  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.
