Unlike their counterparts in the distant past, present-day supermassive black holes
(SMBHs) at galaxy centers are typically very faint, particularly in
X-ray. This phenomenon is exemplified by the dimness of the SMBH at our Galactic center, Sgr A*, which has an X-ray luminosity of a few 
$10^{33}
{\rm~erg~s^{-1}}$, or a factor of $\sim 10^{11}$ lower than the
Eddington luminosity limit. Even this low X-ray luminosity was recently
proposed to be unrelated to the accretion of ambient matter by the
SMBH and instead to be largely due to emission from a putative cusp of stars at the Galactic center. Based on the 3~million second 
Chandra/ACIS-S
data, taken recently as part of the Sgr A* X-ray Visionally Program, we rule out
this proposed scenario. Instead, we find that the X-ray spectrum of
Sgr A* can be well explained by the so-called adiabatic inflow-outflow solution
(ADIOS) of a radiatively inefficient accretion flow (RIAF). In
particular, the radial density profile of the flow, tightly constrained by the X-ray data, matches the exact prediction of the solution, 
indicating that almost
all captured matter is ejected back into the surrounding medium.
There is also X-ray spectral evidence for the ejected plasma to be substantially hotter
than the initial captured matter of a typical temperature $\sim 10^7$ K.
As a result,  little is left for the flow to radiate on the way into
the SMBH. But such inflow-outflow behavior of SMBHs can have strong impact on their environments.