An ALMA study of the massive molecular clump N159W-North in the Large
  Magellanic Cloud: A possible gas flow penetrating one of the most massive
  protocluster systems in the Local Group
  Massive dense clumps in the Large Magellanic Cloud can be an important
laboratory to explore the formation of populous clusters. We report multiscale
ALMA observations of the N159W-North clump, which is the most CO-intense region
in the galaxy. High-resolution CO isotope and 1.3 mm continuum observations
with an angular resolution of $\sim$0."25($\sim$0.07 pc) revealed more than
five protostellar sources with CO outflows within the main ridge clump. One of
the thermal continuum sources, MMS-2, shows especially massive/dense nature
whose total H$_2$ mass and peak column density are $\sim$10$^{4}$ $M_{\odot}$
and $\sim$10$^{24}$ cm$^{-2}$, respectively, and harbors massive ($\sim$100
$M_{\odot}$) starless core candidates identified as its internal substructures.
The main ridge containing this source can be categorized as one of the most
massive protocluster systems in the Local Group. The CO high-resolution
observations found several distinct filamentary clouds extending southward from
the star-forming spots. The CO (1-0) data set with a larger field of view
reveals a conical-shaped, $\sim$30 pc long complex extending toward the
northern direction. These features indicate that a large-scale gas compression
event may have produced the massive star-forming complex. Based on the striking
similarity between the N159W-North complex and the previously reported other
two high-mass star-forming clouds in the nearby regions, we propose a
$"$teardrops inflow model$"$ that explains the synchronized, extreme star
formation across $>$50 pc, including one of the most massive protocluster
clumps in the Local Group.
