe, A. and Ter-Antonyan,
S. and Terliuk, A. and Tešić, G. and Tilav, S. and Toale,
P. A. and Tobin, M. N. and Tosi, D. and Tselengidou, M. and
Unger, E. and Usner, M. and Vallecorsa, S. and van
Eijndhoven, N. and Vandenbroucke, J. and van Santen, J. and
Vehring, M. and Voge, M. and Vraeghe, M. and Walck, C. and
Wallraff, M. and Weaver, Ch. and Wellons, M. and Wendt, C.
and Westerhoff, S. and Whelan, B. J. and Whitehorn, N. and
Wichary, C. and Wiebe, K. and Wiebusch, C. H. and Williams,
D. R. and Wissing, H. and Wolf, M. and Wood, T. R. and
Woschnagg, K. and Xu, D. L. and Xu, X. W. and Yanez, J. P.
and Yodh, G. and Yoshida, S. and Zarzhitsky, P. and Ziemann,
J. and Zierke, S. and Zoll, M.},
title = {{S}earches for small-scale anisotropies from neutrino point
sources with three years of {I}ce{C}ube data},
journal = {Astroparticle physics},
volume = {66},
issn = {0927-6505},
address = {Amsterdam [u.a.]},
publisher = {Elsevier Science},
reportid = {PUBDB-2016-00321},
pages = {39 - 52},
year = {2015},
note = {(c) Elsevier B.V. Post referee full text in progress.},
abstract = {Recently, 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.},
cin = {ZEU-ICE},
ddc = {540},
cid = {I:(DE-H253)ZEU-ICE-20160806},
pnm = {613 - Matter and Radiation from the Universe (POF3-613)},
pid = {G:(DE-HGF)POF3-613},
experiment = {EXP:(DE-H253)IceCube-20150101},
typ = {PUB:(DE-HGF)16},
UT = {WOS:000352045100006},
doi = {10.1016/j.astropartphys.2015.01.001},
url = {https://bib-pubdb1.desy.de/record/293156},
}
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