  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 \textit{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 $<1.3\times10^{9}M_\odot$. The best-fitting supernova rate and the
best-fitting mass injection rate are consistent with their expected values. The
stagnation point is at $r_{\rm st}\lesssim1$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 $2\times10^{-3}M_\odot{\rm
yr}^{-1}$. We find a shallow density profile $n\propto r^{-\beta}$ with
$\beta\approx1$ 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
$r\lesssim1$arcsec, and (4) the outflow at $r\gtrsim1$arcsec. The gas
temperature is close to the virial temperature $T_v$ at any radius.
