JCMT 850 μm continuum observations of density structures in the G35 molecular complex

Shen, Xianjin, Liu, Hong-Li, Ren, Zhiyuan, Tej, Anandmayee, Li, Di, Liu, Hauyu Baobab, Fuller, Gary A., Xie, Jinjin, Jiao, Sihan, Yang, Aiyuan, Koch, Patrick M., Xu, Fengwei, Sanhueza, Patricio, Diep, Pham Ngoc, Peretto, Nicolas ORCID: https://orcid.org/0000-0002-6893-602X, Yadav, R. K., Kramer, Busaba H., Sugiyama, Koichiro, Rawlings, Mark G., Lee, Chang Won, Tatematsu, Ken’ichi, Harsono, Daniel, Eden, David, Kwon, Woojin, Tsai, Chao-Wei, White, Glenn J., Kim, Kee-Tae, Liu, Tie, Wang, Ke, Zhang, Siju, Jiao, Wenyu, Yang, Dongting, Das, Swagat R., Wu, Jingwen and Wang, Chen 2024. JCMT 850 μm continuum observations of density structures in the G35 molecular complex. The Astrophysical Journal 974 (2) , 239. 10.3847/1538-4357/ad6a5f

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Abstract

Filaments are believed to play a key role in high-mass star formation. We present a systematic study of the filaments and their hosting clumps in the G35 molecular complex using James Clerk Maxwell Telescope SCUBA-2 850 μm continuum data. We identified five clouds in the complex and 91 filaments within them, some of which form 10 hub–filament systems (HFSs), each with at least three hub-composing filaments. We also compiled a catalog of 350 dense clumps, 183 of which are associated with the filaments. We investigated the physical properties of the filaments and clumps, such as mass, density, and size, and their relation to star formation. We find that the global mass–length trend of the filaments is consistent with a turbulent origin, while the hub-composing filaments of high line masses (m l > 230 M ⊙ pc−1) in HFSs deviate from this relation, possibly due to feedback from massive star formation. We also find that the most massive and densest clumps (R > 0.2 pc, M > 35 M ⊙, Σ > 0.05 g cm−2) are located in the filaments and in the hubs of HFSs, with the latter bearing a higher probability of the occurrence of high-mass star-forming signatures, highlighting the preferential sites of HFSs for high-mass star formation. We do not find significant variation in the clump mass surface density across different evolutionary environments of the clouds, which may reflect the balance between mass accretion and stellar feedback.

Item Type:	Article
Date Type:	Published Online
Status:	Published
Schools:	Physics and Astronomy
Additional Information:	License information from Publisher: LICENSE 1: URL: http://creativecommons.org/licenses/by/4.0/, Type: cc-by
Publisher:	American Astronomical Society
ISSN:	0004-637X
Date of First Compliant Deposit:	16 October 2024
Date of Acceptance:	29 July 2024
Last Modified:	16 Oct 2024 13:31
URI:	https://orca.cardiff.ac.uk/id/eprint/172938

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