  We used the red clump stars from the photometric data of the Optical
Gravitational Lensing Experiment(OGLE II) survey and the Magellanic Cloud
Photometric Survey (MCPS) for both the Clouds to estimate the depth.The
observed dispersion in the magnitude and colour distribution of red clump stars
is used to estimate the depth, after correcting for population effects,
internal reddening within the Clouds and photometric errors.The observed
dispersion due to the line of sight depth ranges from 0.023 mag to 0.45 mag (a
depth of 500 pc to 10.4 kpc) for LMC and from 0.025 to 0.34 magnitude(a depth
of 670 pc to 9.53 kpc).The depth profile of the LMC bar indicates that it is
flared.The average depth in the bar region is 4.0$\pm$1.4 kpc. The northern
disk is found to have depth(4.17$\pm$0.97 kpc)larger than the southern part of
the disk (2.63$\pm$0.8kpc).There is no indication of depth variation between
the eastern and the western disk.The average depth for the disk is 3.44$\pm$
1.16 kpc.In the case of SMC, the bar depth(4.90$\pm$1.23 kpc)and the disk depth
(4.23$\pm$1.48kpc)are found to be within the standard deviations.A prominent
feature in the SMC is the increase in depth near the optical center.The large
dispersions estimated for the LMC bar and the northern disk suggest that the
LMC either has large depth and/or different stellar populations in these
regions.The halo of the LMC(using RR Lyrae stars)is found to have larger depth
compared to the disk/bar,which supports the existence of an inner halo for the
LMC.On the other hand, the estimated depths for the halo(RR Lyrae stars)and
disk are found to be similar,for the SMC bar region. Thus,increased depth and
enhanced stellar as well as HI density near the optical center suggests that
the SMC may have a bulge.
