The ALMA Survey of 70 mu m Dark High-mass Clumps in Early Stages (ASHES). IV. Star Formation Signatures in G023.477
Artikel i vetenskaplig tidskrift, 2021
With a mass of similar to 1000 M (circle dot) and a surface density of similar to 0.5 g cm(-2), G023.477+0.114, also known as IRDC 18310-4, is an infrared dark cloud (IRDC) that has the potential to form high-mass stars and has been recognized as a promising prestellar clump candidate. To characterize the early stages of high-mass star formation, we have observed G023.477+0.114 as part of the Atacama Large Millimeter/submillimeter Array (ALMA) Survey of 70 mu m Dark High-mass Clumps in Early Stages. We have conducted similar to 1.'' 2 resolution observations with ALMA at 1.3 mm in dust continuum and molecular line emission. We have identified 11 cores, whose masses range from 1.1 to 19.0 M (circle dot). Ignoring magnetic fields, the virial parameters of the cores are below unity, implying that the cores are gravitationally bound. However, when magnetic fields are included, the prestellar cores are close to virial equilibrium, while the protostellar cores remain sub-virialized. Star formation activity has already started in this clump. Four collimated outflows are detected in CO and SiO. H2CO and CH3OH emission coincide with the high-velocity components seen in the CO and SiO emission. The outflows are randomly oriented for the natal filament and the magnetic field. The position-velocity diagrams suggest that episodic mass ejection has already begun even in this very early phase of protostellar formation. The masses of the identified cores are comparable to the expected maximum stellar mass that this IRDC could form (8-19 M (circle dot)). We explore two possibilities on how IRDC G023.477+0.114 could eventually form high-mass stars in the context of theoretical scenarios.
Författare
Kaho Morii
National Institutes of Natural Sciences
University of Tokyo
Patricio Sanhueza
The Graduate University for Advanced Studies (SOKENDAI)
National Institutes of Natural Sciences
Fumitaka Nakamura
National Institutes of Natural Sciences
University of Tokyo
The Graduate University for Advanced Studies (SOKENDAI)
James M. Jackson
National Aeronautics and Space Administration (NASA)
Shanghuo Li
Korea Astronomy and Space Science Institute
Henrik Beuther
Max-Planck-Gesellschaft
Qizhou Zhang
Harvard-Smithsonian Center for Astrophysics
Siyi Feng
Xiamen University
Daniel Tafoya
Chalmers, Rymd-, geo- och miljövetenskap, Onsala rymdobservatorium
Andres E. Guzman
National Institutes of Natural Sciences
Natsuko Izumi
Academia Sinica
Takeshi Sakai
University of Electro-Communications
Xing Lu
National Institutes of Natural Sciences
Ken'ichi Tatematsu
National Institutes of Natural Sciences
The Graduate University for Advanced Studies (SOKENDAI)
Satoshi Ohashi
RIKEN
Andrea Silva
University of Tokyo
Fernando A. Olguin
National Tsing Hua University
Yanett Contreras
Universiteit Leiden
Astrophysical Journal
0004-637X (ISSN) 1538-4357 (eISSN)
Vol. 923 2 147Ämneskategorier (SSIF 2011)
Astronomi, astrofysik och kosmologi
Fusion, plasma och rymdfysik
Den kondenserade materiens fysik
DOI
10.3847/1538-4357/ac2365