Improved Characterization of the Astrophysical Muon–neutrino Flux with 9.5 Years of IceCube Data-Reference-Cited by-同舟云学术

Improved Characterization of the Astrophysical Muon–neutrino Flux with 9.5 Years of IceCube Data

Published:2022-03-01 Issue:1 Volume:928 Page:50
ISSN:0004-637X
Container-title:The Astrophysical Journal
language:
Short-container-title:ApJ

Author:

Abbasi R.^ORCID,Ackermann M.^ORCID,Adams J.,Aguilar J. A.^ORCID,Ahlers M.^ORCID,Ahrens M.,Alameddine J. M.^ORCID,Alispach C.,Alves Jr. A. A.,Amin N. M.,Andeen K.,Anderson T.,Anton G.^ORCID,Argüelles C.^ORCID,Ashida Y.,Axani S.,Bai X.,Balagopal V. A.^ORCID,Barbano A.^ORCID,Barwick S. W.^ORCID,Bastian B.,Basu V.^ORCID,Baur S.^ORCID,Bay R.,Beatty J. J.^ORCID,Becker K.-H.^ORCID,Tjus J. Becker,Bellenghi C.,BenZvi S.^ORCID,Berley D.,Bernardini E.^ORCID,Besson D. Z.,Binder G.,Bindig D.,Blaufuss E.^ORCID,Blot S.^ORCID,Boddenberg M.,Bontempo F.,Borowka J.,Böser S.^ORCID,Botner O.^ORCID,Böttcher J.,Bourbeau E.,Bradascio F.^ORCID,Braun J.,Brinson B.,Bron S.,Brostean-Kaiser J.,Browne S.,Burgman A.^ORCID,Burley R. T.,Busse R. S.,Campana M. A.^ORCID,Carnie-Bronca E. G.,Chen C.^ORCID,Chen Z.,Chirkin D.^ORCID,Choi K.,Clark B. A.^ORCID,Clark K.^ORCID,Classen L.,Coleman A.^ORCID,Collin G. H.,Conrad J. M.^ORCID,Coppin P.^ORCID,Correa P.^ORCID,Cowen D. F.,Cross R.^ORCID,Dappen C.,Dave P.^ORCID,De Clercq C.^ORCID,DeLaunay J. J.^ORCID,López D. Delgado^ORCID,Dembinski H.^ORCID,Deoskar K.,Desai A.^ORCID,Desiati P.^ORCID,de Vries K. D.^ORCID,de Wasseige G.^ORCID,de With M.,DeYoung T.^ORCID,Diaz A.^ORCID,Díaz-Vélez J. C.^ORCID,Dittmer M.,Dujmovic H.^ORCID,Dunkman M.,DuVernois M. A.^ORCID,Dvorak E.,Ehrhardt T.,Eller P.^ORCID,Engel R.,Erpenbeck H.,Evans J.,Evenson P. A.,Fan K. L.,Fazely A. R.^ORCID,Feigl N.,Fiedlschuster S.,Fienberg A. T.,Filimonov K.,Finley C.^ORCID,Fischer L.,Fox D.^ORCID,Franckowiak A.^ORCID,Friedman E.,Fritz A.,Fürst P.^ORCID,Gaisser T. K.^ORCID,Gallagher J.,Ganster E.^ORCID,Garcia A.^ORCID,Garrappa S.^ORCID,Gerhardt L.,Ghadimi A.^ORCID,Glaser C.,Glauch T.^ORCID,Glüsenkamp T.^ORCID,Gonzalez J. G.,Goswami S.,Grant D.,Grégoire T.,Griswold S.^ORCID,Günther C.,Gutjahr P.^ORCID,Haack C.,Hallgren A.^ORCID,Halliday R.,Halve L.^ORCID,Halzen F.^ORCID,Minh M. Ha,Hanson K.,Hardin J.,Harnisch A. A.,Haungs A.^ORCID,Hebecker D.,Helbing K.^ORCID,Henningsen F.^ORCID,Hettinger E. C.,Hickford S.,Hignight J.,Hill C.^ORCID,Hill G. C.,Hoffman K. D.,Hoffmann R.,Hokanson-Fasig B.,Hoshina K.,Huang F.^ORCID,Huber M.,Huber T.^ORCID,Hultqvist K.,Hünnefeld M.,Hussain R.,Hymon K.,In S.,Iovine N.^ORCID,Ishihara A.,Jansson M.,Japaridze G. S.^ORCID,Jeong M.,Jin M.,Jones B. J. P.^ORCID,Kang D.^ORCID,Kang W.^ORCID,Kang X.,Kappes A.^ORCID,Kappesser D.,Kardum L.,Karg T.^ORCID,Karl M.^ORCID,Karle A.^ORCID,Katz U.^ORCID,Kauer M.^ORCID,Kellermann M.,Kelley J. L.^ORCID,Kheirandish A.^ORCID,Kin K.,Kintscher T.,Kiryluk J.,Klein S. R.^ORCID,Koirala R.^ORCID,Kolanoski H.^ORCID,Kontrimas T.,Köpke L.,Kopper C.^ORCID,Kopper S.,Koskinen D. J.^ORCID,Koundal P.^ORCID,Kovacevich M.^ORCID,Kowalski M.^ORCID,Kozynets T.,Kun E.,Kurahashi N.^ORCID,Lad N.,Gualda C. Lagunas^ORCID,Lanfranchi J. L.,Larson M. J.^ORCID,Lauber F.^ORCID,Lazar J. P.^ORCID,Lee J. W.,Leonard K.^ORCID,Leszczyńska A.^ORCID,Li Y.,Lincetto M.,Liu Q. R.^ORCID,Liubarska M.,Lohfink E.,Mariscal C. J. Lozano,Lu L.^ORCID,Lucarelli F.^ORCID,Ludwig A.^ORCID,Luszczak W.^ORCID,Lyu Y.^ORCID,Ma W. Y.^ORCID,Madsen J.^ORCID,Mahn K. B. M.,Makino Y.,Mancina S.,Mariş I. C.^ORCID,Martinez-Soler I.,Maruyama R.^ORCID,Mase K.,McElroy T.,McNally F.^ORCID,Mead J. V.,Meagher K.^ORCID,Mechbal S.,Medina A.,Meier M.^ORCID,Meighen-Berger S.^ORCID,Micallef J.,Mockler D.,Montaruli T.^ORCID,Moore R. W.^ORCID,Morse R.,Moulai M.^ORCID,Naab R.^ORCID,Nagai R.^ORCID,Naumann U.,Necker J.^ORCID,Nguyễn L. V.,Niederhausen H.^ORCID,Nisa M. U.^ORCID,Nowicki S. C.,Pollmann A. Obertacke^ORCID,Oehler M.,Oeyen B.^ORCID,Olivas A.,O’Sullivan E.^ORCID,Pandya H.^ORCID,Pankova D. V.,Park N.^ORCID,Parker G. K.,Paudel E. N.^ORCID,Paul L.,de los Heros C. Pérez^ORCID,Peters L.,Peterson J.,Philippen S.,Pieper S.,Pittermann M.,Pizzuto A.^ORCID,Plum M.^ORCID,Popovych Y.,Porcelli A.^ORCID,Rodriguez M. Prado,Price P. B.,Pries B.,Przybylski G. T.,Raab C.^ORCID,Raissi A.,Rameez M.^ORCID,Rawlins K.,Rea I. C.,Rehman A.^ORCID,Reichherzer P.,Reimann R.^ORCID,Renzi G.,Resconi E.^ORCID,Reusch S.,Rhode W.^ORCID,Richman M.,Riedel B.^ORCID,Roberts E. J.,Robertson S.,Roellinghoff G.,Rongen M.^ORCID,Rott C.^ORCID,Ruhe T.,Ryckbosch D.,Cantu D. Rysewyk^ORCID,Safa I.^ORCID,Saffer J.,Herrera S. E. Sanchez,Sandrock A.^ORCID,Sandroos J.^ORCID,Santander M.^ORCID,Sarkar S.^ORCID,Sarkar S.^ORCID,Satalecka K.^ORCID,Schaufel M.,Schieler H.,Schindler S.,Schmidt T.,Schneider A.^ORCID,Schneider J.^ORCID,Schröder F. G.^ORCID,Schumacher L.,Schwefer G.,Sclafani S.^ORCID,Seckel D.,Seunarine S.,Sharma A.,Shefali S.,Silva M.^ORCID,Skrzypek B.,Smithers B.^ORCID,Snihur R.,Soedingrekso J.,Soldin D.,Spannfellner C.,Spiczak G. M.^ORCID,Spiering C.^ORCID,Stachurska J.,Stamatikos M.,Stanev T.,Stein R.^ORCID,Stettner J.^ORCID,Steuer A.,Stezelberger T.^ORCID,Stürwald T.,Stuttard T.^ORCID,Sullivan G. W.^ORCID,Taboada I.^ORCID,Ter-Antonyan S.^ORCID,Tilav S.,Tischbein F.,Tollefson K.^ORCID,Tönnis C.,Toscano S.^ORCID,Tosi D.,Trettin A.,Tselengidou M.,Tung C. F.^ORCID,Turcati A.,Turcotte R.,Turley C. F.^ORCID,Twagirayezu J. P.,Ty B.,Elorrieta M. A. Unland^ORCID,Valtonen-Mattila N.,Vandenbroucke J.^ORCID,van Eijndhoven N.^ORCID,Vannerom D.,van Santen J.^ORCID,Verpoest S.^ORCID,Walck C.,Watson T. B.^ORCID,Weaver C.^ORCID,Weigel P.,Weindl A.,Weiss M. J.,Weldert J.,Wendt C.^ORCID,Werthebach J.,Weyrauch M.,Whitehorn N.^ORCID,Wiebusch C. H.^ORCID,Williams D. R.,Wolf M.^ORCID,Woschnagg K.,Wrede G.,Wulff J.,Xu X. W.,Yanez J. P.,Yoshida S.^ORCID,Yu S.,Yuan T.^ORCID,Zhang Z.,Zhelnin P.

Abstract

Abstract We present a measurement of the high-energy astrophysical muon–neutrino flux with the IceCube Neutrino Observatory. The measurement uses a high-purity selection of 650k neutrino-induced muon tracks from the northern celestial hemisphere, corresponding to 9.5 yr of experimental data. With respect to previous publications, the measurement is improved by the increased size of the event sample and the extended model testing beyond simple power-law hypotheses. An updated treatment of systematic uncertainties and atmospheric background fluxes has been implemented based on recent models. The best-fit single power-law parameterization for the astrophysical energy spectrum results in a normalization of

ϕ @ 100 TeV ν μ + ν ¯ μ = 1.44 − 0.26 + 0.25 × 10 − 18 GeV − 1 cm − 2 s − 1 sr − 1

and a spectral index

γ SPL = 2.37 − 0.09 + 0.09

, constrained in the energy range from 15 TeV to 5 PeV. The model tests include a single power law with a spectral cutoff at high energies, a log-parabola model, several source-class-specific flux predictions from the literature, and a model-independent spectral unfolding. The data are consistent with a single power-law hypothesis, however, spectra with softening above one PeV are statistically more favorable at a two-sigma level.

Publisher

American Astronomical Society

Subject

Space and Planetary Science,Astronomy and Astrophysics

Link

https://iopscience.iop.org/article/10.3847/1538-4357/ac4d29/pdf

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