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##

reflect: reflection from neutral material

Convolution model for reflection from neutral material according to the
method of Magdziarz & Zdziarski (1995, MNRAS, 273, 837). This is a
generalization of the pexrav and bexrav models. 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. The opacities are those set by the command xsect.
As expected in AGNs, H and He are assumed to be fully ionized.

When using this model it is essential to extend the energy range over
which the model is calculated because photons at higher energies are
Compton down-scattered into the target energy range. 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 REFLECT_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 REFLECT_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
REFLECT_PRECISION eg xset REFLECT_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 |

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