A Comptonized spectrum of Hua & Titarchuk (1994) with reflection from Magdziarz & Zdziarski (MNRAS, 273, 837; 1995). The output spectrum is the sum of the Comptonization spectrum and the reflection component. The Comptonization spectrum is computed as in Hua & Titarchuk (1994) for both optically thick and optically thin case. The transition between the two regimes is in general not continuous. Note that the optically thick Comptonized spectrum of Hua & Titarchuk contains an unphysical kink at a few kT. Use at your own risk. The asymptotic low-energy spectral index is used as a parameter instead of the geometry-dependent optical depth. The reflection component alone can be obtained for rel_refl < 0. Then the actual reflection normalization is |rel_refl|. Note that you need to change then the limits of rel_refl excluding zero (as then the direct component appears). The abundances and opacities are as in pexrav. Send questions or comments to aaz@camk.edu.pl.
par1 = Temperature in keVpar2 = photon spectral index
par3 = scale, scaling factor for reflection; if < 0, no direct component
(scale=1 for isotropic source above disk)
par4 = redshift, z
par5 = abundance of elements heavier than He relative to the solar
abundance.
par6 = iron abundance relative to the solar iron abundance (7.52)
par7 = cosine of inclination angle
K = The photon flux at 1 keV (photons/keV/cm
/s) of the
incident spectrum only (without reflection) and in the earth frame.