Study of the Polarized X-Ray Reflection Spectrum from the Black Hole Accretion Disk and TES Detectors for Future X-Ray Balloon-Borne Missions

The polarized radiative transfer equation (PRTE) deals with the Compton scattering of the radiation by the elections in the accretion disk. The scattering part of the PRTE contains all the information of the photon momentum change due to the Compton scattering. In current reflection models, the electron scattering and its effect in the reflected spectrum is done in an approximated way based on a simple redistribution function. This approximation is accurate at relatively low temperatures and for photon energies (E<< mec2= 511 keV). However, at higher energies and temperatures show significant discrepancies and need to use different approximation. We are going to use the exact expression of the RFs from Poutanen paper (Poutanen 1993), which includes Klein-Nishina corrections, as well as relativistic corrections that become important at high temperatures. Our present work will be applicable for an accretion disk with high electron energies and temperature and to study and analyze the Fe-Kα line from the future X-ray mission i.e., NASA’s IXPE and XL-Calibur. Besides this, I will talk on the lab works on NIST developed Transition edge sensor detector for a future X-ray balloon flight.