Initial Conditions for Star Formation: A Physical Description of the Filamentary ISM
arXiv:2203.09562
Abstract
The interstellar medium contains filamentary structure over a wide range of scales. Understanding the role of this structure, both as a conduit of gas across the scales and a diagnostic tool of local physics, is a major focus of star formation studies. We review recent progress in studying filamentary structure in the ISM, interpreting its properties in terms of physical processes, and exploring formation and evolution scenarios. We include structures from galactic-scale filaments to tenth-of-a-parsec scale filaments, comprising both molecular and atomic structures, from both observational and theoretical perspectives. In addition to the literature overview, we assemble a large amount of catalogue data from different surveys and provide the most comprehensive census of filamentary structures to date. Our census consists of 22 803 filamentary structures, facilitating a holistic perspective and new insights. We use our census to conduct a meta-analysis, leading to a description of filament properties over four orders of magnitudes in length and eight in mass. Our analysis emphasises the hierarchical and dynamical nature of filamentary structures. Filaments do not live in isolation, nor they generally resemble static structures close to equilibrium. We propose that accretion during filament formation and evolution sets some of the key scaling properties of filaments. This highlights the role of accretion during filament formation and evolution and also in setting the initial conditions for star formation. Overall, the study of filamentary structures during the past decade has been observationally driven. While great progress has been made on measuring the basic properties of filaments, our understanding of their formation and evolution is clearly lacking. In this context, we identify a number of directions and questions we consider most pressing for the field.
36 pages, 10 figures. To appear in Protostars and Planets VII, Editors: Shu-ichiro Inutsuka, Yuri Aikawa, Takayuki Muto, Kengo Tomida, and Motohide Tamura
Cited by in corpus (14)
- ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- XI. From inflow to infall in hub-filament systems
- Full-sky Models of Galactic Microwave Emission and Polarization at Sub-arcminute Scales for the Python Sky Model
- Formation of hub-filament structure triggered by cloud-cloud collision in W33 complex
- Three-dimensional magnetic fields of molecular clouds
- The Kinematic Structure of Magnetically Aligned HI Filaments
- Neutral hydrogen filaments in interstellar media: Are they physical?
- Probing the Global Dust Properties and Cluster Formation Potential of the Giant Molecular Cloud G148.24+00.41
- Bimodal orientation distribution and head-tail asymmetry of a sample of filamentary molecular clouds
- Properties of 3D HI Filaments in the Smith High Velocity Cloud
- Polarization fraction of Planck Galactic cold clumps and forecasts for the Simons Observatory
- Impact of the shape of the prestellar density fluctuations on the core mass function
- FIRESTORM I: Stellar Feedback and Gas Kinematics in the Evolved W40 Hub-Filament System
- Non-ideal MHD and protostellar feedback effects on disc formation and evolution in numerical simulations of star cluster formation
- Revealing the Connection Between the Filamentary Hierarchy and Star Cluster Formation in a Simulated NGC 628 Galaxy