Based on the dynamical black hole ( BH ) mass estimates , NGC3115 hosts the closest billion solar mass BH .
Deep studies of the center revealed a very underluminous active galactic nucleus ( AGN ) immersed in an old massive nuclear star cluster .
Recent 1 Ms Chandra X-ray visionary project observations of the NGC3115 nucleus resolved hot tenuous gas , which fuels the AGN .
In this paper we connect the processes in the nuclear star cluster with the feeding of the supermassive BH .
We model the hot gas flow sustained by the injection of matter and energy from the stars and supernova explosions .
We incorporate electron heat conduction as the small-scale feedback mechanism , the gravitational pull of the stellar mass , cooling , and Coulomb collisions .
Fitting simulated X-ray emission to the spatially and spectrally resolved observed data , we find the best-fitting solutions with \chi ^ { 2 } / { dof } = 1.00 for { dof } = 236 both with and without conduction .
The radial modeling favors a low BH mass < 1.3 \times 10 ^ { 9 } M _ { \odot } .
The best-fitting supernova rate and the best-fitting mass injection rate are consistent with their expected values .
The stagnation point is at r _ { st } \lesssim 1 arcsec , so that most of gas , including the gas at a Bondi radius r _ { B } = 2 - 4 arcsec , outflows from the region .
We put an upper limit on the accretion rate at 2 \times 10 ^ { -3 } M _ { \odot } { yr } ^ { -1 } .
We find a shallow density profile n \propto r ^ { - \beta } with \beta \approx 1 over a large dynamic range .
This density profile is determined in the feeding region 0.5 - 10 arcsec as an interplay of four processes and effects : ( 1 ) the radius-dependent mass injection , ( 2 ) the effect of the galactic gravitational potential , ( 3 ) the accretion flow onset at r \lesssim 1 arcsec , and ( 4 ) the outflow at r \gtrsim 1 arcsec .
The gas temperature is close to the virial temperature T _ { v } at any radius .