We present measurements of the Fe Kα emission line of the intermediate polar V1223 Sagittarii observed with the Suzaku satellite. The spectrum is modeled with an absorbed thermal bremsstrahlung spectrum and three Gaussians for the three components of the Fe Kα lines. We resolve the neutral or low- ionized (6.41keV), He-like (6.70keV), and H-like (7.00keV) iron lines. We also obtain a thermal continuum temperature of 25 keV, which supports a thermal origin of the hard X-rays observed from the shock heated layers of gas between the white dwarf and the shock front. Hence, we believe that the He-like and H-like lines are from the collisional plasma. On the origin of the Fe Kα fluorescence line, we find that it could be partly from reflections of hard X-rays from the white dwarf surface and the NH absorption columns. We also discuss the Fe Kα emission line as veritable tool for the probe of some astrophysical sites.

Abstract
1. INTRODUCTION
2. OBSERVATION
3. DATA ANALYSIS AND RESULTS
4. DISCUSSIONS AND CONCLUSION
    4.1. Hard X-rays from V1223 Sgr
    4.2. On the Origin of the Fe Kα Emission Line
    4.3. The 6.7 and 7.0 keV Emission Lines
    4.4. Fe Kα Emission Line as Veritable Tool for the Probe of Hot Astrophysical Sites
REFERENCES

• R. N. C. EZE(Department of Physics and Astronomy, University of Nigeria) CORRESPONDING AUTHOR
• J. U. NWAFFIAH(Department of Physics and Astronomy, University of Nigeria)