A broken power-law spectrum
multiplied by exponential high-energy cutoff, *exp(-E/E _{c}*

The output spectrum is the sum of an e-folded broken power
law and the reflection component. 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 *E _{c}*

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 BEXRAV_PRECISION eg xset BEXRAV_PRECISION 0.05. The default precision is 0.01 (ie 1%).

par1 |
, first power law photon index |

par2 |
Ebreak, break energy (keV) |

par3 |
, second power law photon index |

par4 |
Ec, the
e-folding energy in keV (if |

par5 |
relrefl, reflection scaling factor (1 for isotropic source above disk) |

par6 |
redshift, z |

par7 |
abundance of elements heavier than He relative to the solar abundances |

par8 |
iron abundance relative to the above |

par9 |
cosine of inclination angle |

norm |
photon flux at 1 keV of the cutoff broken power-law only (no reflection) in the observed frame.} |