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Polarization of interstellar dust emission is a powerful probe of dustproperties and magnetic field structure. Yet studies of external galaxies arehampered by foreground dust contribution. The aim of this study is to separatethe polarised signal from the Large Magellanic Cloud (LMC) from that of theMilky Way (MW) in order to construct a wide-field, spatially complete map ofdust polarization using the Planck 353 GHz data. To estimate the foregroundpolarization direction, we used velocity gradients in HI spectral line data andassessed the performance of the output by comparing to starlight extinctionpolarization. We estimate the foreground intensity using dust propertiesderived previously from the Planck data and we assume the foregroundpolarization to be uniform and equal to the average of the MW around thegalaxy. After foreground removal, the geometry of the plane-of-the-sky magneticfield in the LMC tends to follow the structure of the atomic gas in the LMC.This is notably the case along the molecular ridges extending south andsouth-east of the 30 Doradus star-forming complex, and along more diffusesouthern arm extending towards the Small Magellanic Cloud. There is also analignment between the magnetic field and the outer arm in the western part. Themedian polarization fraction in the LMC is slightly lower than that observedfor the MW while the anti-correlation between the polarization angle dispersionfunction and the polarization fraction is slightly larger. Overall,polarization fraction distribution is similar to that observed in the MW.

Unveiling polarized emission from interstellar dust of the Large Magellanic Cloud with Planck