We present a study of three-dimensional structure of the Small Magellanic Cloud ( SMC ) .
The V - and I -band light curves of the fundamental mode RR Lyrae stars ( RRab ) obtained by the Optical Gravitational Lensing Experiment ( OGLE ) -III project were utilized in order to comprehend the SMC structure .
The [ Fe / H ] - P - \phi _ { 31 } relation of is exploited to obtain the metallicities .
From the three-dimensional RRab distance distributions , northeast ( NE ) arm and main body of the galaxy is identified .
Combining metallicities with spatial distribution of these tracers , no radial metallicity gradient in the SMC has been detected .
Dividing the entire sample into three parts : northeastern ( NE ) , central and southwestern ( SW ) , we find that the central part has a significantly larger line of sight depth as compared to rest of the parts , indicating that the SMC may have a bulge .
Results obtained from the I -band data seem to be reliable and were further substantiated using the relation .
Distribution of SMC RRab stars were modeled as a tri-axial ellipsoid .
Errors in structural parameters of the SMC ellipsoid were obtained from Monte Carlo simulations .
We estimated the axes ratios of the galaxy as 1.00 \pm 0.000 : 1.310 \pm 0.029 : 8.269 \pm 0.934 , the inclination of the longest axis with line of sight i = 2 ^ { \circ } .265 \pm 0 ^ { \circ } .784 , and the position angle of the line of nodes \theta _ { \text { lon } } = 74 ^ { \circ } .307 \pm 0 ^ { \circ } .509 from the variance weighted I -band determinations .