Matching dust emission structures and magnetic field in high-latitude cloud L1642: comparing Herschel and Planck maps

Abstract

The nearby cloud L1642 is one of only two known very high latitude (|b| > 30 deg) clouds actively forming stars. It is a rare example of star formation in isolated conditions, and can reveal important details of star formation in general, e.g., of the effect of magnetic fields. We compare Herschel dust emission structures and magnetic field orientation revealed by Planck polarization maps in L1642. The high-resolution ($\sim 20"$) Herschel data reveal a complex structure including a dense, compressed central clump, and low density striations. The Planck polarization data (at 10${}^{\prime }$ resolution) reveal an ordered magnetic field pervading the cloud and aligned with the surrounding striations. There is a complex interplay between the cloud structure and large scale magnetic field. This suggests that the magnetic field is closely linked to the formation and evolution of the cloud. CO rotational emission confirms that the striations are connected with the main clumps and likely to contain material either falling into or flowing out of the clumps. There is a clear transition from aligned to perpendicular structures approximately at a column density of $N_{\mathrm{H}}=1.6\times 10^{21}{\mathrm{cm}}^{-2}$. Comparing the Herschel maps with the Planck polarization maps shows the close connection between the magnetic field and cloud structure even in the finest details of the cloud.

accepted to MNRAS; 14 pages; changes: moderate text and figure editing

References in corpus (30)

• Herschel Space Observatory - An ESA facility for far-infrared and submillimetre astronomy
• Theory of Star Formation
• Planck 2013 results. I. Overview of products and scientific results
• Cold Dark Clouds: The Initial Conditions for Star Formation
• The persistent cosmic web and its filamentary structure I: Theory and implementation
• Herschel view of the Taurus B211/3 filament and striations: Evidence of filamentary growth?
• Large-Scale Structure of the Molecular Gas in Taurus Revealed by High Linear Dynamic Range Spectral Line Mapping
• Planck intermediate results. XXXV. Probing the role of the magnetic field in the formation of structure in molecular clouds
• Planck intermediate results. XIX. An overview of the polarized thermal emission from Galactic dust
• Tracing Magnetic Fields with Aligned Grains
• An Imprint of Molecular Cloud Magnetization in the Morphology of the Dust Polarized Emission
• SCUBA Polarization Measurements of the Magnetic Field Strengths in the L183, L1544, and L43 Prestellar Cores
• Magnetically Aligned HI Fibers and the Rolling Hough Transform
• Analysis of the emission of very small dust particles from Spitzer spectro-imagery data using blind signal separation methods
• A Large Catalog of Accurate Distances to Molecular Clouds from PS1 Photometry
• First Observations of the Magnetic Field Geometry in Pre-stellar Cores
• On the origin of non self-gravitating filaments in the ISM
• Planck intermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence
• Galactic cold cores III. General cloud properties
• The Pipe Nebula as seen with Herschel: Formation of filamentary structures by large-scale compression ?
• A novel estimator of the polarization amplitude from normally distributed Stokes parameters
• Neutral hydrogen structures trace dust polarization angle: Implications for cosmic microwave background foregrounds
• Planck intermediate results. XXXIII. Signature of the magnetic field geometry of interstellar filaments in dust polarization maps
• Planck intermediate results. XXXII. The relative orientation between the magnetic field and structures traced by interstellar dust
• Polarization measurements analysis I. Impact of the full covariance matrix on polarization fraction and angle measurements
• Triggered Star Formation on the Border of the Orion-Eridanus Superbubble
• Planck intermediate results. XXXVIII. E- and B-modes of dust polarization from the magnetized filamentary structure of the interstellar medium
• Multiwavelength study of the high-latitude cloud L1642: chain of star formation
• Morphology and kinematics of Lynds 1642
• Polarized Emission from Interstellar Dust

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• Velocity Gradient in the Presence of Self-Gravity: Identifying Gravity-induced Inflow and Determining Collapsing Stage
• Statistical analysis of the interplay between magnetic fields and filaments hosting Planck Galactic Cold Clumps
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• The Simons Observatory: Galactic Science Goals and Forecasts
• The Hough Stream Spotter: A New Method for Detecting Linear Structure in Resolved Stars and Application to the Stellar Halo of M31
• Dense gas formation in the Musca filament due to the dissipation of a supersonic converging flow
• The JCMT BISTRO-2 Survey: Magnetic Fields of the Massive DR21 Filament
• Galactic cold cores IX. Column density structures and radiative transfer modelling
• Galactic Cold Cores. VIII. Filament formation and evolution: Filament properties in context with evolutionary models
• Large-scale magnetic field in the Monoceros OB-1 East molecular cloud
• A new method for probing magnetic field strengths from striations in the interstellar medium
• Template matching method for the analysis of interstellar cloud structure
• Filamentary Dust Polarization and the Morphology of Neutral Hydrogen Structures
• Magnetic field tomography in two clouds towards Ursa Major using HI fibers
• MaLeFiSenta: Machine Learning for FilamentS Identification and orientation in the ISM
• The Role of Magnetic Fields in the Formation of the Filamentary Infrared Dark Cloud G11.11-0.12
• Synthetic observations of dust emission and polarisation of Galactic cold clumps
• Dust emission, extinction, and scattering in LDN 1642
• Dust polarisation studies on MHD simulations of molecular clouds: methods comparison for the relative orientations analysis
• CO enhancement by magnetohydrodynamic waves; Striations in the Polaris Flare
• Correlation of gas dynamics and dust in the evolved filament G82.65-02.00
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