ALMA view of G0.253+0.016: Can cloud-cloud collision form the cloud?

Abstract

We present the results of sulfur monoxide, SO line emission observations of G0.253+0.016 with the Atacama Large Millimeter/submillimeter Array (ALMA) at an angular resolution of 1.7 arcsec. The dense and massive molecular cloud of G0.253+0.016 is highly sub-structured, yet shows no obvious signs of cluster formation. We found three outstanding features of the cloud from the SO emission, namely, shell structure of radius 1.3 pc, large velocity gradients of 20 km/s/pc with the cloud, and cores with large velocity dispersions (30-40 km/s) around the shell structure. We suggest that these large-velocity dispersion cores will form high-mass stars in the future. In attempt to explore the formation scenario of the dense cloud, we compared our results with numerical simulations, thus, we propose that G0.253+0.016 may have formed due to a cloud-cloud collision process.

arXiv comment16 pages, 5 figures, accepted for publication in the Astronomical Journal

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• ALMA Observations of Giant Molecular Clouds in M33. II. Triggered High-mass Star Formation by Multiple Gas Colliding Events at the NGC 604 Complex
• IRAS16547-4247: A New Candidate of a Protocluster Unveiled with ALMA
• Stability of filaments in star-forming clouds and the formation of prestellar cores in them
• CO-0.30-0.07: A Peculiar Molecular Clump with an Extremely Broad Velocity Width
• The physical and chemical structure of Sagittarius B2, VIII. Full molecular line survey of hot cores
• The initial conditions for young massive cluster formation in the Galactic Centre: convergence of large-scale gas flows
• HCN $J$=4-3, HNC $J$=1-0, ${\mathrm{H}}^{13}\mathrm{CN}$ $J$=1-0, and $\mathrm{H}{\mathrm{C}}_3\mathrm{N}$ $J$=10-9 Maps of Galactic Center Region II.: Physical Properties of Dense Gas Clumps and Probability of Star Formation
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