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arXiv · 2009.11868

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

V. M. Kalari·M. Rubio·H. P. Saldaño·A. D. Bolatto
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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.

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V. M. Kalari, M. Rubio, H. P. Saldaño, A. D. Bolatto. 2020-09-24. Resolved star formation in the metal poor star-forming region Magellanic Bridge C. https://doi.org/10.1093/mnras%2Fstaa2963

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