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.

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))

Fusco L. A.;Migliozzi P.;
2019

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.
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/11386/4781455
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