The DR21(OH) Trident—Resolving the Massive Ridge into Three Entangled Fibers as the Initial Condition of Cluster Formation

DR21(OH) ridge, the central part of a high-mass star- and cluster-forming hub-filament system, is resolved spatially and kinematically into three nearly parallel fibers (f1, f2, and f3) with a roughly north–south orientation, using the observations of molecular transitions of H 13 CO + (1 − 0), N 2...

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Bibliographic Details
Published in:The Astrophysical journal 2022-03, Vol.927 (1), p.106
Main Authors: Cao, Yue, Qiu, Keping, Zhang, Qizhou, Li, Guang-Xing
Format: Article
Language:English
Subjects:
Astronomy
Astrophysics
Clusters
Dense interstellar clouds
Dust continuum emission
Fibers
Filaments
Interstellar filaments
Interstellar line emission
Massive stars
Star & galaxy formation
Star formation
Star forming regions
Tidal effects
Velocity
Velocity gradient
Young massive clusters
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Summary:DR21(OH) ridge, the central part of a high-mass star- and cluster-forming hub-filament system, is resolved spatially and kinematically into three nearly parallel fibers (f1, f2, and f3) with a roughly north–south orientation, using the observations of molecular transitions of H 13 CO + (1 − 0), N 2 H + (1 − 0), and NH 2 D (1 1,1 − 1 0,1 ) with the Combined Array for Research in Millimeter Astronomy. These fibers are all mildly supersonic ( σ velocity dispersions about 2 times the sound speed), having lengths around 2 pc and widths about 0.1 pc, and they entangle and conjoin in the south where the most active high-mass star formation takes place. They all have line masses 1–2 orders of magnitude higher than their low-mass counterparts and are gravitationally unstable both radially and axially. However, only f1 exhibits high-mass star formation all the way along the fiber, yet f2 and f3 show no signs of significant star formation in their northern parts. A large velocity gradient increasing from north to south is seen in f3, and can be well reproduced with a model of freefall motion toward the most massive and active dense core in the region, which corroborates the global collapse of the ridge and suggests that the disruptive effects of the tidal forces may explain the inefficiency of star formation in f2 and f3. On larger scales, some of the lower-density, peripheral filaments are likely to be the outer extensions of the fibers, and provide hints on the origin of the ridge.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/ac4696