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The inner kiloparsec regions surrounding sub-Eddington (luminosity less than10$^{-3}$ in Eddington units, L$_{Edd}$) supermassive black holes (BHs) oftenshow a characteristic network of dust filaments that terminate in a nuclearspiral in the central parsecs. Here we study the role and fate of thesefilaments in one of the least accreting BHs known, M31 (10$^{-7}$ L$_{Edd}$)using hydrodynamical simulations. The evolution of a streamer of gas particlesmoving under the barred potential of M31 is followed from kiloparsec distanceto the central parsecs. After an exploratory study of initial conditions, acompelling fit to the observed dust/ionized gas morphologies and line-of-sightvelocities in the inner hundreds of parsecs is produced. After several millionyears of streamer evolution, during which friction, thermal dissipation, andself-collisions have taken place, the gas settles into a disk tens of parsecswide. This is fed by numerous filaments that arise from an outer circumnuclearring and spiral toward the center. The final configuration is tightlyconstrained by a critical input mass in the streamer of several 10$^3$M$_{\odot}$ (at an injection rate of 10$^{-4}$ M$_{\odot}$ yr$^{-1}$); valuesabove or below this lead to filament fragmentation or dispersion respectively,which are not observed. The creation of a hot gas atmosphere in the region of$\sim$10$^6$ K is key to the development of a nuclear spiral during thesimulation. The final inflow rate at 1pc from the center is $\sim$1.7 $\times$10$^{-7}$ M$_{\odot}$ yr$^{-1}$, consistent with the quiescent state of the M31BH.

The Accretion Mode in Sub-Eddington Supermassive Black Holes: Getting into the Central Parsecs of Andromeda