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We report molecular line and continuum observations toward one of the mostmassive giant molecular clouds (GMCs), GMC-16, in M33 using ALMA with anangular resolution of 0$''$44 $\times$ 0$''$27 ($\sim$2 pc $\times$ 1 pc). Wehave found that the GMC is composed of several filamentary structures in$^{12}$CO and $^{13}$CO ($J$ = 2-1). The typical length, width, and total massare $\sim$50-70 pc, $\sim$5-6 pc, and $\sim$10$^{5}$ $M_{\odot}$, respectively,which are consistent with those of giant molecular filaments (GMFs) as seen inthe Galactic GMCs. The elongations of the GMFs are roughly perpendicular to thedirection of the galaxy's rotation, and several H$\;${\sc ii} regions arelocated at the downstream side relative to the filaments with an offset of$\sim$10-20 pc. These observational results indicate that the GMFs areconsidered to be produced by a galactic spiral shock. The 1.3 mm continuum andC$^{18}$O ($J$ = 2-1) observations detected a dense clump with the size of$\sim$2 pc at the intersection of several filamentary clouds, which is referredto as the $"$hub filament,$"$ possibly formed by a cloud-cloud collision. Astrong candidate for protostellar outflow in M33 has also been identified atthe center of the clump. We have successfully resolved the parsec-scale localstar formation activity in which the galactic scale kinematics may induce theformation of the parental filamentary clouds.

astrophysical journal/the astrophysical journal

ALMA Observations of Giant Molecular Clouds in M33 I: Resolving Star  Formation Activities in the Giant Molecular Filaments Possibly Formed by a  Spiral Shock