Hydrodynamics of galaxy mergers with supermassive black holes: is there a last parsec problem ?

TL;DR

This study uses high-resolution simulations to investigate the dynamics of supermassive black hole binaries during galaxy mergers, revealing the challenges in their inward migration at sub-parsec scales due to reduced dynamical friction.

Contribution

First detailed AMR simulation resolving black hole separation down to 0.1 pc, confirming the last parsec problem in gas-rich galaxy mergers.

Findings

Black holes sink rapidly to 1 pc within 10 million years.

Dynamical friction becomes ineffective below 1 pc due to subsonic velocities.

Gas torques do not significantly aid black hole pairing at small scales.

Abstract

We study the formation of a supermassive black hole (SMBH) binary and the shrinking of the separation of the two holes to sub-pc scales starting from a realistic major merger between two gas-rich spiral galaxies with mass comparable to our Milky Way. The simulations, carried out with the Adaptive Mesh Refinement (AMR) code RAMSES, are capable of resolving separations as small as 0.1 pc. The collision of the two galaxies produces a gravo-turbulent rotating nuclear disk with mass (10^9 Msun) and size (60 pc) in excellent agreement with previous SPH simulations with particle splitting that used a similar setup (Mayer et al. 2007) but were limited to separations of a few parsecs. The AMR results confirm that the two black holes sink rapidly as a result of dynamical friction onto the gaseous background, reaching a separation of 1 pc in less than 10^7 yr. We show that the dynamical friction wake is well resolved by our model and we find good agreement with analytical predictions of the drag force as a function of the Mach number. Below 1 pc, black hole pairing slows down significantly, as the relative velocity between the sinking SMBH becomes highly subsonic and the mass contained within their orbit falls below the mass of the binary itself, rendering dynamical friction ineffective. In this final stage, the black holes have not opened a gap as the gaseous background is highly pressurized in the center. Non-axisymmetric gas torques do not arise to restart sinking in absence of efficient dynamical friction, at variance with previous calculations using idealized equilibrium nuclear disk models. (abridged)