Determine the physical origin of NGC 1275’s optical/UV and X-ray emission

Determine whether the optical/UV and X-ray photon fluxes observed from NGC 1275 are dominated by jet emission or are substantially contaminated by the host galaxy, accretion-disk–corona system, or intracluster medium.

Background

The paper compares inverse-Compton-supported pair-cascade emission with the broadband spectral energy distribution of NGC 1275. Because the source was not spatially resolved during the relevant observations, the optical/UV and X-ray measurements may include contributions from the host galaxy, the accretion-disk–corona system, and the surrounding intracluster medium. This uncertainty affects the interpretation of the cascade model because these measurements are treated as effective upper limits rather than definitive jet-emission constraints.

References

Hence, also given the misaligned nature of the source it is not entirely clear that the photon flux in these two frequency bands is dominated by emission from the jet.

— Compton-induced HE -- VHE $γ$-rays from pair cascade emissions in the SEDs of radio galaxies: NGC 1275  (2609.08787 - Ntshatsha et al., 8 Sep 2026) in Section 3, “Simulated AGN: NGC 1275”