Giant Molecular Cloud Formation at the Interface of Colliding Supershells in the Large Magellanic Cloud
arXiv:2104.14191 · doi:10.1093/mnras/stab1202
Abstract
We investigate the Hi envelope of the young, massive GMCs in the star-forming regions N48 and N49, which are located within the high column density Hi ridge between two kpc-scale supergiant shells, LMC 4 and LMC 5. New long-baseline Hi 21 cm line observations with the Australia Telescope Compact Array (ATCA) were combined with archival shorter baseline data and single dish data from the Parkes telescope, for a final synthesized beam size of 24.75" by 20.48", which corresponds to a spatial resolution of ~ 6 pc in the LMC. It is newly revealed that the Hi gas is highly filamentary, and that the molecular clumps are distributed along filamentary Hi features. In total 39 filamentary features are identified and their typical width is ~ 21 (8-49) [pc]. We propose a scenario in which the GMCs were formed via gravitational instabilities in atomic gas which was initially accumulated by the two shells and then further compressed by their collision. This suggests that GMC formation involves the filamentary nature of the atomic medium.
arXiv comment22 pages, 4 tables, 16 figures
References in corpus (44)
- Planck 2013 results. XI. All-sky model of thermal dust emission
- Characterizing interstellar filaments with Herschel in IC5146
- Structure of Stationary Photodissociation Fronts
- Spitzer Survey of the Large Magellanic Cloud, Surveying the Agents of a Galaxy's Evolution (SAGE) I: Overview and Initial Results
- The persistent cosmic web and its filamentary structure I: Theory and implementation
- Structural Analysis of Molecular Clouds: Dendrograms
- An Origin of Supersonic Motions in Interstellar Clouds
- Global Hierarchical Collapse In Molecular Clouds. Towards a Comprehensive Scenario
- GASS: The Parkes Galactic All-Sky Survey. I. Survey Description, Goals, and Initial Data Release
- Thermal condensation in a turbulent atomic hydrogen flow
- The Second Survey of the Molecular Clouds in the Large Magellanic Cloud by NANTEN I: Catalog of Molecular Clouds
- The Magellanic Mopra Assessment (MAGMA). I. The Molecular Cloud Population of the Large Magellanic Cloud
- Molecular Cloud Formation in Shock-Compressed Layers
- The Formation and Destruction of Molecular Clouds and Galactic Star Formation
- A New Look at the Large-Scale HI Structure of the LMC
- Magnetically Aligned HI Fibers and the Rolling Hough Transform
- The Birth of Molecular Clouds: Formation of Atomic Precursors in Colliding Flows
- GASS: The Parkes Galactic All-Sky Survey. II. Stray-Radiation Correction and Second Data Release
- Formation of Structure in Molecular Clouds: A Case Study
- Ages and Luminosities of Young SMC/LMC Star Clusters and the recent Star Formation History of the Clouds
- Formation of Turbulent and Magnetized Molecular Clouds via Accretion Flows of HI Clouds
- Two-Fluid MHD Simulations of Converging HI Flows in the Interstellar Medium. I: Methodology and Basic Results
- How long does it take to form a molecular cloud?
- The two molecular clouds in RCW 38; evidence for formation of the youngest super star cluster in the Milky Way triggered by cloud-cloud collision
- The Galactic Center Cloud G0.253+0.016: A Massive Dense Cloud with low Star Formation Potential
- Two-Fluid MHD Simulations of Converging Hi Flows in the Interstellar Medium. II: Are Molecular Clouds Generated Directly from Warm Neutral Medium?
- On the structure of the turbulent interstellar atomic hydrogen. I- Physical characteristics
- Effects of Magnetic Field Strength and Orientation on Molecular Cloud Formation
- Molecular and Atomic Gas in the Large Magellanic Cloud II. Three-dimensional Correlation between CO and HI
- Cold and Warm Atomic Gas around the Perseus Molecular Cloud. II. The Impact of High Optical Depth on the HI Column Density Distribution and Its Implication for the HI-to-H2 Transition
- Optically thick HI dominant in the local interstellar medium; an alternative interpretation to "dark gas"
- Formation of Cold Filamentary Structure from Wind Blown Superbubbles
- Dust-Gas Scaling Relations and OH Abundance in the Galactic ISM
- CARMA Large Area Star Formation Survey: Structure and Kinematics of Dense Gas in Serpens Main
- HI, CO, and Planck/IRAS dust properties in the high-latitude-cloud complex, MBM 53, 54, 55 and HLCG 92-35; Possible evidence for an optically thick HI envelope around the CO clouds
- Kinematic Structure of Molecular Gas around High-mass Star YSO, Papillon Nebula, in N159 East in the Large Magellanic Cloud
- Formation of the active star forming region LHA 120-N 44 triggered by tidally-driven colliding HI flows
- CARMA Large Area Star Formation Survey: Project Overview with Analysis of Dense Gas Structure and Kinematics in Barnard 1
- The role of magnetic fields in the structure and interaction of supershells
- Optically thick HI does not dominate dark gas in the local ISM
- A Catalog of HI Clouds in the Large Magellanic Cloud
- Synthetic Observations of 21cm HI Line Profiles from Inhomogeneous Turbulent Interstellar HI Gas with Magnetic Field
- A Young GMC Formed at the Interface of Two Colliding Supershells: Observations Meet Simulations
- Dense Molecular Clumps associated with the LMC Supergiant Shells LMC 4 \& LMC 5
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- The R136 star cluster dissected with Hubble Space Telescope/STIS. III. The most massive stars and their clumped winds
- Quantifying the energy balance between the turbulent ionised gas and young stars
- Metallicity Dependence of Molecular Cloud Hierarchical Structure at Early Evolutionary Stages
- Properties of star formation of the Large Magellanic Cloud as probed by young stellar objects
- Influence of protostellar jets and HII regions on the formation and evolution of stellar clusters