We have extended our earlier study ( , Paper I ) of the X-ray emission emanating from the central 100 pc \times 100 pc region of our Galaxy to an investigation of several features prominent in the soft X-ray ( 2–4.5 keV ) band .
We focus on three specific structures : a putative bipolar outflow from the vicinity of Sgr A* ; a high surface brightness region located roughly 12 arcmin ( 25 pc ) to the north-east of Sgr A* ; and a lower surface-brightness extended loop feature seen to the south of Sgr A* .
We show , unequivocally , that all three structures are thermal in nature and have similar temperatures ( kT \approx 1 keV ) .
The inferred X-ray luminosities lie in the range ( 2 - 10 ) \times 10 ^ { 34 } ~ { } erg~ { } s ^ { -1 } .
In the case of the bipolar feature we suggest that the hot plasma is produced by the shock-heating of the winds from massive stars within the Central Cluster , possibly collimated by the Circumnuclear Disc .
Alternatively the outflow may be driven by outbursts on Sgr A* , which follow tidal disruption events occurring at a rate of roughly 1 every 4000 yr .
The north-east enhancement is centred on a candidate pulsar wind nebula which has a relatively hard non-thermal X-ray spectrum .
We suggest that the coincident soft-thermal emission traces the core of a new thermal-composite supernova remnant , designated as SNR G0.13-0.12 .
There is no clear evidence for an associated radio shell but such a feature may be masked by the bright emission of the nearby Radio Arc and other filamentary structures .
SNR G0.13-0.12 is very likely interacting with the nearby molecular cloud , G0.11-0.11 , and linked to the Fermi source , 2FGL J1746.4-2851c .
Finally we explore a previous suggestion that the elliptically-shaped X-ray loop to the south of Sgr A* , of maximum extent \sim 45 pc , represents the shell of a superbubble located in the GC region .
Although plausible , the interpretation of this feature in terms a coherent physical structure awaits confirmation .