We used the red clump stars from the Optical Gravitational Lensing Experiment ( OGLE II ) survey and the the Magellanic Cloud Photometric Survey ( MCPS ) , to estimate the line of sight depth .
The observed dispersion in the magnitude and colour distribution of red clump stars is used to estimate the line of sight depth , after correcting for the contribution due to other effects .
This dispersion due to depth , has a range from minimum dispersion that can be estimated , to 0.46 mag ( a depth of 500 pc to 10.44 Kpc ) , in the LMC .
In the case of SMC , the dispersion ranges from minimum dispersion to 0.35 magnitude ( a depth of 665 pc to 9.53 Kpc ) .
The thickness profile of LMC bar indicates that it is flared .
The average depth in the bar region is 4.0 \pm 1.4 kpc .
The halo of the LMC ( using RR Lyrea stars ) is found to have larger depth compared to the disk/bar , which supports the presence of inner halo for the LMC .
The large depth estimated for the LMC bar and the disk suggests that the LMC might have had minor mergers .
In the case of SMC , the bar depth ( 4.90 \pm 1.23 Kpc ) and the disk depth ( 4.23 \pm 1.48 Kpc ) are found to be within the standard deviations .
We find evidence for increase in depth near the optical center ( up to 9 kpc ) .
On the other hand , the estimated depth for the halo ( RR Lyrea stars ) and disk ( RC stars ) for the bar region of the SMC is found to be similar .
Thus , increased depth and enhanced stellar as well as HI density near the optical center suggests that the SMC may have a bulge .