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The structural parameters, like the inclination, i and the position angle ofthe line of nodes (PA_lon) of the disk of the Large Magellanic Cloud (LMC) areestimated using the JH photometric data of red clump stars from the InfraredSurvey Facility - Magellanic Cloud Point Source Catalog (IRSF-MCPSC). Theobserved LMC region is divided into several sub-regions and stars in eachregion are cross identified with the optically identified red clump stars toobtain the near infrared magnitudes. The peak values of H magnitude and (J-H)colour of the observed red clump distribution are obtained by fitting a profileto the distributions and also by taking the average value of magnitude andcolour of the red clump stars in the bin with largest number. Then thedereddened peak H0 magnitude of the red clump stars in each sub-region isobtained. The RA, Dec and relative distance from the center of each sub-regionare converted into x, y & z Cartesian coordinates. A weighted least squareplane fitting method is applied to this x,y,z data to estimate the structuralparameters of the LMC disk. A reddening map based on (J-H) colour of the RCstars is presented. When the peaks of the red clump distribution wereidentified by averaging, an inclination of 25.7 +/- 1.6 and PA_lon = 141.5 +/-4.5 were obtained. We estimate a distance modulus of 18.47 +/- 0.1 mag to theLMC. Extra-planar features which are in front as well as behind the fittedplane are identified which match with the optically identified extra-planarfeatures. The bar of the LMC is found to be part of the disk within 500 pc. Theestimates of the structural parameters are found to be independent of thephotometric bands used for the analysis. We find that the inner disk, within3.0, is less inclined and has larger value of PA_lon when compared to the outerdisk.

Structure of the Large Magellanic Cloud from the Near Infrared magnitudes of Red Clump stars