Resolved star formation in the metal poor star-forming region Magellanic
  Bridge C
  Magellanic Bridge C (MB-C) is a metal-poor ($\sim$1/5 $Z_{\odot}$)
low-density star-forming region located 59 kpc away in the Magellanic Bridge,
offering a resolved view of the star formation process in conditions different
to the Galaxy. From Atacama Large Millimetre Array CO (1-0) observations, we
detect molecular clumps associated to candidate young stellar objects (YSOs),
pre-main sequence (PMS) stars, and filamentary structure identified in
far-infrared imaging. YSOs and PMS stars form in molecular gas having densities
between 17-200 $M_{\odot}$ pc$^{-2}$, and have ages between $\lesssim$0.1-3
Myr. YSO candidates in MB-C have lower extinction than their Galactic
counterparts. Otherwise, our results suggest that the properties and
morphologies of molecular clumps, YSOs, and PMS stars in MB-C present no patent
differences with respect to their Galactic counterparts, tentatively alluding
that the bottleneck to forming stars in regions similar to MB-C is the
conversion of atomic gas to molecular.
