Relations Between Molecular Cloud Structure Sizes and Line Widths in the Large Magellanic Cloud. (arXiv:1905.11827v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Wong_T/0/1/0/all/0/1">Tony Wong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hughes_A/0/1/0/all/0/1">Annie Hughes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tokuda_K/0/1/0/all/0/1">Kazuki Tokuda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Indebetouw_R/0/1/0/all/0/1">R&#xe9;my Indebetouw</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Onishi_T/0/1/0/all/0/1">Toshikazu Onishi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bandurski_J/0/1/0/all/0/1">Jeffrey B. Bandurski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_C/0/1/0/all/0/1">C.-H. Rosie Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Glover_S/0/1/0/all/0/1">Simon C. O. Glover</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klessen_R/0/1/0/all/0/1">Ralf S. Klessen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pineda_J/0/1/0/all/0/1">Jorge L. Pineda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roman_Duval_J/0/1/0/all/0/1">Julia Roman-Duval</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sewilo_M/0/1/0/all/0/1">Marta Sewi&#x142;o</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wojciechowski_E/0/1/0/all/0/1">Evan Wojciechowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zahorecz_S/0/1/0/all/0/1">Sarolta Zahorecz</a>

We present a comparative study of the size-line width relation for
substructures within six molecular clouds in the Large Magellanic Cloud (LMC)
mapped with the Atacama Large Millimeter/submillimeter Array (ALMA). Our sample
extends our previous study, which compared a Planck detected cold cloud in the
outskirts of the LMC with the 30 Doradus molecular cloud and found the typical
line width for 1 pc radius structures to be 5 times larger in 30 Doradus. By
observing clouds with intermediate levels of star formation activity, we
demonstrate a clear correlation between line width at fixed size and both local
and cloud-scale 8${mu}$m intensity. At the same time, line width at a given
size appears to independently correlate with measures of mass surface density.
Our results suggest that both virial-like motions due to gravity and local
energy injection by star formation feedback play important roles in determining
intracloud dynamics.

We present a comparative study of the size-line width relation for
substructures within six molecular clouds in the Large Magellanic Cloud (LMC)
mapped with the Atacama Large Millimeter/submillimeter Array (ALMA). Our sample
extends our previous study, which compared a Planck detected cold cloud in the
outskirts of the LMC with the 30 Doradus molecular cloud and found the typical
line width for 1 pc radius structures to be 5 times larger in 30 Doradus. By
observing clouds with intermediate levels of star formation activity, we
demonstrate a clear correlation between line width at fixed size and both local
and cloud-scale 8${mu}$m intensity. At the same time, line width at a given
size appears to independently correlate with measures of mass surface density.
Our results suggest that both virial-like motions due to gravity and local
energy injection by star formation feedback play important roles in determining
intracloud dynamics.

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