Context : We analyze 134 ks Chandra ACIS-I observations of the Galactic Centre ( GC ) performed in July 2011 .
The X-ray image with the field of view 17 ^ { \prime } \times 17 ^ { \prime } contains the hot plasma surrounding the Sgr A* .
The obtained surface brightness map allow us to fit Bondi hot accretion flow to the innermost hot plasma around the GC .

Aims : Contrary to the XMM-Newton data where strong 6.4 keV iron line was observed and interpreted as a reflection from molecular clouds , we search here for the diffuse X-ray emission with prominent 6.69 keV iron line .
The surface brightness profile found by us allowed to determine the stagnation radius of the flow around Sgr A* .

Methods : We have fitted spectra from region up to 5 ^ { \prime \prime } from Sgr A* using a thermal bremsstrahlung model and four Gaussian profiles responsible for K _ { \alpha } emission lines of Fe , S , Ar , and Ca .
The X-ray surface brightness profile up to 3 ^ { \prime \prime } from Sgr A* found in our data image , was successfully fitted with the dynamical model of Bondi spherical accretion .

Results : We show that the temperature of the hot plasma derived from our spectral fitting is of the order of 2.2-2.7 keV depending on the choice of background .
By modelling the surface brightness profile , we derived the temperature and number density profiles in the vicinity of the black hole .
The best fitted model of spherical Bondi accretion shows that this type of flow works only up to 3 ^ { \prime \prime } and implies outer plasma density and temperature to be : n _ { e } ^ { out } = 18.3 \pm { 0.1 } cm ^ { -3 } and T _ { e } ^ { out } = 3.5 \pm { 0.3 } keV respectively .

Conclusions : We show that the Bondi flow can reproduce observed surface brightness profile up to 3 ^ { \prime \prime } from Sgr A* in the Galactic Center .
This result strongly suggests the position of stagnation radius in the complicated dynamics around GC .
The temperature at the outer radius of the flow is higher by 1 keV , than this found by our spectral fitting of thermal plasma within the circle of 5 ^ { \prime \prime } .
The Faraday rotation computed from our model towards the pulsar PSR J1745-2900 near the GC agrees with the observed one , recently reported .
We speculate here , that the emission lines observed in spectra up to 5 ^ { \prime \prime } can be interpreted as the reflection of the radiation from two-phase regions occurring at distances between 3 - 5 ^ { \prime \prime } of the flow .
The hot plasma in Sgr A* illuminated in the past by strong radiation field may be a seed for thermal instabilities and eventual strong clumpiness .