Applying mass model to disk galaxy NGC 300, since the observed rotation curve of NGC 300 is flatter than Toomre's mass model n = 1, two cases are used; obtaining parameters a n and b n from the polynomial fitting of the observed rotation curve (case A) and from the least square fitting between the observed rotation curve and model rotation curve (case B). In any case, n bas a fixed value of 1. Brandt's mass model is also discussed. which has a shape parameter n = 1.4. Calculated total mass and total mass to luminosity ratio are 3.3 × 10 10 M ⊙ , l2.1 for case A and 2.8 × 10 10 M ⊙ , 10.3 for case B. In case of Brandt's model, the values are 4.2 × 10 10 M ⊙ and 15.4. The rise in the local mass to luminosity ratio in the outer part of NGC 300 implies existence of massive halo. Other dynamical properties are also discussed.

ABSTRACT
    Ⅰ. INTRODUCTION
    Ⅱ. SURFACE BRIGHTNESS DISTRIBUTION OF NGC 300
    Ⅲ. ROTATIONAL VELOCITY
    Ⅳ. DYNAMICAL PARAMETERS OF NGC 300
    Ⅴ. CONCLUSION
    ACKNOWLEDGEMENTS
    REFERENCES

• RHEE MYUNG-HYUN(Department of Astronomy and Atmospheric Science, Yonsei University)
• CHUN MUN-SUK(Department of Astronomy and Atmospheric Science, Yonsei University)