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 ![]() ![]() |
par7 | beta; accretion disk emissivity scales as ![]() ![]() |
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 (![]() ![]() |
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. |