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tokens: But, under a simplistic steady state assumption, our results do not favour the surface density thresholds required for star formation commonly adopted in Galactic studies that assume a certain magnetic field strength (Heiderman et al. 2010 ). However, low-density gas in the Magellanic Bridge has been evolving into denser molecular gas, from which stars form, and the lower densities of the molecular gas in this region may signal the exhausting of the latter. The density of YSOs and PMS stars in the subregions ranges in a continuum from moderately clustered to relative isolation, reminiscent of star formation in the Milky Way (e.g. Bressert et al. 2010 ). However, low number statistics precludes us from defining a surface density for each subregion. Our results suggest that star formation observed in MB -C is underway in localized regions depending on the density inhomogeneities within an initial cloud, and is intimately linked with the presence of dense molecular gas. 5.2 Molecular gas structure in the Magellanic Bridge In Section 2 , we have investigated the properties of the molecular clumps in MB -C. The clumps were gravitationally stable, and very similar to clumps related to star formation in the Milky Way. Their densities, radii, masses, and linewidths do not differentiate them from clumps previously identified in the intermediate to low-density regimes of star formation in the Milky Way (Kennicutt Evans 2012 ). The clumps are related to star formation, as seen by their proximity to YSOs and PMS stars. The properties of YSOs and PMS stars show no remarkable differences compared to the Galaxy on account of their metallicities, except lower extinctions towards them. Overall, this suggests that even though the CO has lower filling factors in the Magellanic Bridge than found in solar metallicity molecular clouds, the actual star formation process proceeds similarly once cold molecular gas is formed, and differences may arise due to the conversion of atomic to molecular gas. The lower dust-to-gas ratio results in lower extinction towards the line of sight of protostars, which affects similarly the X CO factor, but the formation of molecular gas is the unifying factor between star formation. The effect of the lower self-shielding by CO on its durability is unclear, since the incident radiation field in MB -C is not particularly strong only containing early B-type stars. Recent observations from the Herschel space telescope at far-infrared wavelengths have suggested a common unifying factor between star formation and the formation of filamentary structure in the cold interstellar medium (André 2017 ), ubiquitous in star-forming regions. Unfortunately, the FWHM of Herschel imaging (∼5–10 pc) at the distance to MB -C is more than an order of magnitude larger than the average width of filaments detected in the Milky Way (∼0.1 pc) therefore it is currently not possible to identify filaments in the Magellanic Bridge. Instead, we simply overplot YSOs