Resolved star formation in the metal poor star-forming region Magellanic Bridge C

Abstract

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.

Accepted for publication in MNRAS; 22 pages, 14 figs

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Cited by in corpus (1)

• Sequential Star Formation in the Young SMC Region NGC 602: Insights from ALMA