Issue |
A&A
Volume 676, August 2023
|
|
---|---|---|
Article Number | A15 | |
Number of page(s) | 11 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361/202346248 | |
Published online | 27 July 2023 |
Gravitational collapse and accretion flows in the hub filament system G323.46-0.08
1
XingJiang Astronomical Observatory, Chinese Academy of Sciences,
Urumqi
830011, PR China
e-mail: zhoujj@xao.ac.cn; jarken@xao.ac.cn; mayingxiu@xao.ac.cn
2
University of Chinese Academy of Sciences,
Beijing
100049, PR China
3
Key Laboratory of Radio Astronomy, Chinese Academy of Sciences,
Urumqi
830011, PR China
4
Xinjiang Key Laboratory of Radio Astrophysics,
Urumqi
830011, PR China
5
Netherlands Institute for Radio Astronomy, ASTRON,
7991 PD
Dwingeloo, The Netherlands
6
Max-Planck-Institut für Radioastronomie,
Auf dem Hügel 69,
53121
Bonn, Germany
7
Energetic Cosmos Laboratory, Nazarbayev University,
Astana
010000, Kazakhstan
8
Faculty of Physics and Technology, Al-Farabi Kazakh National University,
Almaty
050040, Kazakhstan
Received:
26
February
2023
Accepted:
8
June
2023
We studied the hub-filament system G323.46-0.08 based on archival molecular line data from the SEDIGISM 13CO survey and infrared data from the GLIMPSE, MIPS, and Hi-GAL surveys. G323.46-0.08 consists of three filaments, F-north, F-west, and F-south, that converge toward the central high-mass clump AGAL 323.459-0.079. F-west and Part1 of the F-south show clear large-scale velocity gradients 0.28 and 0.44 km s−1 pc−1, respectively. They seem to be channeling materials into AGAL 323.459-0.079. The minimum accretion rate was estimated to be 1216 M⊙ Myr−1. A characteristic V-shape appears around AGAL323.459-0.079 in the PV diagram, which traces the accelerated gas motions under gravitational collapse. This has also been supported by model fitting results. All three filaments are supercritical and they have fragmented into many dense clumps. The seesaw patterns near most dense clumps in the PV diagram suggests that mass accretion also occurs along the filament toward the clumps. Our results show that filamentary accretion flows appear to be an important mechanism for supplying the materials necessary to form the central high-mass clump AGAL 323.459-0.079 and to propel the star forming activity taking place therein.
Key words: ISM: clouds / ISM: kinematics and dynamics / ISM: individual objects: G323.46-0.08 / stars: formation / radio lines: ISM
© The Authors 2023
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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