stribution, with a total dust mass of 2.1 $\times$ 10$^4$ [$M_\odot$]{} (2.8 times less than if carbon dust was modelled by standard graphite grains) in the resolved elements we model. We also find a non-negligible amount of dust in the region called “N159 South", a molecular cloud that does not show massive star formation. We also investigate the drivers of the [[*Herschel*]{}]{}/PACS and SPIRE submm colours and find that the submm ratios correlate strongly with the radiation field intensity and with the near and mid-IR surface brightnesses equally well. Comparing our dust map to H[i]{} and CO observations in N159, we then investigate variations in the gas-to-dust mass ratio (G/D) and the CO-to-H$_2$ conversion factor X$_{CO}$. A mean value of G/D$\sim$356 is derived when using X$_{CO}$ = 7$\times$10$^{20}$ H$_2$ cm$^{-2}$ (K km s$^{-1}$)$^{-1}$ [@Fukui2009]. If a constant G/D across N159 is assumed, we derive a X$_{CO}$ conversion factor of 5.4$\times$10$^{20}$ H$_2$ cm$^{-2}$ (K km s$^{-1}$)$^{-1}$. We finally model individual regions to analyse variations in the SED shape across the complex and the 870 [$\mu$m]{} emission in more details. No measurable submm excess emission at 870 [$\mu$m]{} seems to be detected in these regions.'
author:
- '\'
bibliography:
- '/Users/maudgalametz/Documents/Work/Papers/mybiblio.bib'
title: 'The thermal dust emission in N158-N159-N160 (LMC) star forming complex mapped by Spitzer, Herschel and LABOCA'
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galaxies: ISM – galaxies:dwarf– galaxies:SED model – ISM: dust – submillimeter: galaxies

Introduction
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As potential templates of primordial environments, low-metallicity galaxies are keystones to understand how galaxies evolve through cosmic time. Studying the Interstellar Medium (ISM) of low-metallicity galaxies is a necessary step to get a handle on the interplay between star formation and the ISM under conditions characteristic of the early universe. Low-metallicity galaxies also have quite different infrared (IR) Spectral Energy Distributions (S