Search for steady point-like sources in the astrophysical muon neutrino flux with 8 years of IceCube data

被引：99

作者：

Aartsen, M. G. ^{[18
]}

Ackermann, M. ^{[56
]}

Adams, J. ^{[18
]}

Aguilar, J. A. ^{[13
]}

Ahlers, M. ^{[23
]}

Ahrens, M. ^{[48
]}

Altmann, D. ^{[27
]}

Andeen, K. ^{[38
]}

Anderson, T. ^{[53
]}

Ansseau, I. ^{[13
]}

Anton, G. ^{[27
]}

Arguelles, C. ^{[15
]}

Auffenberg, J. ^{[1
]}

Axani, S. ^{[15
]}

Backes, P. ^{[1
]}

Bagherpour, H. ^{[18
]}

Bai, X. ^{[45
]}

Barbano, A. ^{[28
]}

Barron, J. P. ^{[26
]}

Barwick, S. W. ^{[30
]}

Baum, V. ^{[37
]}

Bay, R. ^{[9
]}

Beatty, J. J. ^{[20
,21
,22
]}

Tjus, J. Becker ^{[12
]}

Becker, K. -H. ^{[55
]}

BenZvi, S. ^{[47
]}

Berley, D. ^{[19
]}

Bernardini, E. ^{[56
]}

Besson, D. Z. ^{[31
]}

Binder, G. ^{[9
,10
]}

Bindig, D. ^{[55
]}

Blaufuss, E. ^{[19
]}

Blot, S. ^{[56
]}

Bohm, C. ^{[48
]}

Boerner, M. ^{[24
]}

Bos, F. ^{[12
]}

Boeser, S. ^{[37
]}

Botner, O. ^{[54
]}

Bourbeau, E. ^{[23
]}

Bourbeau, J. ^{[35
,36
]}

Bradascio, F. ^{[56
]}

Braun, J. ^{[35
,36
]}

Bretz, H. -P. ^{[56
]}

Bron, S. ^{[28
]}

Brostean-Kaiser, J. ^{[56
]}

Burgman, A. ^{[54
]}

Busse, R. S. ^{[35
,36
]}

Carver, T. ^{[28
]}

Chen, C. ^{[6
,7
]}

Cheung, E. ^{[19
]}

机构：

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

[2] Univ Adelaide, Dept Phys, Adelaide, SA 5005, Australia

[3] Univ Alaska Anchorage, Dept Phys & Astron, 3211 Provdence Dr, Anchorage, AK 99508 USA

[4] Univ Texas Arlington, Dept Phys, 502 Yates St,Sci Hall Rm 108,POB 19059, Arlington, TX 76019 USA

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

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

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

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

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

[10] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA

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

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

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

[14] VUB, Dienst ELEM, B-1050 Brussels, Belgium

[15] MIT, Dept Phys, Cambridge, MA 02139 USA

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

[17] Chiba Univ, Inst Global Prominent Res, Chiba 2638522, Japan

[18] Univ Canterbury, Dept Phys & Astron, Private Bag 4800, Christchurch, New Zealand

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

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

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

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

[23] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark

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

[25] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA

[26] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada

[27] Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany

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

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

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

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

[32] SNOLAB, 1039 Reg Rd 24,Creighton Mine 9, Lively, ON P3Y 1N2, Canada

[33] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA

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

[35] Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA

[36] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, 1150 Univ Ave, Madison, WI 53706 USA

[37] Johannes Gutenberg Univ Mainz, Inst Phys, Staudinger Weg 7, D-55099 Mainz, Germany

[38] Marquette Univ, Dept Phys, Milwaukee, WI 53201 USA

[39] Tech Univ Munich, Phys Dept, D-85748 Garching, Germany

[40] Westfal Wilhelms Univ Munster, Inst Kernphys, D-48149 Munster, Germany

[41] Univ Delaware, Dept Phys & Astron, Bartol Res Inst, Newark, DE 19716 USA

[42] Yale Univ, Dept Phys, New Haven, CT 06520 USA

[43] Univ Oxford, Dept Phys, 1 Keble Rd, Oxford OX1 3NP, England

[44] Drexel Univ, Dept Phys, 3141 Chestnut St, Philadelphia, PA 19104 USA

[45] South Dakota Sch Mines & Technol, Phys Dept, Rapid City, SD 57701 USA

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

[47] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA

[48] Stockholm Univ, Dept Phys, Oskar Klein Ctr, S-10691 Stockholm, Sweden

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

[50] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea

来源：

EUROPEAN PHYSICAL JOURNAL C | 2019年 / 79卷 / 03期

基金：

新加坡国家研究基金会; 瑞士国家科学基金会; 美国国家科学基金会; 加拿大自然科学与工程研究理事会; 澳大利亚研究理事会; 加拿大创新基金会; 瑞典研究理事会;

关键词：

CRAB-NEBULA; ENERGY; PROPAGATION; RESOLUTION;

D O I：

10.1140/epjc/s10052-019-6680-0

中图分类号：

O412 [相对论、场论]; O572.2 [粒子物理学];

学科分类号：

摘要：

The IceCube Collaboration has observed a high-energy astrophysical neutrino flux and recently found evidence for neutrino emission from the blazar TXS 0506+056. These results open a new window into the high-energy universe. However, the source or sources of most of the observed flux of astrophysical neutrinos remains uncertain. Here, a search for steady point-like neutrino sources is performed using an unbinned likelihood analysis. The method searches for a spatial accumulation of muon-neutrino events using the very high-statistics sample of about 497,000 neutrinos recorded by IceCube between 2009 and 2017. The median angular resolution is approximate to 1 degrees at 1 TeV and improves to approximate to 0.3 degrees for neutrinos with an energy of 1 PeV. Compared to previous analyses, this search is optimized for point-like neutrino emission with the same flux-characteristics as the observed astrophysical muon-neutrino flux and introduces an improved event-reconstruction and parametrization of the background. The result is an improvement in sensitivity to the muon-neutrino flux compared to the previous analysis of approximate to 35% assuming an E-2 spectrum. The sensitivity on the muon-neutrino flux is at a level of E2dN/dE=310-13s-1. No new evidence for neutrino sources is found in a full sky scan and in an a priori candidate source list that is motivated by gamma-ray observations. Furthermore, no significant excesses above background are found from populations of sub-threshold sources. The implications of the non-observation for potential source classes are discussed.

引用

页数：19

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