The unified scheme of Seyfert galaxies hypothesizes that the observed differences between the two categories of Seyfert galaxies, type 1 (Sy1) and type 2 (Sy2) are merely due to the difference in the orientation of the toroidal shape of the obscuring material in the active galactic nuclei. We used in this paper, a sample consisting of 120 Seyfert galaxies at 1.40 × 109 Hz in radio, 2.52 × 1017 Hz in X-ray and 2.52 × 1023 Hz in γ-ray luminosities observed by the Fermi Large Area Telescope (Fermi- LAT) in order to test the unified scheme of radio-quiet Seyfert galaxies. Our main results are as follows: (i) We found that the distributions of multiwave luminosities (Lradio, LX-ray, and Lγ-ray) of Sy1 and Sy2 are completely overlapped with up to a factor of 4. The principal component analysis result reveals that Sy1 and Sy2 also occupy the same parameter spaces, which agrees with the notion that Sy1 and Sy2 are the same class objects. A Kolmogorov-Smirnov test performed on the sub-samples indicates that the null hypothesis (both are from the same population) cannot be rejected with chance probability p ~ 0 and separation distance K = 0.013. This result supports the fact that there is no statistical difference between the properties of Sy1 and Sy2 (ii) We found that the coefficient of the best-fit linear regression equation between the common properties of Sy1 and Sy2 is significant (r > 0.50) which plausibly implies that Sy1 and Sy2 are the same type of objects observed at different viewing angle.

1. INTRODUCTION
2. THEORETICAL RELATIONSHIP
3. DATA SAMPLE
4. ANALYSIS AND RESULTS
    4.1 Distribution of Parameters of Sy1 and Sy2
    4.2 Principal Component Analysis (PCA)
    4.3 Pearson’s Correlations
5. DISCUSSION
6. CONCLUSION
ACKNOWLEDGMENTS
REFERENCES

• Evaristus U. Iyida(Astronomy and Astrophysics Research Group, Department of Physics and Astronomy, University of Nigeria, Nsukka 410001, Nigeria, Department of Physics and Astronomy, Faculty of Physical Sciences, University of Nigeria, Nsukka 410001, Nigeria) Corresponding author
• Innocent O. Eya(Astronomy and Astrophysics Research Group, Department of Physics and Astronomy, University of Nigeria, Nsukka 410001, Nigeria, Department of Physics and Astronomy, Faculty of Physical Sciences, University of Nigeria, Nsukka 410001, Nigeria, Department of Science Laboratory Technology, Faculty of Physical Sciences, University of Nigeria, Nsukka 410001, Nigeria)
• Christian I. Eze(Astronomy and Astrophysics Research Group, Department of Physics and Astronomy, University of Nigeria, Nsukka 410001, Nigeria, Department of Physics and Astronomy, Faculty of Physical Sciences, University of Nigeria, Nsukka 410001, Nigeria)