The filamentary structures in the CO emission toward the Milky Way disk

Abstract

We present a statistical study of the filamentary structure orientation in the CO emission observations obtained in the Milky Way Imaging Scroll Painting (MWISP) survey in the range $25.8°<l<49.7°$, $|b|\le 1.25°$, and $-100<v_{\mathrm{LSR}}<135$ km/s. We found that most of the filamentary structures in the ${}^{12}$CO and ${}^{13}$CO emission do not show a global preferential orientation either parallel or perpendicular to the Galactic plane. However, we found ranges in Galactic longitude and radial velocity where the ${}^{12}$CO and ${}^{13}$CO filamentary structures are parallel to the Galactic plane. These preferential orientations are different from those found for the HI emission. We consider this an indication that the molecular structures do not simply inherit these properties from parental atomic clouds. Instead, they are shaped by local physical conditions, such as stellar feedback, magnetic fields, and Galactic spiral shocks.

arXiv commentAccepted for publication in Astronomy & Astrophysics (7 pages, 7 figures). arXiv admin note: text overlap with arXiv:2007.07285

References in corpus (50)

• Binary companions of evolved stars in APOGEE DR14: Search method and catalog of ~5,000 companions
• Star Formation in the Milky Way and Nearby Galaxies
• Structure of Stationary Photodissociation Fronts
• Star Clusters Across Cosmic Time
• Re-examining Larson's Scaling Relationships in Galactic Molecular Clouds
• The Boston University-Five College Radio Astronomy Observatory Galactic Ring Survey
• Planck intermediate results. XXXV. Probing the role of the magnetic field in the formation of structure in molecular clouds
• Physical properties of molecular clouds for the entire Milky Way disk
• The SILCC (SImulating the LifeCycle of molecular Clouds) project: I. Chemical evolution of the supernova-driven ISM
• A Parallax-based Distance Estimator for Spiral Arm Sources
• On the Relationship Between Molecular Hydrogen and Carbon Monoxide Abundances in Molecular Clouds
• Three-phase Interstellar medium in Galaxies Resolving Evolution with Star formation and Supernova feedback (TIGRESS): Algorithms, Fiducial model, and Convergence
• The Vertical Structure of the Outer Milky Way HI Disk
• Magnetically Aligned HI Fibers and the Rolling Hough Transform
• FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45-m telescope (FUGIN) I: Project Overview and Initial Results
• The Milky Way Imaging Scroll Painting (MWISP): Project Details and Initial Results from the Galactic Longitude of 25.8deg to 49.7deg
• Numerical Simulations of Multiphase Winds and Fountains from Star-Forming Galactic Disks: I. Solar Neighborhood TIGRESS Model
• Large-scale filaments associated with Milky Way spiral arms
• Giant Molecular Filaments in the Milky Way
• The Bones of the Milky Way
• The identification of filaments on far infrared and submillimiter images. Morphology, physical conditions and relation with star formation of filamentary structure
• The molecular cloud lifecycle
• Simulations of magnetized multiphase galactic disk regulated by supernovae explosions
• Two Mass Distributions in the L 1641 Molecular Clouds: The Herschel connection of Dense Cores and Filaments in Orion A
• Quantifying Observational Projection Effects Using Molecular Cloud Simulations
• The modelling of feedback in star formation simulations
• ATLASGAL -- A Galaxy-wide sample of dense filamentary structures
• The Cloud Factory I: Generating resolved filamentary molecular clouds from galactic-scale forces
• The Physical Properties of Large-Scale Galactic Filaments
• The Skeleton of the Milky Way
• Simulations of the star-forming molecular gas in an interacting M51-like galaxy
• Gas Accretion via Condensation and Fountains
• Discovery of a Population of HI Clouds in the Galactic Halo
• Distribution and mass of diffuse and dense CO gas in the Milky Way
• Cold Milky Way Hi gas in filaments
• An application of an optimal statistic for characterising relative orientations
• Relative Alignment Between the Magnetic Field and Molecular Gas Structure in the Vela C Giant Molecular Cloud using Low and High Density Tracers
• From diffuse gas to dense molecular cloud cores
• The HI/OH/Recombination line survey of the inner Milky Way (THOR): data release 2 and HI overview
• Histogram of oriented gradients: a technique for the study of molecular cloud formation
• Interstellar Turbulence Driving by Galactic Spiral Shocks
• The FRIGG project: From intermediate galactic scales to self-gravitating cores
• The history of dynamics and stellar feedback revealed by the HI filamentary structure in the disk of the Milky Way
• Dynamical cloud formation traced by atomic and molecular gas
• Autonomous Gaussian decomposition of the Galactic Ring Survey. I. Global statistics and properties of the 13CO emission data
• The relative orientation between the magnetic field and gradients of surface brightness within thin velocity slices of 12CO and 13CO emission from the Taurus molecular cloud
• Dense Gas in a Giant Molecular Filament
• Kinetic Tomography. II. A second method for mapping the velocity field of the Milky Way Interstellar Medium and a comparison with spiral structure models
• Atomic and molecular gas properties during cloud formation
• Fourier-space combination of Planck and Herschel images

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• The Impact of Expanding HII Regions on Filament G37:Curved Magnetic Field and Multiple Direction Material Flows
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