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We present a study of the three-dimensional (3D) structure of the LargeMagellanic Cloud (LMC) using ~2.2 million red clump (RC) stars selected fromthe Survey of the MAgellanic Stellar History. To correct for line-of-sight dustextinction, the intrinsic RC color and magnitude and their radial dependenceare carefully measured by using internal nearly dust-free regions. These arethen used to construct an accurate 2D reddening map (165 square degrees with~10 arcmin resolution) of the LMC disk and the 3D spatial distribution of RCstars. An inclined disk model is fit to the 2D distance map yielding a best-fitinclination angle i = 25.86(+0.73,-1.39) degrees with random errors of +\-0.19degrees and line-of-nodes position angle theta = 149.23(+6.43,-8.35) degreeswith random errors of +/-0.49 degrees. These angles vary with galactic radius,indicating that the LMC disk is warped and twisted likely due to the repeatedtidal interactions with the Small Magellanic Cloud (SMC). For the first time,our data reveal a significant warp in the southwestern part of the outer diskstarting at rho ~ 7 degrees that departs from the defined LMC plane up to ~4kpc toward the SMC, suggesting that it originated from a strong interactionwith the SMC. In addition, the inner disk encompassing the off-centered barappears to be tilted up to 5-15 degrees relative to the rest of the LMC disk.These findings on the outer warp and the tilted bar are consistent with thepredictions from the Besla et al. simulation of a recent direct collision withthe SMC.

SMASHing the LMC: A Tidally-induced Warp in the Outer LMC and a Large-scale Reddening Map