A case investigation of an end-dominated collapse and hub-filament system, G53
Meng D. Esimbek J. Henkel C. Zhou J. Wu G. Tang X. Li D. He Y. Komesh T. Ma Y. Tursun K. Zhou D. Baan W. Sobolev A.M. Sailanbek S. Jandaolet Q.
1 September 2025EDP Sciences
Astronomy and Astrophysics
2025#701
Aims. G53 is an active star formation region with approximately 300 young stellar object (YSO) candidates and exhibits a long filament in CO (VLSR ~ 23 km s–1). To date, there has been no detailed study of its filament characteristics. We therefore explored the kinematics of the filament in the G53 region and the star formation activities triggered along it by combining data from various facilities. Methods. We primarily utilized archival 13CO (1–0) data from the Galactic Ring Survey and NH3(1,1) observations from the Nanshan 26-meter radio telescope. Additionally, we incorporated 12CO (3–2) data from the CO High-Resolution Survey, as well as infrared data from Spitzer and Herschel, to study the G53 region. NH3 (1,1) was used to trace the ends of the molecular cloud G53 (G53W and G53E), while 13CO (1–0) was used to map the entire molecular cloud. We used CRISPY to identify the filament spine in the 13CO (1–0) position-position-velocity cube. Position-velocity diagrams along the filament spine were analyzed to extract kinematic information. Numerical simulations of a turbulent filament were conducted for comparison with the observed kinematics of G53. Additionally, YSOs in G53 were collected to evaluate the star formation activity. Results. The velocity-integrated intensity map of 13CO (1–0) and the H2 column density map indicate that the filament G53 appears to be undergoing an end-dominated collapse (EDC) process. Position-velocity diagrams of 13CO (1–0) show that in G53W, the clumps C2 and C4 are possibly moving toward each other while accreting surrounding material. Our numerical simulations of the EDC scenario indicate that an isothermal filament initially fragments into several clumps due to turbulence, which subsequently merge at the ends. This further adds to the credibility of our hypothesis regarding the approaching motion of C2 and C4 in G53W. NH3 signals are detected only in the G53W and G53E regions, with significantly stronger signals in G53W. In G53W, the NH3(14) data reveal a hub-filament system (HFS) centered around C2. The analysis of NH3(1,1) shows a strong correlation between the magnitude of the velocity gradient and the velocity dispersion in the G53W region, suggesting that the accumulation of material in this area contributes to large-scale turbulence. Additionally, C2, located at the center of the HFS, exhibits a higher star formation efficiency than other regions in G53.
ISM: kinematics and dynamics , ISM: molecules , ISM: structure , stars: formation
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Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, 830011, China
University of Chinese Academy of Sciences, Beijing, 100080, China
State Key Laboratory of Radio Astronomy and Technology, A20 Datun Road, Chaoyang District, Beijing, 100101, China
Xinjiang Key Laboratory of Radio Astrophysics, Urumqi, 830011, China
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, Bonn, 53121, Germany
Energetic Cosmos Laboratory, Nazarbayev University, Astana, 010000, Kazakhstan
Netherlands Institute for Radio Astronomy, ASTRON, Dwingeloo, 7991 PD, Netherlands
Ural Federal University, 19 Mira Street, Ekaterinburg, 620002, Russian Federation
Department of Electronics and Astrophysics, Faculty of Physics and Technology, Al-Farabi Kazakh National University, Almaty, 050040, Kazakhstan
Xinjiang Astronomical Observatory
University of Chinese Academy of Sciences
State Key Laboratory of Radio Astronomy and Technology
Xinjiang Key Laboratory of Radio Astrophysics
Max-Planck-Institut für Radioastronomie
Energetic Cosmos Laboratory
Netherlands Institute for Radio Astronomy
Ural Federal University
Department of Electronics and Astrophysics
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