The Milky Way atlas for linear filaments II. clump rotation versus filament orientation
arXiv:2410.12215 · doi:10.1093/mnras/stae2379
Abstract
Dense clumps distributed along filaments are the immediate medium for star formation. Kinematic properties of the clumps, such as velocity gradient and angular momentum, combined with filament orientation, provide important clues to the formation mechanism of filament-clump configurations and the role of filaments in star formation. By cross-matching the Milky Way atlas for linear filaments and the Structure, Excitation and Dynamics of the Inner Galactic Interstellar Medium (SEDIGISM) 13CO (2-1) data, we aim to derive the velocity gradient and its direction, the specific angular momentum (J/M), and the ratio (β) between the rotational energy and gravitational energy of clumps, as well as to investigate the alignment between clump rotation and filament orientation. We found a monotonic increase in J/M as a function of clump size (R), following a power-law relation J/M~\propto~R^{1.5\pm0.2}. The ratio βranges from 1.1~\times~10^{-5} to 0.1, with a median value 1.0~\times~10^{-3}, suggesting that clump rotation provides insignificant support against gravitational collapse. The distribution of the angle between clump rotation and natal filament orientation is random, indicating that the clumps' rotational axes have no discernible correlation with the orientation of their hosting filaments. Counting only the most massive clump in each filament also finds no alignment between clump rotation and filament orientation.
Accepted by MNRAS. 9 pages, 5 figures, 2 tables
References in corpus (26)
- Magnetic Fields and Massive Star Formation
- Properties of Hi-GAL clumps in the inner Galaxy]{The Hi-GAL compact source catalogue. I. The physical properties of the clumps in the inner Galaxy ()
- Large-scale filaments associated with Milky Way spiral arms
- Driven and Decaying Turbulence Simulations of Low-Mass Star Formation: From Clumps to Cores to Protostars
- The Hi-GAL compact source catalogue -- II. The 360° catalogue of clump physical properties
- The SEDIGISM survey: first data release and overview of the Galactic structure
- Supersonic turbulence, filamentary accretion,and the rapid assembly of massive stars and disks
- Alignment Between Protostellar Outflows and Filamentary Structure
- A Census of Large-Scale ( 10 pc), Velocity-Coherent, Dense Filaments in the Northern Galactic Plane: Automated Identification Using Minimum Spanning Tree
- ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- XV. Steady Accretion from Global Collapse to Core Feeding in Massive Hub-filament System SDC335
- The SEDIGISM survey: Molecular clouds in the inner Galaxy
- Evidence of high-mass star formation through multi-scale mass accretion in hub-filament-system clouds
- Probing fragmentation and velocity sub-structure in the massive NGC 6334 filament with ALMA
- Widespread Molecular Outflows in the Infrared Dark Cloud G28.37+0.07: Indications of Orthogonal Outflow-Filament Alignment
- ALMA observations reveal no preferred outflow--filament and outflow--magnetic field orientations
- Large-scale Velocity-coherent Filaments in the SEDIGISM Survey: Association with Spiral Arms and Fraction of Dense Gas
- The Milky Way Atlas for Linear Filaments
- Evolution of the Angular Momentum of Molecular Cloud Cores Formed from Filament Fragmentation
- Resolution-dependent Subsonic Non-thermal Line Dispersion Revealed by ALMA
- Distance, magnetic field and kinematics of a filamentary cloud LDN 1157
- Search for Alignment of Disk Orientations in Nearby Star-Forming Regions: Lupus, Taurus, Upper Scorpius, Ophiuchi, and Orion
- Filament Intersections and Cold Dense Cores in Orion A North
- Rotation of Two Micron All Sky Survey Clumps in Molecular Clouds
- Independent Core Rotation in Massive Filaments in Orion
- Core formation via filament fragmentation and the impact of ambient pressure on it
- A High-Mass Young Star-forming Core Escaping from Its Parental Filament