Five different calibrations of metal abundances of globular clusters are examined and these are compared with metallicity ranking parameters such as ( S p ) c , . Q39 and IR-indices. Except for the calibration [ F e / H ] H by the high dispersion echelle analysis. the other calibration scales are correlated with the morphological parameters of red giant branch. In the [ F e / H ] H -scale. the clusters later than ∼ F 8 have nearly a constant metal abundance. [ F e / H ] H ≃ − 1.05 , regradless of morphological characteristics of horizontal branch and red giant branch. By the two fundamental calibration scales of [ F e / H ] L (derived by the low dispersion analysis) and [ F e / H ] Δ s (derived by the spectral analysis of RR Lyrae stars). the globular clusters are divided into the halo clusters with [Fe/H]<-1.0 and the disk clusters confined within the galactocentric distance τ G = 10 k p c and galactic plane distance |z|=3 kpc. In this case the abundance gradient is given by d[Fe/H]/ d r G ≈ − 0.05 k p c − 1 and d[Fe/H]/ d | z | ≃ − 0.08 k p c − 1 within τ G = 20 k p c and |z|=10 kpc, respectively. According to these characteristics of the spatial distribution of globular clusters. the chemical evolution of the galactic globular clusters can be accounted for by the two-zone (disk-halo) slow collapse model when the [ F e / H ] L -or [ F e / H ] Δ s -scale is applied. In the case of [ F e / H ] H -scale, the one-zone fast collapse model is preferred for the evolution of globular clusters.

ABSTRACT
Ⅰ. INTRODUCTION
Ⅱ. FUNDAMENTAL CALIBRATIONS OF METAL ABUNDANCE
Ⅲ. RANKING PARAMETERS OF METALLICITY
Ⅳ. SPATIAL DISTRIBUTION OF METAL ABUNDANCE AND ITS IMPLICATION FOR THE GALACTIC EVOLUTION
Ⅴ. SUMMARY
REFERENCES

• LEE SEE-WOO(Department of Astronomy, Seoul National University)
• PARK NAM-KYU(Department of Astronomy, Seoul National University)