We show that the Iron K emission line from MCG-6-30-15 could be broadened due to Comptonization by a surrounding highly ionized cloud with radius \sim 10 ^ { 14 } cms .
We calculate the temperature of the cloud to be \sim 0.21 { keV } , provided a reasonable estimate of the UV flux is made .
The X-ray/ \gamma -ray emission observed from the source is compatible with this model .
Such a cloud should be highly ionized and strong absorption edges are not expected from the source ( Fabian et al .
1995 ) .

For a 10 ^ { 6 } M _ { \odot } black hole the size of the could corresponds to about 300 Schwarzschild radius .
The intrinsic line could then be emitted far from the black hole and gravitational red-shift and Doppler effects would be negligible .
If the black hole mass is much larger than 10 ^ { 6 } M _ { \odot } , gravitational/Doppler red-shifts would also contribute significantly to the broadening .

We argue that the broad red wing observed in the source does not by itself imply emission from regions close ( R < 5 r _ { s } ) to the black hole .
However , Comptonization can not produce a double peak .
The presence of such a feature is a clear sign of inner disk emission influenced by gravitational and Doppler effects , perhaps broadened by the Comptonization .
We note that simultaneous broad band ( 2-100 keV ) study of this source can also reveal ( or rule out ) the presence of such a Comptonizing cloud .