Convolves the current spectrum with the line shape from the kerrdisk model. A detailed description can be found in Brenneman & Reynolds (2006). This model is quite slow so is best used after models such as laor or diskline have been employed to get an estimate of the best-fit parameters.
Note that due to the energy binning the convolution process can produce spurious structures around sharp features in the spectrum being convolved. We strongly recommend testing for this by using the energies command to change the binning.
|par1||emissivity index for the inner disk|
|par2||emissivity index for the outer disk|
|par3||break radius separating the inner and outer portions of the disk (gravitational radii)|
|par4||dimensionless black hole spin|
|par5||disk inclination angle to the line of sight (degrees)|
|par6||inner radius of the disk in units of the radius of marginal stability|
|par7||outer radius of the disk in units of the radius of marginal stability|