Constraining the Size of the Corona with Fully Relativistic Calculations of Spectra of Extended Coronae. I. The Monte Carlo Radiative Transfer Code

The size and geometry of the X-ray emitting coronain AGNs are still not well constrained. Dovciak & Done (2016) proposed a method based on calculations assuming a point-like lamp-post corona. To perform more self-consistent calculations of energy spectra of extended coronae, we develop monk, a Monte Carlo radiative transfer code dedicated to calculations of Comptonised spectra in the Kerr spacetime. In monk we assume Klein-Nishina scattering cross section and include all general relativistic effects. We find that for a coronalocated above the disc, the spectrum is not isotropic, but with harder and less luminous spectra towards observers at lower inclinations, owing to anisotropic illumination of the seed photons. This anisotropy also leads to an underestimated size of the coronaif we assume the coronato be a point-like, isotropic source located on the black hole rotation axis, demonstrating the necessity of more self-consistent calculations. We also inspect the effect of motion and geometry of the coronaon the emergent spectrum. Finally, we discuss the implication of anisotropic coronaemission for the reflection spectrum in AGNs as well as black hole X-ray binaries(BHXRBs). We find that by assuming the coronaemission to be isotropic, one may underestimate the soft excess in AGNs and the reflection continuum and iron K fluorescent line flux in BHXRBs.