2024/08/22 by Wenlian Li, Li, Wenlian, Tian-Qi Huang +5 · 1 citation
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #Dark Matter and Cosmic Phenomena #FOS: Physical sciences #High Energy Astrophysical Phenomena (astro-ph.HE) #Neutrino Physics Research
paper · pdf · doi:10.48550/arxiv.2408.12123
openalex publication_date 2024/08/22 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The diffuse Galactic γ-ray emission originates from the interactions between cosmic rays and the interstellar medium or radiation fields within our Galaxy, where the production of neutrinos is also anticipated. Recently, the Large High Altitude Air Shower Observatory (LHAASO) reported measurements of diffuse γ-rays from the Galactic plane with energies ranging from sub-TeV to 1 PeV. Using publicly available 7 years of IceCube track data with the full detector, we conduct a template search using the γ-ray flux map observed by LHAASO-KM2A as the neutrino emission template and perform a scan search of the Galactic plane. In the template search, a mild excess of neutrinos is observed in the Galactic plane with a pretrial (posttrial) significance of 1.9σ (1.1σ). The measured muon neutrino intensity at 25 TeV is 4.73+2.53-2.51×10-14 \rm TeV-1 cm-2 s-1 sr-1, consistent with the expected neutrino flux assuming that all the diffuse Galactic γ-rays originate from hadronic interactions. In the Galactic plane scan search, the most significant location is found at l=63.57∘ and b=0.93∘ with a pretrial (posttrial) significance of 4.6σ (1.8σ).