Simulating AGN feedback and its evolution in galaxy mergers: case study for NGC 5252

Abstract

We are investigating the evolution of merging galaxies using numerical simulations. This research focuses on the AGN-driven feedback mechanism that can be responsible for the outflow gas found on kiloparsecs scales in Seyfert galaxies. The initial conditions of the galaxy were designed to replicate the observable characteristics of NGC 5252. NGC 5252 is an off-nucleus ultraluminous X-ray (ULX) source and has extended [OIII] emission up to 10 kpc scales. The optical spectrum properties of CXO J133815.6+043255 are comparable to those of Low-Luminosity AGNs (LLAGNs). Observations of high angular resolution very long baseline interferometry (VLBI) also showed that it is a suitable option for a dual radio-emitting AGN system. Moreover, the NGC 5252 off-nucleus component is thought to be a stripped leftover of a merging dwarf galaxy. The supermassive black hole (SMBH) physics module is used in smoothed-particle hydrodynamics (SPH) simulations of merging galaxies using the GIZMO code to investigate the evolutionary changes of such a system. Our major-merger test run could not produce the observed morphology contrary to a report that one would be able to produce a spiral galaxy. The minor-merger test run up to around 0.2-0.3 Gyr shows a promising early result of the final system however further works will be conducted to investigate the properties of the resulting double AGN system and its evolution.