We improve the method proposed by Yao et al ( 2003 ) to resolve the X-ray dust scattering halos of point sources .
Using this method we re-analyze the Cygnus X-1 data observed with Chandra ( ObsID 1511 ) and derive the halo radial profile in different energy bands and the fractional halo intensity ( FHI ) as I ( E ) = 0.402 \times E _ { { keV } } ^ { -2 } .
We also apply the method to the Cygnus X-3 data ( Chandra ObsID 425 ) and derive the halo radial profile from the first order data with the Chandra ACIS+HETG .
It is found that the halo radial profile could be fit by the halo model MRN ( Mathis , Rumpl \& Nordsieck , 1977 ) and WD01 ( Weingartner \& Draine , 2001 ) ; the dust clouds should be located at between 1/2 to 1 of the distance to Cygnus X-1 and between 1/6 to 3/4 ( from MRN model ) or 1/6 to 2/3 ( from WD01 model ) of the distance to Cygnus X-3 , respectively .