kyconv: convolution using a relativistic line from axisymmetric accretion disk

Convolution using as a kernel the relativistic line from an axisymmetic accretion disk. See Dovciak et al. (2004).

par1 | a/M; BH angular momentum (GM/c) |

par2 | theta_o; observer inclination (0 = pole on, degrees) |

par3 | rin; inner radius (GM/c) |

par4 | ms; 0 means integrate from rin, 1 means integrate emission from above the marginally stable orbit only |

par5 | rout; outer radius (GM/c) |

par6 | alpha; accretion disk emissivity scales as for |

par7 | beta; accretion disk emissivity scales as for |

par8 | rb; boundary radius between inner and outer emissivity laws (GM/c) |

par9 | zshift; overall Doppler shift |

par10 | limb; 0 means isotropic emission, 1 means Laor's limb darkening (), 2 means Haardt's limb brightening ( |

par11 | ne_loc; number of grid points in local energy (energy resolution of local flux, the grid is equidistant in logarithmic scale) |

par12 | normal; 0 means normalize total flux to unity, +ve value means normalize to unity at the energy given by the parametervalue, -ve value means unnormalized. |