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The structure and evolution of the disk of the Small Magellanic Cloud (SMC)are traced by studying the Cepheids. We aim to estimate the orientationmeasurements of the disk, such as the inclination and the position angle of theline of nodes, and the depth of the disk. We used the V and I band photometricdata of the fundamental and first-overtone Cepheids from the OpticalGravitational Lensing Experiment survey. The period-luminosity relations wereused to estimate the relative distance and reddening of each Cepheid. Aweighted least-square plane fitting method was then applied to estimate thestructural parameters. The line-of-sight depth and then the orientationcorrected depth or thickness of the disk were estimated from the relativedistance measurements. The period-age-colour relation of Cepheids were used toderive the age of the Cepheids. A break in the PL relations of thefundamental-mode and first-overtone Cepheids at P ~ 2.95 days and P ~ 1 day areobserved. An inclination of 64$^o$.4$\pm$0$^o$.7 and aPA$_{lon}$=155$^o$.3$\pm$6$^o$.3 are obtained from the full sample. A reddeningmap of the SMC disk is also presented. The orientation-corrected depth orthickness of the SMC disk is found to be 1.76 $\pm$ 0.6 kpc. The scale heightis estimated to be 0.82 $\pm$ 0.3 kpc. The age distribution of Cepheids matchesthe SMC cluster age distribution. The radial variation of the disk parametersmildly indicate structures/disturbances in the inner SMC (0.5 $<$ r $<$ 2.5degree). Some of the Cepheids found in front of the fitted plane in the easternregions are possibly the youngest tidally stripped counterpart of the H {{\sci}} gas of the Magellanic Bridge. The Cepheids behind the fitted plane are mostlikely the population in the Counter Bridge predicted in recent numericalsimulations. Different scenarios for the origin of the extra-planar Cepheidsare also discussed.

Disk of the Small Magellanic Cloud as traced by Cepheids