The magnetic field of the Radcliffe Wave: starlight polarization at nearest approach to the Sun

Abstract

We investigate the geometry of the magnetic field towards the Radcliffe Wave, a coherent 3-kpc-long part of the nearby Local Arm recently discovered via three-dimensional dust mapping. We use archival stellar polarization in the optical and new measurements in the near-infrared to trace the magnetic field as projected on the plane of the sky. Our new observations cover the portion of the structure that is closest to the Sun, between Galactic longitudes of 122${}^{\circ }$ and 188${}^{\circ }$. The polarization angles of stars immediately background to the Radcliffe Wave appear to be aligned with the structure as projected on the plane of the sky. The observed magnetic field configuration is inclined with respect to the Galactic disk at an angle of 18${}^{\circ }$. This departure from a geometry parallel to the plane of the Galaxy is contrary to previous constraints from more distant stars and polarized dust emission. We confirm that the polarization angle of stars at larger distances shows a mean orientation parallel to the Galactic disk. We discuss implications of the observed morphology of the magnetic field for models of the large-scale Galactic magnetic field, as well as formation scenarios for the Radcliffe Wave itself.

arXiv commentSubmitted to A&A

References in corpus (73)

• SciPy 1.0--Fundamental Algorithms for Scientific Computing in Python
• The Gaia mission
• HEALPix -- a Framework for High Resolution Discretization, and Fast Analysis of Data Distributed on the Sphere
• The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package
• dynesty: A Dynamic Nested Sampling Package for Estimating Bayesian Posteriors and Evidences
• Estimating distances from parallaxes. V: Geometric and photogeometric distances to 1.47 billion stars in Gaia Early Data Release 3
• A 3D Dust Map Based on Gaia, Pan-STARRS 1 and 2MASS
• Trigonometric Parallaxes Of High-Mass Star Forming Regions: Our View Of The Milky Way
• A New Model of the Galactic Magnetic Field
• Planck Early Results: The Planck mission
• 9286 Stars: An Agglomeration of Stellar Polarization Catalogs
• Magnetic Fields in Spiral Galaxies
• Planck 2018 results. IV. Diffuse component separation
• Planck intermediate results. XIX. An overview of the polarized thermal emission from Galactic dust
• Planck intermediate results. XXXV. Probing the role of the magnetic field in the formation of structure in molecular clouds
• A Large Catalog of Accurate Distances to Local Molecular Clouds: The Gaia DR2 Edition
• A Compendium of Distances to Molecular Clouds in the Star Formation Handbook
• Magnetically Aligned HI Fibers and the Rolling Hough Transform
• Star formation near the Sun is driven by expansion of the Local Bubble
• Placing Confidence Limits on Polarization Measurements
• Updated Gaia-2MASS 3D maps of Galactic interstellar dust
• Planck 2018 results. XII. Galactic astrophysics using polarized dust emission
• A Galactic-scale gas wave in the Solar Neighborhood
• A parsec-scale Galactic 3D dust map out to 1.25 kpc from the Sun
• The Magnetic Field in Taurus Probed by Infrared Polarization
• Statistical Properties of Galactic Starlight Polarization
• Foreground component separation with generalised ILC
• Parameters of 220 million stars from Gaia BP/RP spectra
• Three-Dimensional Simulations of Parker, Magneto-Jeans, and Swing Instabilities in Shearing Galactic Gas Disks
• Neutral hydrogen structures trace dust polarization angle: Implications for cosmic microwave background foregrounds
• What are we learning from the relative orientation between density structures and the magnetic field in molecular clouds?
• Internal calibration of Gaia BP/RP low-resolution spectra
• Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at 353 GHz with interstellar polarization in the visible
• On the Three-Dimensional Structure of Local Molecular Clouds
• Magnetic Fields in the Milky Way
• Modeling the magnetized Local Bubble from dust data
• An application of an optimal statistic for characterising relative orientations
• On the formation of density filaments in the turbulent interstellar medium
• The Physical Nature of Neutral Hydrogen Intensity Structure
• The magnetic field and dust filaments in the Polaris Flare
• The Per-Tau Shell: A Giant Star-Forming Spherical Shell Revealed by 3D Dust Observations
• The Galactic Faraday depth sky revisited
• Magnetic field morphology in nearby molecular clouds as revealed by starlight and submillimetre polarization
• The magnetic environment of the Orion-Eridanus superbubble as revealed by Planck
• Practical Modeling of Large-Scale Galactic Magnetic Fields: Status and Prospects
• Demonstration of magnetic field tomography with starlight polarization towards a diffuse sightline of the ISM
• The Galactic dynamics revealed by the filamentary structure in atomic hydrogen emission
• The Radcliffe Wave is Oscillating
• The Role of the Parker Instability in Structuring the Interstellar Medium
• Formation of Interstellar Clouds: Parker Instability with Phase Transitions
• The Galactic Magnetic Field's Effect in Star-Forming Region
• The Fan Region at 1.5 GHz. I: Polarized synchrotron emission extending beyond the Perseus Arm
• Evidence of a vertical kinematic oscillation beyond the Radcliffe Wave
• Resolved Magnetic Field Mapping of a Molecular Cloud Using GPIPS
• Starlight-polarization-based tomography of the magnetized interstellar medium: PASIPHAE's line-of-sight inversion method
• A minimum-hypothesis explanation for the Radcliffe Wave: Kelvin-Helmholtz instability
• The Galactic Plane Infrared Polarization Survey (GPIPS): Data Release 4
• The first degree-scale starlight-polarization-based tomography map of the magnetized interstellar medium
• A Unified Model for the Fan Region and the North Polar Spur: A bundle of filaments in the Local Galaxy
• Two-component Magnetic Field along the Line of Sight to the Perseus Molecular Cloud: Contribution of the Foreground Taurus Molecular Cloud
• Interstellar Polarization Survey II: General Interstellar Medium
• Discovery of a coherent, wave-like velocity pattern for the Radcliffe Wave
• A Kpc Scale Molecular Wave in the Inner Galaxy: Feather of the Milky Way?
• The Effect of the Random Magnetic Field Component on the Parker Instability
• Using Red Clump Stars to Decompose the Galactic Magnetic Field with Distance
• Constraining Galactic Magnetic Field Models with Starlight Polarimetry
• A panoptic view of the Taurus molecular cloud I. The cloud dynamics revealed by gas emission and 3D dust
• The RoboPol sample of optical polarimetric standards
• Steady states of the Parker instability
• Characterizing the 3D Kinematics of Young Stars in the Radcliffe Wave
• Three-Dimensional Aquila Rift: Magnetized HI Arch Anchored by Molecular Complex
• Open Clusters as Probes of the Galactic Magnetic Field: I. Cluster Properties
• The Impact of Cosmic Ray Injection on Magnetic Flux Tubes in a Galactic Disk

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