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##

ireflect: reflection from ionized material

Convolution model for reflection from ionized material according to the
method of Magdziarz & Zdziarski (1995). 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 .
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 energies `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=z |
redshift |

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

par4 |
iron abundance relative to the above |

par5 |
cos i, the inclination angle |

par6 |
disk temperature in K |

par7 |
disk ionization parameter,
, where
is the 5eV - 20keV irradiating flux, n is the density of the reflector;
see Done et al. (1992) |

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