Convolution model for reflection from ionized material
according to the method of Magdziarz & Zdziarski (1995, MNRAS, 273, 837).
This is a generalization of the pexriv and bexriv models. Ionization and
opacities of the reflecting medium is computed as in the absori model. The
reflection component alone can be obtained for _{}. Then the actual reflection
normalization is |*rel*_{refl}|. Note that you need to change then
the limits of _{} excluding zero (as then the
direct component appears). If _{}, there is no cutoff in the
power law. The metal and iron abundance are variable with respect to those set
by the command **abund**.

When using this model it is essential to extend the energy
range over which the model is calculated both on the high and low end. The high
end extension is required because photons at higher energies are Compton
down-scattered into the target energy range. The low energy extension may be
required to calculate ionization fractions correctly. The energy range can be
extended using the extend command. The upper limit on the energies should be
set above that for which the input spectrum has significant flux. To speed up
the model, calculation of the output spectrum can be limited to energies below
a given value by using **xset** to define IREFLECT_MAX_E (in units of keV).
For instance, suppose that the original data extends up to 100 keV. To
accurately determine the reflection it may be necessary to extend the energy
range up to 500 keV. Now to avoid calculating the output spectrum between 100
and 500 keV use the command xset IREFLECT_MAX_E 100.0.

The core of this model is a Greens' function integration with one numerical integral performed for each model energy. The numerical integration is done using an adaptive method which continues until a given estimated fractional precision is reached. The precision can be changed by setting IREFLECT_PRECISION eg xset IREFLECT_PRECISION 0.05. The default precision is 0.01 (ie 1%).

par1 |
reflection scaling factor (1 for isotropic source above disk) |

par2 = |
redshift |

par3 |
abundance of elements heavier than He relative to the solar abundances |

par4 |
iron abundance relative to the above |

par5 |
cos |

par8 |
disk temperature in |

par9 |
disk ionization parameter, |