# Modeling the Spectral Energy Distribution of the radio galaxy IC310

## TL;DR

This study models the spectral energy distribution of the radio galaxy IC310 using both leptonic and hadronic frameworks, explaining multiwavelength data and TeV gamma-ray emissions, and assesses its neutrino and cosmic ray contributions.

## Contribution

It introduces a combined leptonic and hadronic modeling approach for IC310's SED, highlighting the limitations of each model and providing insights into particle interactions in active galactic nuclei.

## Key findings

- Leptonic model requires an exceedingly high electron Lorentz factor (~10^5).
- Hadronic model's proton luminosity is around 10^44 erg/s, feasible under charge neutrality.
- IC310's contribution to observed neutrino and cosmic ray fluxes is negligible.

## Abstract

The radio galaxy IC310 located in the Perseus Cluster is one of the brightest objects in the radio and X-ray bands, and one of the closest active galactic nuclei observed in very-high energies. In GeV - TeV $\gamma$-rays, IC310 was detected in low and high flux states by the MAGIC telescopes from October 2009 to February 2010. Taking into account that the spectral energy distribution (SED) up to a few GeV seems to exhibit a double-peak feature and that a single-zone synchrotron self-Compton (SSC) model can explain all of the multiwavelength emission except for the non-simultaneous MAGIC emission, we interpret, in this work, the multifrequency data set of the radio galaxy IC310 in the context of homogeneous hadronic and leptonic models. In the leptonic framework, we present a multi-zone SSC model with two electron populations to explain the whole SED whereas for the hadronic model, we propose that a single-zone SSC model describes the SED up to a few GeVs and neutral pion decay products resulting from p$\gamma$ interactions could describe the TeV - GeV $\gamma$-ray spectra. These interactions occur when Fermi-accelerated protons interact with the seed photons around the SSC peaks. We show that, in the leptonic model the minimum Lorentz factor of second electron population is exceedingly high $\gamma_e\sim10^5$ disfavoring this model, and in the hadronic model the required proton luminosity is not extremely high $\sim 10^{44}$ erg/s, provided that charge neutrality between the number of electrons and protons is given. Correlating the TeV $\gamma$-ray and neutrino spectra through photo-hadronic interactions, we find that the contribution of the emitting region of IC310 to the observed neutrino and ultra-high-energy cosmic ray fluxes are negligible.