The Large and Small Magellanic Clouds are a pair of nearby, likely rather massive dwarf galaxies. Located at 50 and 60 kpc from us, at the moment well within the halo of the Milky Way, the LMC and the SMC are believed to be the satellites of our Galaxy. However, the epoch of their accretion, their binary lifetime and their masses are largely unconstrained. This uncertainty poses a serious challenge to our attempts to reconstruct the properties of the Milky Way from the observables delivered by the ESA's Gaia satellite. Using the wide and deep DECam images we have mapped out the Magellanic periphery and detected BHB stars possibly residing in the LMC's halo. I will present the results of a spectroscopic follow-up campaign of our candidate Magellanic halo stars carried out with the FORS2 (VLT). Implications of the extension of the LMC stellar halo as well as the past interaction of the Large Cloud with the Small will be discussed.