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EnglishLimits on the neutrino flux for a given mass [Formula presented] and annihilation channel are calculated as in Eq. (7) (page 252), with the integrated acceptances defined in Eq. (8) (page 252) as the effective area averaged over the neutrino energy. A numerical approximation of WIMP annihilation spectra, adapted from [1] with a too coarse binning, led to an overestimation of the integrated acceptances for dark-matter induced neutrino events. The spectra were replaced with a fine-binned version both in the likelihood and in the acceptances. The main change is a weaker limit for WIMP masses larger than 1 TeV/c2. Updated versions of Figs. 3–6 are provided.
| Titolo: | Erratum to “Results from the search for dark matter in the Milky Way with 9 years of data of the ANTARES neutrino telescope” (Physics Letters B (2017) 769 (249–254), (S037026931730254X), (10.1016/j.physletb.2017.03.063)) | |
| Autore/i: | Albert A.; Andre M.; Anghinolfi M.; Anton G.; Ardid M.; Aubert J. -J.; Avgitas T.; Baret B.; Barrios-Marti J.; Basa S.; Bertin V.; Biagi S.; Bormuth R.; Bourret S.; Bouwhuis M. C.; Bruijn R.; Brunner J.; Busto J.; Capone A.; Caramete L.; Carr J.; Celli S.; Chiarusi T.; Circella M.; Coelho J. A. B.; Coleiro A.; Coniglione R.; Costantini H.; Coyle P.; Creusot A.; Deschamps A.; De Bonis G.; Distefano C.; Di Palma I.; Donzaud C.; Dornic D.; Drouhin D.; Eberl T.; El Bojaddaini I.; Elsasser D.; Enzenhofer A.; Felis I.; Fusco L. A.; Galata S.; Gay P.; Geisselsoder S.; Geyer K.; Giordano V.; Gleixner A.; Glotin H.; Gozzini R.; Gregoire T.; Gracia Ruiz R.; Graf K.; Hallmann S.; van Haren H.; Heijboer A. J.; Hello Y.; Hernandez-Rey J. J.; Hossl J.; Hofestadt J.; Hugon C.; Illuminati G.; James C. W.; de Jong M.; Jongen M.; Kadler M.; Kalekin O.; Katz U.; Kiessling D.; Kouchner A.; Kreter M.; Kreykenbohm I.; Kulikovskiy V.; Lachaud C.; Lahmann R.; Lefevre D.; Leonora E.; Lotze M.; Loucatos S.; Marcelin M.; Margiotta A.; Marinelli A.; Martinez-Mora J. A.; Mathieu A.; Mele R.; Melis K.; Michael T.; Migliozzi P.; Moussa A.; Mueller C.; Nezri E.; Pavalas G. E.; Pellegrino C.; Perrina C.; Piattelli P.; Popa V.; Pradier T.; Quinn L.; Racca C.; Riccobene G.; Roensch K.; Sanchez-Losa A.; Saldana M.; Salvadori I.; Samtleben D. F. E.; Sanguineti M.; Sapienza P.; Schnabel J.; Schussler F.; Seitz T.; Sieger C.; Spurio M.; Stolarczyk T.; Taiuti M.; Tayalati Y.; Trovato A.; Tselengidou M.; Turpin D.; Tonnis C.; Vallage B.; Vallee C.; Van Elewyck V.; Vivolo D.; Vizzoca A.; Wagner S.; Wilms J.; Zornoza J. D.; Zuniga J. | |
| Autore/i Unibo: | ||
| Anno: | 2019 | |
| Rivista: | ||
| Digital Object Identifier (DOI): | http://dx.doi.org/10.1016/j.physletb.2019.05.022 | |
| Abstract: | Limits on the neutrino flux for a given mass [Formula presented] and annihilation channel are calculated as in Eq. (7) (page 252), with the integrated acceptances defined in Eq. (8) (page 252) as the effective area averaged over the neutrino energy. A numerical approximation of WIMP annihilation spectra, adapted from [1] with a too coarse binning, led to an overestimation of the integrated acceptances for dark-matter induced neutrino events. The spectra were replaced with a fine-binned version both in the likelihood and in the acceptances. The main change is a weaker limit for WIMP masses larger than 1 TeV/c2. Updated versions of Figs. 3–6 are provided. | |
| Data stato definitivo: | 2-mar-2022 | |
| Appare nelle tipologie: | 1.04 Replica / breve intervento (e simili) |
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