Resolved star formation in the metal poor star-forming region Magellanic Bridge C. (arXiv:2009.11868v1 [astro-ph.GA])

Resolved star formation in the metal poor star-forming region Magellanic Bridge C. (arXiv:2009.11868v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kalari_V/0/1/0/all/0/1">V. M. Kalari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rubio_M/0/1/0/all/0/1">M. Rubio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Saldano_H/0/1/0/all/0/1">H. P. Salda&#xf1;o</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bolatto_A/0/1/0/all/0/1">A. D. Bolatto</a>

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.

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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