The unmatched X-ray resolution of Chandra allows probing the gas flow near quiescent supermassive black holes ( BHs ) .
The radius of BH gravitational influence on gas , called the Bondi radius , is resolved in Sgr A* and NGC 3115 .
Shallow accretion flow density profiles n \propto r ^ { - \beta } with \beta = 0.7 - 1.0 were found for Sgr A* and NGC 3115 with the help of Chandra .
We construct self-consistent models with gas feeding and dynamics from near the Bondi radius to the event horizon to explain the observations .
Gas is mainly supplied to the region by hot colliding stellar winds .
Small-scale feedback such as conduction effectively flattens the density profile from steep \beta = 1.5 in a Bondi flow .
We further constrain density and temperature profiles using the observed radio/sub-mm radiation emitted near the event horizon .
We discuss the present state of our numerical model and its qualitative features , such as the role of the galactic gravitational potential and the random motion of wind-emitting stars .