Abstract Details
| Name: Raj Prince Affiliation: Department of Physics, Banaras Hindu University, Varanasi, Uttar Pradesh Conference ID: ASI2025_259 Title : Dissecting the broad-band emission from γ-ray blazar PKS 0735+178 in search of neutrinos Authors and Co-Authors : Raj Prince^1, Saikat Das^2, Nayantara Gupta^3, Pratik Majumdar^4, and Bozena Czerny^5 Abstract Type : Poster Abstract Category : High Energy Phenomena, Fundamental Physics and Astronomy Abstract : The origin of the diffuse flux of TeV–PeV astrophysical neutrinos is still unknown. The γ -ray blazar PKS 0735+178, located outside the 90 percent localization region at 2.2deg from the best-fitting IC-211208A event, was found to be flaring across all wavebands. In addition to leptonic synchrotron (SYN) and SYN self-Compton (SSC) emission, we invoke photohadronic (pγ ) interactions inside the jet to model the spectral energy distribution (SED) and neutrino emission. We analyze the 100 d γ -ray and X-ray data and 10 d around the neutrino event are chosen to generate the broad-band SED. The temporal light curve indicates that the source was in a high state in optical, UV, γ -ray, and X-ray frequencies during the neutrino detection epoch. In the one-zone lepto-hadronic model, the SSC photons do not provide enough seed photons for pγ interactions to explain the neutrino event. However, including an external photon field yields a neutrino event rate of 0.12 in 100 d, for the IceCube detector, using physically motivated values of the magnetic field, an external photon field peaking at optical wavelength, and other jet parameters. The radiation from secondary electrons at X-ray energies severely constrains the neutrino flux to a lower value than found in previous studies. Moreover, the flux of high-energy γ -rays at GeV energies from the decay of neutral pions is sub-dominant at the high-energy peak of the SED, suggesting a higher correlation of neutrino flux with X-ray flux is plausible. I will also show the result of other possible blazar found in connection with IceCube neutrinos. |