Searching for High-energy Neutrino Emission from Galaxy Clusters with IceCube

被引：14

作者：

Abbasi, R. ^{[1
]}

Ackermann, M. ^{[2
]}

Adams, J. ^{[3
]}

Aguilar, J. A. ^{[4
]}

Ahlers, M. ^{[5
]}

Ahrens, M. ^{[6
,7
]}

Alameddine, J. M. ^{[8
]}

Alves, A. A., Jr. ^{[9
]}

Amin, N. M. ^{[10
,11
]}

Andeen, K. ^{[12
]}

Anderson, T. ^{[13
]}

Anton, G. ^{[14
]}

Arguelles, C. ^{[15
,16
]}

Ashida, Y. ^{[17
,18
]}

Athanasiadou, S. ^{[2
]}

Axani, S. ^{[19
]}

Bai, X. ^{[20
]}

Balagopal, A. ^{[17
,18
]}

Baricevic, M. ^{[17
,18
]}

Barwick, S. W. ^{[21
]}

Basu, V ^{[17
,18
]}

Bay, R. ^{[22
]}

Beatty, J. J. ^{[23
,24
,25
]}

Becker, K-H ^{[26
]}

Tjus, J. Becker ^{[27
]}

Beise, J. ^{[28
]}

Bellenghi, C. ^{[29
]}

Benda, S. ^{[17
,18
]}

BenZvi, S. ^{[30
]}

Berley, D. ^{[31
]}

Bernardini, E. ^{[2
,69
]}

Besson, D. Z. ^{[32
]}

Binder, G. ^{[22
,33
]}

Bindig, D. ^{[26
]}

Blaufuss, E. ^{[31
]}

Blot, S. ^{[2
]}

Bontempo, F. ^{[9
]}

Book, J. Y. ^{[15
,16
]}

Borowka, J. ^{[34
]}

Boeser, S. ^{[35
]}

Botner, O. ^{[28
]}

Boettcher, J. ^{[34
]}

Bourbeau, E. ^{[5
]}

Bradascio, F. ^{[2
]}

Braun, J. ^{[17
,18
]}

Brinson, B. ^{[36
,37
]}

Bron, S. ^{[38
]}

Brostean-Kaiser, J. ^{[2
]}

Burley, R. T. ^{[39
]}

Busse, R. S. ^{[40
]}

机构：

[1] Loyola Univ Chicago, Dept Phys, Chicago, IL 60660 USA

[2] DESY, D-15738 Zeuthen, Germany

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

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

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

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

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

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

[9] Karlsruhe Inst Technol, Inst Astroparticle Phys, D-76021 Karlsruhe, Germany

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

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

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

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

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

[15] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA

[16] Harvard Univ, Lab Particle Phys & Cosmol, Cambridge, MA 02138 USA

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

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

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

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

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

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

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

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

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

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

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

[28] Uppsala Univ, Dept Phys & Astron, Box 516, SE-75120 Uppsala, Sweden

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

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

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

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

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

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

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

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

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

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

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

[40] Westfalische Withelms Univ Munster, Inst Kernphys, D-48149 Munster, Germany

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

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

[43] Sungkyunkwan Univ, Dept Phys, Suwon 16419, South Korea

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

[45] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON K7L 3N6, Canada

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

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

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

[49] Catholic Univ Louvain, Ctr Cosmol Particle Phys & Phenomenol CP3, Louvain La Neuve, Belgium

[50] Karlsruhe Inst Technol, Inst Expt Particle Phys, D-76021 Karlsruhe, Germany

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2022年 / 938卷 / 02期

基金：

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

关键词：

LARGE-SCALE STRUCTURE; GAMMA-RAY; ASTROPHYSICAL SOURCES; SHOCK-WAVES; COSMOLOGY; SPECTRUM; RADIO; FLUX; YR;

D O I：

10.3847/2041-8213/ac966b

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Galaxy clusters have the potential to accelerate cosmic rays (CRs) to ultrahigh energies via accretion shocks or embedded CR acceleration sites. The CRs with energies below the Hillas condition will be confined within the cluster and eventually interact with the intracluster medium gas to produce secondary neutrinos and gamma rays. Using 9.5 yr of muon neutrino track events from the IceCube Neutrino Observatory, we report the results of a stacking analysis of 1094 galaxy clusters with masses greater than or similar to 10(14) M (circle dot) and redshifts between 0.01 and similar to 1 detected by the Planck mission via the Sunyaev-Zel'dovich effect. We find no evidence for significant neutrino emission and report upper limits on the cumulative unresolved neutrino flux from massive galaxy clusters after accounting for the completeness of the catalog up to a redshift of 2, assuming three different weighting scenarios for the stacking and three different power-law spectra. Weighting the sources according to mass and distance, we set upper limits at a 90% confidence level that constrain the flux of neutrinos from massive galaxy clusters (greater than or similar to 10(14) M (circle dot)) to be no more than 4.6% of the diffuse IceCube observations at 100 TeV, assuming an unbroken E (-2.5) power-law spectrum.

引用

页数：10

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