Active Galactic Nucleus

                                                                            (1.2) Where = increase in wavelength of the scattered photon,  over the wavelength of the incident photon, ; =Plank’s constant (=6.63×10-31Js),  = Mass of electron (=9.11×10-34), = Speed of light and = Scattering angle (Weidner and Sells, 1980).

1.5 x-ray spectroscopy

        x-ray is a very high energy photon with wavelength in the range of 0.01 to 10 nanometer corresponding to the frequency in the range 3.0×1016  to 3.0x`1019 Hz and energy in the range 1.2×102eV to 1.2×105eV. They are longer than gamma ray but shorter than UV rays.

        In x-ray spectroscopy, K  emission lines occur when an electron transits to the innermost K shell (principal quantum number 1) from 2p orbital of the second or L shell (with principal quantum number 2). This K  is the strongest x-ray spectral line for an element bombarded with sufficient energy.  The diagram shows the x-ray energy levels transition which involves in Fe K  emission in fig.1.2.

1.6 Purpose of the Study

        Over the years, the discussions of the observed asymmetries in radio-loud AGNs like FRII and quasars have agitated the minds of curious astrophysics scientists. Many researches have been geared towards the study of the asymmetries such as structural, jets, spectral index and depolarization asymmetries. They have suggested that majority of the asymmetries are due to orientation and relativistic beaming effects (Garrington, 1998; Ubachukwu et al., 2002). Observation, theoretical and statistical approaches were employed and unanimously asymmetries was established in each study. These works have not completely achieved the cause, nature and origin of the above asymmetries.