The "C": The large Chameleon-Musca-Coalsack cloud
arXiv:2404.09592 · doi:10.1051/0004-6361/202450374
Abstract
Recent advancements in 3D dust mapping have transformed our understanding of the Milky Way's local interstellar medium, enabling us to explore its structure in three spatial dimensions for the first time. In this Letter, we use the most recent 3D dust map by Edenhofer et al. to study the well-known Chameleon, Musca, and Coalsack cloud complexes, located about 200 pc from the Sun. We find that these three complexes are not isolated but rather connect to form a surprisingly well-defined half-ring, constituting a single C-shaped cloud with a radius of about 50 pc, a thickness of about 45 pc, and a total mass of about , or if including everything in the vicinity of the C-shaped cloud. Despite the absence of an evident feedback source at its center, the dynamics of young stellar clusters associated with the C structure suggest that a single supernova explosion about 4 Myr to 10 Myr ago likely shaped this structure. Our findings support a single origin story for these cloud complexes, suggesting that they were formed by feedback-driven gas compression, and offer new insights into the processes that govern the birth of star-forming clouds in feedback-dominated regions, such as the Scorpius-Centaurus association.
arXiv comment6 pages, 3 figures, to be published in Astronomy & Astrophysics (A&A)
References in corpus (58)
- Gaia Data Release 3: Summary of the content and survey properties
- Interstellar Dust Grains
- Local Kinematics and the Local Standard of Rest
- galpy: A Python Library for Galactic Dynamics
- A 3D Dust Map Based on Gaia, Pan-STARRS 1 and 2MASS
- Planck 2013 results. XI. All-sky model of thermal dust emission
- The GALAH+ Survey: Third Data Release
- Galactic Reddening in 3D from Stellar Photometry - An Improved Map
- Momentum Injection by Supernovae in the Interstellar Medium
- Gaia-2MASS 3D maps of Galactic interstellar dust within 3 kpc
- Gaia Data Release 3 Properties and validation of the radial velocities
- Improving the open cluster census. II. An all-sky cluster catalogue with Gaia DR3
- A Large Catalog of Accurate Distances to Local Molecular Clouds: The Gaia DR2 Edition
- Three-dimensional mapping of the local interstellar medium with composite data
- The Formation and Destruction of Molecular Clouds and Galactic Star Formation
- A Compendium of Distances to Molecular Clouds in the Star Formation Handbook
- Star formation near the Sun is driven by expansion of the Local Bubble
- 3D maps of interstellar dust in the Local Arm: using , 2MASS and APOGEE-DR14
- Updated Gaia-2MASS 3D maps of Galactic interstellar dust
- Three-dimensional interstellar dust reddening maps of the Galactic plane
- A Galactic-scale gas wave in the Solar Neighborhood
- A parsec-scale Galactic 3D dust map out to 1.25 kpc from the Sun
- Resolving nearby dust clouds
- Parameters of 220 million stars from Gaia BP/RP spectra
- Three-dimensional extinction maps: Inverting inter-calibrated extinction catalogues
- Mapping Distances Across the Perseus Molecular Cloud Using CO Observations, Stellar Photometry, and Gaia DR2 Parallax Measurements
- The Musca cloud: A 6 pc-long velocity-coherent, sonic filament
- The star formation history of the Sco-Cen association. Coherent star formation patterns in space and time
- On the Three-Dimensional Structure of Local Molecular Clouds
- Modeling the magnetized Local Bubble from dust data
- Gravitational fragmentation caught in the act: the filamentary Musca molecular cloud
- Variable structures in M87* from space, time and frequency resolved interferometry
- Significance Mode Analysis (SigMA) for hierarchical structures. An application to the Sco-Cen OB association
- Charting nearby dust clouds using Gaia data only
- Formation of the Musca filament: Evidence for asymmetries in the accretion flow due to a cloud-cloud collision
- The role of magnetic fields in the structure and interaction of supershells
- Magnetic Seismology of Interstellar Gas Clouds: Unveiling a Hidden Dimension
- Detection of the Milky Way spiral arms in dust from 3D mapping
- Inferring the three-dimensional distribution of dust in the Galaxy with a non-parametric method: Preparing for Gaia
- Detailed 3D structure of OrionA in dust with Gaia DR2
- The Radcliffe Wave is Oscillating
- Local Interstellar Medium Kinematics towards the Southern Coalsack and Chamaeleon-Musca dark clouds
- Three-dimensional dust density structure of the Orion, Cygnus X,Taurus, and Perseus star-forming regions
- Dense gas formation in the Musca filament due to the dissipation of a supersonic converging flow
- FEDReD II : 3D Extinction Map with 2MASS and Gaia DR2 data
- 3D shape explains star formation mystery of California and Orion A
- Re-Envisioning Numerical Information Field Theory (NIFTy.re): A Library for Gaussian Processes and Variational Inference
- The Coalsack near and far
- Bayesian radio interferometric imaging with direction-dependent calibration
- The Corona Australis star formation complex is accelerating away from the Galactic plane
- Bayesian inference of three-dimensional gas maps: II. Galactic HI
- Star formation in Chamaeleon I and III: a molecular line study of the starless core population
- Description of turbulent dynamics in the interstellar medium: multifractal/microcanonical analysis I. Application to Herschel observations of the Musca filament
- FEDReD I: 3D extinction and stellar maps by Bayesian deconvolution
- Spectroscopic Confirmation of a Population of Isolated, Intermediate-Mass YSOs
- On the 3D Curvature and Dynamics of the Musca filament
- The Musca molecular cloud: The perfect "filament" is still a sheet
- Fast-Cadence High-Contrast Imaging with Information Field Theory