TY - JOUR
T1 - ALMA CO observations of a giant molecular cloud in M 33 : evidence for high-mass star formation triggered by cloud-cloud collisions
AU - Sano, Hidetoshi
AU - Tsuge, Kisetsu
AU - Tokuda, Kazuki
AU - Muraoka, Kazuyuki
AU - Tachihara, Kengo
AU - Yamane, Yumiko
AU - Kohno, Mikito
AU - Fujita, Shinji
AU - Enokiya, Rei
AU - Rowell, Gavin
AU - Maxted, Nigel
AU - Filipović, Miroslav D.
AU - Knies, Jonathan
AU - Sasaki, Manami
AU - Onishi, Toshikazu
AU - Plucinsky, Paul P.
AU - Fukui, Yasuo
PY - 2021
Y1 - 2021
N2 - We report the first evidence for high-mass star formation triggered by collisions of molecular clouds in M 33. Using the Atacama Large Millimeter/submillimeter Array, we spatially resolved filamentary structures of giant molecular cloud 37 in M 33 using 12CO(J = 2-1), 13CO(J = 2-1), and C18O(J = 2-1) line emission at a spatial resolution of ∼2 pc. There are two individual molecular clouds with a systematic velocity difference of ∼6 km s-1. Three continuum sources representing up to ∼10 high-mass stars with spectral types of B0V-O7.5V are embedded within the densest parts of molecular clouds bright in the C18O(J = 2-1) line emission. The two molecular clouds show a complementary spatial distribution with a spatial displacement of ∼6.2 pc, and show a V-shaped structure in the position-velocity diagram. These observational features traced by CO and its isotopes are consistent with those in high-mass star-forming regions created by cloud-cloud collisions in the Galactic and Magellanic Cloud H II regions. Our new finding in M 33 indicates that cloud-cloud collision is a promising process for triggering high-mass star formation in the Local Group.
AB - We report the first evidence for high-mass star formation triggered by collisions of molecular clouds in M 33. Using the Atacama Large Millimeter/submillimeter Array, we spatially resolved filamentary structures of giant molecular cloud 37 in M 33 using 12CO(J = 2-1), 13CO(J = 2-1), and C18O(J = 2-1) line emission at a spatial resolution of ∼2 pc. There are two individual molecular clouds with a systematic velocity difference of ∼6 km s-1. Three continuum sources representing up to ∼10 high-mass stars with spectral types of B0V-O7.5V are embedded within the densest parts of molecular clouds bright in the C18O(J = 2-1) line emission. The two molecular clouds show a complementary spatial distribution with a spatial displacement of ∼6.2 pc, and show a V-shaped structure in the position-velocity diagram. These observational features traced by CO and its isotopes are consistent with those in high-mass star-forming regions created by cloud-cloud collisions in the Galactic and Magellanic Cloud H II regions. Our new finding in M 33 indicates that cloud-cloud collision is a promising process for triggering high-mass star formation in the Local Group.
UR - https://hdl.handle.net/1959.7/uws:64421
U2 - 10.1093/pasj/psaa045
DO - 10.1093/pasj/psaa045
M3 - Article
SN - 0004-6264
VL - 73
SP - S62-S74
JO - Publications of the Astronomical Society of Japan
JF - Publications of the Astronomical Society of Japan
IS - SP1
ER -