Galactic and Extragalactic Analysis of the Astrophysical Muon Neutrino Flux with 12.3 years of IceCube Track Data. (arXiv:2308.08233v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Furst_P/0/1/0/all/0/1">Philipp F&#xfc;rst</a> (for the IceCube Collaboration)

The Ice Cube Neutrino Observatory has been measuring an isotropic
astrophysical neutrino flux in multiple detection channels for almost a decade.
Galactic diffuse emission, which arises from the interactions between cosmic
rays and the interstellar medium, is an expected signal in IceCube. The
superposition of an extragalactic flux and a galactic flux results in
directional structure and variations in the spectrum. In this work, we use 12.3
years of high-purity muon-neutrino induced muon track data to perform a
dedicated search for this galactic emission, combined with a spectral
measurement of the isotropic astrophysical neutrino flux. To distinguish a
galactic component from the dominant atmospheric and isotropic astrophysical
components, the precise directional information available for muon tracks is
fully utilized in a three-dimensional forward folding likelihood fit. We test a
state-of-the-art model prediction of galactic diffuse emission based on recent
cosmic ray data (CRINGE). We fit this prediction as a template scaled by a
factor $Psi_{mathrm{CRINGE}}$, and find $2.9pm 1.1 times
Psi_{mathrm{CRINGE}}$ with a significance of $2.7sigma$ in an energy range
between 400 GeV and 60 TeV in the Northern Sky.

The Ice Cube Neutrino Observatory has been measuring an isotropic
astrophysical neutrino flux in multiple detection channels for almost a decade.
Galactic diffuse emission, which arises from the interactions between cosmic
rays and the interstellar medium, is an expected signal in IceCube. The
superposition of an extragalactic flux and a galactic flux results in
directional structure and variations in the spectrum. In this work, we use 12.3
years of high-purity muon-neutrino induced muon track data to perform a
dedicated search for this galactic emission, combined with a spectral
measurement of the isotropic astrophysical neutrino flux. To distinguish a
galactic component from the dominant atmospheric and isotropic astrophysical
components, the precise directional information available for muon tracks is
fully utilized in a three-dimensional forward folding likelihood fit. We test a
state-of-the-art model prediction of galactic diffuse emission based on recent
cosmic ray data (CRINGE). We fit this prediction as a template scaled by a
factor $Psi_{mathrm{CRINGE}}$, and find $2.9pm 1.1 times
Psi_{mathrm{CRINGE}}$ with a significance of $2.7sigma$ in an energy range
between 400 GeV and 60 TeV in the Northern Sky.

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