From filaments to the hub: Gas kinematics and massive star formation in G329.34+0.14
Rattachement africain : cn, mx, cl, in, no, kr, hu. Niveau de preuve : code pays fourni par la source.
Le résumé fourni par la source
We present 13CO (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 13CO (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 H13CO+ (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 H13CO+ (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.
Ce résumé expose les affirmations des auteurs. BNTIC ne l’interprète pas comme une validation indépendante des résultats.
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Xinjiang Astronomical Observatory pays non établi dans la noticeStructure de recherche
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University of Chinese Academy of Sciences Shanghai Astronomical Observatory pays non établi dans la noticeUniversité ou école supérieure
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Clínica Las Condes pays non établi dans la noticeÉtablissement de santé
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Chinese Academy of Science South America Center for Astronomy pays non établi dans la noticeStructure de recherche
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Xinjiang Astronomical Observatory, Shanghai Astronomical Observatory — University of Chinese Academy of Sciences et Shanghai Astronomical Observatory, avec 9 autres affiliations.
Une affiliation ne permet pas de déduire la nationalité d’un auteur.