The origin of the Galactic center diffuse X-ray emission ( GCDX ) is still under intense investigation .
In particular , the interpretation of the hot ( kT \approx 7 keV ) component of the GCDX , characterised by the strong Fe 6.7 keV line emission , has been contentious .
If the hot component originates from a truly diffuse interstellar plasma , not a collection of unresolved point sources , such plasma can not be gravitationally bound , and its regeneration would require a huge amount of energy .
Here we show that the spatial distribution of the GCDX does not correlate with the number density distribution of an old stellar population traced by near-infrared light , strongly suggesting a significant contribution of the diffuse interstellar plasma .
Contributions of the old stellar population to the GCDX are implied to be \sim 50 % and \sim 20 % in the Nuclear stellar disk and Nuclear star cluster , respectively .
For the Nuclear stellar disk , a scale height of 0 \fdg 32 \pm 0 \fdg 02 is obtained for the first time from the stellar number density profiles .
We also show the results of the extended near-infrared polarimetric observations in the central 3 \arcdeg \times 2 \arcdeg region of our Galaxy , and confirm that the GCDX region is permeated by a large scale , toroidal magnetic field as previously claimed .
Together with observed magnetic field strengths close to energy equipartition , the hot plasma could be magnetically confined , reducing the amount of energy required to sustain it .