Why Are AGN and Host Galaxies Misaligned?

TL;DR

This paper explains that misalignments between AGN and host galaxy angular momentum axes naturally occur due to gravitational instabilities and angular momentum exchange in gas inflows, affecting AGN feedback and black hole spin.

Contribution

It demonstrates through high-resolution simulations that AGN-host misalignments arise from gravitational modes and angular momentum exchange, challenging previous assumptions about alignment indicators.

Findings

Misalignments occur naturally in simulations with gravitational instabilities.

Resonant angular momentum exchange can flip the inner mode's spin.

Misalignments influence black hole spin and jet formation efficiency.

Abstract

It is well-established observationally that the characteristic angular momentum axis on small scales around AGN, traced by radio jets and the putative torus, is not well-correlated with the large-scale angular momentum axis of the host galaxy. In this paper, we show that such misalignments arise naturally in high-resolution simulations in which we follow angular momentum transport and inflows from galaxy to sub-pc scales near AGN, triggered either during galaxy mergers or by instabilities in isolated disks. Sudden misalignments can sometimes be caused by single massive clumps falling into the center slightly off-axis, but more generally, they arise even when the gas inflows are smooth and trace only global gravitational instabilities. When several nested, self-gravitating modes are present, the inner ones can precess and tumble in the potential of the outer modes. Resonant angular momentum exchange can flip or re-align the spin of an inner mode on a short timescale, even without the presence of massive clumps. We therefore do not expect that AGN and their host galaxies will be preferentially aligned, nor should the relative alignment be an indicator of the AGN fueling mechanism. We discuss implications of this conclusion for AGN feedback and BH spin evolution. The misalignments may mean that even BHs accreting from smooth large-scale disks will not be spun up to maximal rotation, and so have more modest radiative efficiencies and inefficient jet formation. Even more random orientations are possible if there is further, un-resolved clumpiness in the gas, and more ordered accretion may occur if the inflow is slower and not self-gravitating.