AGN and DSNB Neutrino Oscillation in Dark Matter Background
Abstract
The neutrino-matter interaction cause the final flavor compositions deviating from those expected in vacuum. In this work we consider neutrinos interact with ultra-light scalar dark matters ϕ (mϕ≪ 1 eV). When the neutrinos emitted from a distant source and propagate through the dark matter medium, the MSW potential in the Hamiltonian is replaced by the hypothetical νϕ effective potential. Two types of neutrino sources are adopted in our calculations. The first is point-like neutrino source, the Active Galactic Nuclei (AGN), which produce 𝒪(TeV) neutrinos primarily through charged pion decay, yielding an initial flavor ratio of (νe,νμ,ντ)=(1:2:0). We focus on two specific AGNs, NGC 1068 and TXS 0506+056 in our analysis, whose distances from Earth are much larger than the neutrino oscillation lengths. We consider the range of νϕ coupling constant such that the adiabatic condition and mean free path can be satisfied. Hence, by assuming neutrinos are produced randomly from their corona regions, we compute the averaged flavor ratio at Earth with mϕ=10,1,0.1 peV and mϕ=1,0.1,0.01 feV, generate the ternary plots of neutrino flavors, and compare the results with the IceCube present and future sensitivities. The second source considered is the Diffuse Supernova Neutrino Background (DSNB), it is an isotropic neutrino source with energy 𝒪(MeV). Applying the core-collapse simulation neutrino temperatures to the DSNB flux, we repeat the similar analysis for the DSNB with mϕ=10−22 eV, and we estimate different neutrino flavors lies in the HK/DUNE/JUNO combined sensitivities limit.
Related
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BibTeX
@misc{tseng2026dsnb,
title = {{AGN and DSNB Neutrino Oscillation in Dark Matter Background}},
author = {Po-Yan Tseng and Yu-Min Yeh},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.21768},
eprint = {2609.21768},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.21768},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - AGN and DSNB Neutrino Oscillation in Dark Matter Background
AU - Po-Yan Tseng
AU - Yu-Min Yeh
PY - 2026
DA - 2026/09/18
PB - arXiv
DO - 10.48550/arxiv.2609.21768
UR - https://arxiv.org/abs/2609.21768
AB - The neutrino-matter interaction cause the final flavor compositions deviating from those expected in vacuum. In this work we consider neutrinos interact with ultra-light scalar dark matters ϕ (m_ϕ≪ 1 eV). When the neutrinos emitted from a distant source and propagate through the dark matter medium, the MSW potential in the Hamiltonian is replaced by the hypothetical νϕ effective potential. Two types of neutrino sources are adopted in our calculations. The first is point-like neutrino source, the Active Galactic Nuclei (AGN), which produce 𝒪(TeV) neutrinos primarily through charged pion decay, yielding an initial flavor ratio of (ν_e,ν_μ,ν_τ)=(1:2:0). We focus on two specific AGNs, NGC 1068 and TXS 0506+056 in our analysis, whose distances from Earth are much larger than the neutrino oscillation lengths. We consider the range of νϕ coupling constant such that the adiabatic condition and mean free path can be satisfied. Hence, by assuming neutrinos are produced randomly from their corona regions, we compute the averaged flavor ratio at Earth with m_ϕ=10,1,0.1 peV and m_ϕ=1,0.1,0.01 feV, generate the ternary plots of neutrino flavors, and compare the results with the IceCube present and future sensitivities. The second source considered is the Diffuse Supernova Neutrino Background (DSNB), it is an isotropic neutrino source with energy 𝒪(MeV). Applying the core-collapse simulation neutrino temperatures to the DSNB flux, we repeat the similar analysis for the DSNB with m_ϕ=10^−22 eV, and we estimate different neutrino flavors lies in the HK/DUNE/JUNO combined sensitivities limit.
ER -