Constraints on Populations of Neutrino Sources from Searches in the Directions of IceCube Neutrino Alerts

被引：8

作者：

Abbasi, R. ^{[1
]}

Ackermann, M. ^{[2
]}

Adams, J. ^{[3
,38
]}

Aggarwal, N. ^{[4
]}

Aguilar, J. A. ^{[5
]}

Ahlers, M. ^{[6
]}

Alameddine, J. M. ^{[7
]}

Alves, A. A. ^{[8
]}

Amin, N. M. ^{[9
]}

Andeen, K. ^{[10
]}

Anderson, T. ^{[11
,12
]}

Anton, G. ^{[13
]}

Arguelles, C. ^{[14
,15
]}

Ashida, Y. ^{[16
,17
]}

Athanasiadou, S. ^{[2
]}

Axani, S. N. ^{[18
]}

Bai, X. ^{[19
]}

Balagopal, A. ^{[16
,17
]}

Baricevic, M. ^{[16
,17
]}

Barwick, S. W. ^{[20
]}

Basu, V. ^{[16
,17
]}

Bay, R. ^{[21
]}

Beatty, J. J. ^{[22
,23
,24
]}

Becker, K. -H. ^{[25
]}

Tjus, J. Becker ^{[26
]}

Beise, J. ^{[27
]}

Bellenghi, C. ^{[28
]}

Benda, S. ^{[16
,17
]}

BenZvi, S. ^{[29
]}

Berley, D. ^{[30
]}

Bernardini, E. ^{[31
]}

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

Binder, G. ^{[21
,33
]}

Bindig, D. ^{[25
]}

Blaufuss, E. ^{[30
]}

Blot, S. ^{[2
]}

Bontempo, F. ^{[8
]}

Book, J. Y. ^{[14
,15
]}

Borowka, J. ^{[34
]}

Meneguolo, C. Boscolo ^{[31
]}

Boeser, S. ^{[35
]}

Botner, O. ^{[27
]}

Boettcher, J. ^{[34
]}

Bourbeau, E. ^{[6
]}

Braun, J. ^{[16
,17
]}

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

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

Burley, R. T. ^{[38
]}

Busse, R. S. ^{[39
]}

Campana, M. A. ^{[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 Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

[24] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA

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

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

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

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

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

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

[31] Univ Studi Padova, Dipartimento Fis & Astron Galileo Galilei, I-35122 Padua, PD, Italy

[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 Adelaide, Dept Phys, Adelaide, SA 5005, Australia

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

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

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

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

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

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

[45] Columbia Univ, Columbia Astrophys & Nevis Labs, New York, NY 10027 USA

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

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

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

[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 | 2023年 / 951卷 / 01期

基金：

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

关键词：

HIGH-ENERGY NEUTRINOS; FLUX; COINCIDENT; BURSTS; ORIGIN;

D O I：

10.3847/1538-4357/acd2ca

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Beginning in 2016, the IceCube Neutrino Observatory has sent out alerts in real time containing the information of high-energy (E & GSIM; 100 TeV) neutrino candidate events with moderate to high (& GSIM;30%) probability of astrophysical origin. In this work, we use a recent catalog of such alert events, which, in addition to events announced in real time, includes events that were identified retroactively and covers the time period of 2011-2020. We also search for additional, lower-energy neutrinos from the arrival directions of these IceCube alerts. We show how performing such an analysis can constrain the contribution of rare populations of cosmic neutrino sources to the diffuse astrophysical neutrino flux. After searching for neutrino emission coincident with these alert events on various timescales, we find no significant evidence of either minute-scale or day-scale transient neutrino emission or of steady neutrino emission in the direction of these alert events. This study also shows how numerous a population of neutrino sources has to be to account for the complete astrophysical neutrino flux. Assuming that sources have the same luminosity, an E (-2.5) neutrino spectrum, and number densities that follow star formation rates, the population of sources has to be more numerous than 7 x 10(-9) Mpc(-3). This number changes to 3 x 10(-7) Mpc(-3) if number densities instead have no cosmic evolution.

引用

页数：16

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