Filamentary Dust Polarization and the Morphology of Neutral Hydrogen Structures
Filamentary structures in neutral hydrogen (H i ) emission are well aligned with the interstellar magnetic field, so H i emission morphology can be used to construct templates that strongly correlate with measurements of polarized thermal dust emission. We explore how the quantification of filament...
| Main Authors: | , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad06aa |
| _version_ | 1797357485326073856 |
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| author | George Halal Susan E. Clark Ari Cukierman Dominic Beck Chao-Lin Kuo |
| author_facet | George Halal Susan E. Clark Ari Cukierman Dominic Beck Chao-Lin Kuo |
| author_sort | George Halal |
| collection | DOAJ |
| description | Filamentary structures in neutral hydrogen (H i ) emission are well aligned with the interstellar magnetic field, so H i emission morphology can be used to construct templates that strongly correlate with measurements of polarized thermal dust emission. We explore how the quantification of filament morphology affects this correlation. We introduce a new implementation of the Rolling Hough Transform (RHT) using spherical harmonic convolutions, which enables efficient quantification of filamentary structure on the sphere. We use this Spherical RHT algorithm along with a Hessian-based method to construct H i -based polarization templates. We discuss improvements to each algorithm relative to similar implementations in the literature and compare their outputs. By exploring the parameter space of filament morphologies with the Spherical RHT, we find that the most informative H i structures for modeling the magnetic field structure are the thinnest resolved filaments. For this reason, we find a ∼10% enhancement in the B -mode correlation with polarized dust emission with higher-resolution H i observations. We demonstrate that certain interstellar morphologies can produce parity-violating signatures, i.e., nonzero TB and EB , even under the assumption that filaments are locally aligned with the magnetic field. Finally, we demonstrate that B modes from interstellar dust filaments are mostly affected by the topology of the filaments with respect to one another and their relative polarized intensities, whereas E modes are mostly sensitive to the shapes of individual filaments. |
| first_indexed | 2024-03-08T14:45:50Z |
| format | Article |
| id | doaj.art-40a224804bdd4a00babab7f024dd048c |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-08T14:45:50Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-40a224804bdd4a00babab7f024dd048c2024-01-11T09:50:53ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-0196112910.3847/1538-4357/ad06aaFilamentary Dust Polarization and the Morphology of Neutral Hydrogen StructuresGeorge Halal0https://orcid.org/0000-0003-2221-3018Susan E. Clark1https://orcid.org/0000-0002-7633-3376Ari Cukierman2https://orcid.org/0000-0002-7471-719XDominic Beck3https://orcid.org/0000-0003-0848-2756Chao-Lin Kuo4Department of Physics, Stanford University , Stanford, CA 94305, USA ; georgech@stanford.edu; Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University , Stanford, CA 94305, USADepartment of Physics, Stanford University , Stanford, CA 94305, USA ; georgech@stanford.edu; Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University , Stanford, CA 94305, USADepartment of Physics, Stanford University , Stanford, CA 94305, USA ; georgech@stanford.edu; Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University , Stanford, CA 94305, USA; SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA; Department of Physics, California Institute of Technology , Pasadena, CA 91125, USADepartment of Physics, Stanford University , Stanford, CA 94305, USA ; georgech@stanford.edu; Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University , Stanford, CA 94305, USA; SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USADepartment of Physics, Stanford University , Stanford, CA 94305, USA ; georgech@stanford.edu; Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University , Stanford, CA 94305, USA; SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USAFilamentary structures in neutral hydrogen (H i ) emission are well aligned with the interstellar magnetic field, so H i emission morphology can be used to construct templates that strongly correlate with measurements of polarized thermal dust emission. We explore how the quantification of filament morphology affects this correlation. We introduce a new implementation of the Rolling Hough Transform (RHT) using spherical harmonic convolutions, which enables efficient quantification of filamentary structure on the sphere. We use this Spherical RHT algorithm along with a Hessian-based method to construct H i -based polarization templates. We discuss improvements to each algorithm relative to similar implementations in the literature and compare their outputs. By exploring the parameter space of filament morphologies with the Spherical RHT, we find that the most informative H i structures for modeling the magnetic field structure are the thinnest resolved filaments. For this reason, we find a ∼10% enhancement in the B -mode correlation with polarized dust emission with higher-resolution H i observations. We demonstrate that certain interstellar morphologies can produce parity-violating signatures, i.e., nonzero TB and EB , even under the assumption that filaments are locally aligned with the magnetic field. Finally, we demonstrate that B modes from interstellar dust filaments are mostly affected by the topology of the filaments with respect to one another and their relative polarized intensities, whereas E modes are mostly sensitive to the shapes of individual filaments.https://doi.org/10.3847/1538-4357/ad06aaInterstellar dustInterstellar filamentsMilky Way magnetic fieldsNeutral hydrogen cloudsCosmic microwave background radiationAlgorithms |
| spellingShingle | George Halal Susan E. Clark Ari Cukierman Dominic Beck Chao-Lin Kuo Filamentary Dust Polarization and the Morphology of Neutral Hydrogen Structures The Astrophysical Journal Interstellar dust Interstellar filaments Milky Way magnetic fields Neutral hydrogen clouds Cosmic microwave background radiation Algorithms |
| title | Filamentary Dust Polarization and the Morphology of Neutral Hydrogen Structures |
| title_full | Filamentary Dust Polarization and the Morphology of Neutral Hydrogen Structures |
| title_fullStr | Filamentary Dust Polarization and the Morphology of Neutral Hydrogen Structures |
| title_full_unstemmed | Filamentary Dust Polarization and the Morphology of Neutral Hydrogen Structures |
| title_short | Filamentary Dust Polarization and the Morphology of Neutral Hydrogen Structures |
| title_sort | filamentary dust polarization and the morphology of neutral hydrogen structures |
| topic | Interstellar dust Interstellar filaments Milky Way magnetic fields Neutral hydrogen clouds Cosmic microwave background radiation Algorithms |
| url | https://doi.org/10.3847/1538-4357/ad06aa |
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