From filaments to the hub: Gas kinematics and massive star formation in G329.34+0.14

Wenjun Zhang, Jianjun Zhou, Tie Liu, Xunchuan Liu, Dongting Yang, Enrique Vazquez‐Semadeni, Gilberto C. Gómez, Hong-Li Liu, Jarken Esimbek, Xindi Tang

25 more authors

Gang Wu, Siju Zhang, Di Li, Swagat Ranjan Das, Guido Garay, Fengwei Xu, Naval Kishor Bhadari, Lokesh Kumar Dewangan, Prasanta Gorai, Jihye Hwang, Aiyuan Yang, James O. Chibueze, Pablo García, Chang Won Lee, Ariful Hoque, L. V. Toth, Kee-Tae Kim, Willem A. Baan, Dalei Li, Yuxin He, Yingxiu Ma, Dongdong Zhou, Kadirya Tursun, Toktarkhan Komesh, Weiguang Ji

Astronomy and Astrophysics, 2026

Full text Open access: Gold Metadata (CSL-JSON)
DOI 10.1051/0004-6361/202554094
Data confidence 85 high
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Abstract

We present 13 CO (J=2–1) emission from the SEDIGISM survey, together with ALMA Band 3 and Band 6 observations from the ATOMS and QUARKS surveys, to investigate the gas kinematics and feedback processes in the massive hub-filament system G329.34+0.14 (hereafter G329). Based on Herschel continuum morphology together with the 13 CO (J=2–1) integrated intensity and velocity distributions, a parsec-scale network of filaments was identified, converging toward the hub that hosts two massive clumps, MC 1 and MC 2, with respective masses of ~4210 (±1259) M ⊙ and ~1483 (±443) M ⊙ . Position-velocity analysis reveals systematic projected velocity gradients along the filaments, consistent with organized gas motions on parsec scales and possible inflows toward the hub. Within MC 1, ALMA resolves a sub-parsec network of intra-hub filaments (IHFs) traced by H 13 CO + (J=1–0), with a velocity organization similar to that seen on parsec scales. These IHFs are distributed around a central H II region, surrounded by a shell-like structure traced by CS (J=2–1) and H 13 CO + (J=1–0) emission, with dense gas concentrated in its northeastern and southwestern sectors. The shell further shows SiO (J=2–1) and SO (J=3(2)–2(1)) emission, excited mainly by low-velocity shocks from the expansion of the H II region, with a minor contribution from protostellar outflows. Compared with the surrounding parsec-scale filaments, the IHFs are more compact but exhibit larger velocity gradients and line masses, suggesting that the inner hub gas is denser and dynamically more complex. MC 1 and MC 2 are interpreted as two massive clumps embedded in the same hub, with MC 1 appearing more evolved and more strongly affected by feedback than MC 2. G329 therefore provides an observational case in which the parsec-scale hub-filament structure and the dense IHF network show a broadly similar velocity organization. This suggests a possible kinematic connection between the surrounding filaments and dense gas in the hub interior.