The Disk Wind Contribution to the Gamma-Ray emission from the nearby Seyfert Galaxy GRS 1734-292

TL;DR

This paper demonstrates that AGN disk winds can produce gamma-ray emission in Seyfert galaxy GRS 1734-292, suggesting these winds are potential cosmic ray accelerators reaching ultra-high energies, supported by multi-wavelength data and models.

Contribution

It provides the first detailed multi-wavelength analysis showing AGN disk winds as a source of gamma-ray emission in a Seyfert galaxy, introducing viable lepto-hadronic models.

Findings

AGN disk wind models can explain gamma-ray emission in GRS 1734-292.

Future CTA and SWGO observations could detect TeV emission from the disk wind.

Seyfert galaxies may be significant cosmic ray accelerators.

Abstract

Radio-quiet Seyfert galaxies have been detected in GeV gamma-rays by the $Fermi$ Large Area Telescope (LAT), but the origin of much of this emission is unclear. We consider the nearby example, the Seyfert galaxy GRS 1734-292, which exhibits weak starburst and jet activities that are insufficient to explain the observed gamma-ray flux. With the first detailed multi-wavelength study of this source, we demonstrate that an active galactic nucleus (AGN) disk wind can account for its gamma-ray emission. Using a lepto-hadronic emission model based on a shocked ambient medium and a shocked wind region created by an AGN accretion disk wind, we identify two viable scenarios that are consistent with the $Fermi$-LAT data and multi-wavelength observations: a hadronic $pp$-dominated scenario and a leptonic external Compton-dominated scenario. Both of these show that future observations with the Cherenkov Telescope Array (CTA) and the Southern Wide-field Gamma-ray Observatory (SWGO) could detect TeV emission from a disk wind in GRS 1734-292. Such a detection would substantially improve our understanding of cosmic ray acceleration efficiency in AGN disk wind systems, and would establish radio-quiet Seyfert galaxies as cosmic ray accelerators capable of reaching ultra-high energies.