Modeling the Far-Infrared Polarization Spectrum of a High-Mass Star Forming Cloud
arXiv:2407.12917 · doi:10.3847/1538-4357/ad631c
Abstract
The polarization spectrum, or wavelength dependence of the polarization fraction, of interstellar dust emission provides important insights into the grain alignment mechanism of interstellar dust grains. We investigate the far-infrared polarization spectrum of a realistic simulated high-mass star forming cloud under various models of grain alignment and emission. We find that neither a homogeneous grain alignment model nor a grain alignment model that includes collisional dealignment is able to produce the falling spectrum seen in observations. On the other hand, we find that a grain alignment model with grain alignment efficiency dependent on local temperature is capable of producing a falling spectrum that is in qualitative agreement with observations of OMC-1. For the model most in agreement with OMC-1, we find no correlation between temperature and the slope of the polarization spectrum. However, we do find a positive correlation between column density and the slope of the polarization spectrum. We suggest this latter correlation to be the result of wavelength-dependent polarization by absorption.
arXiv comment14 pages, 6 figures, 2 tables; Accepted to ApJ
References in corpus (42)
- SciPy 1.0--Fundamental Algorithms for Scientific Computing in Python
- Array Programming with NumPy
- Astropy: A Community Python Package for Astronomy
- The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package
- The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package
- Dust Grain Size Distributions and Extinction in the Milky Way, LMC, and SMC
- Infrared Emission from Interstellar Dust. II. The Diffuse Interstellar Medium
- Density, Velocity, and Magnetic Field Structure in Turbulent Molecular Cloud Models
- Rosseland and Planck Mean Opacities for Protoplanetary Discs
- High-Mass Star and Massive Cluster Formation in the Milky Way
- Radiative torques: Analytical Model and Basic Properties
- Planck intermediate results. XXXV. Probing the role of the magnetic field in the formation of structure in molecular clouds
- The Effects of Radiative Transfer on Low-Mass Star Formation
- Dispersion of Magnetic Fields in Molecular Clouds. I
- Radiative Torques on Interstellar Grains: II. Grain Alignment
- An Imprint of Molecular Cloud Magnetization in the Morphology of the Dust Polarized Emission
- Dispersion of Magnetic Fields in Molecular Clouds. II
- The Gould's Belt Distances Survey (GOBELINS) II. Distances and structure towards the Orion Molecular Clouds
- Radiative transfer with POLARIS: I. Analysis of magnetic fields through synthetic dust continuum polarization measurements
- Radiation-Hydrodynamic Simulations of Massive Star Formation with Protostellar Outflows
- Polarized Sub-Millimetre Emission from Filamentary Molecular Clouds
- HAWC+/SOFIA Multiwavelength Polarimetric Observations of OMC-1
- Variation in dust properties in a dense filament of the Taurus molecular complex (L1506)
- Using Herschel and Planck observations to delineate the role of magnetic fields in molecular cloud structure
- Magnetized Interstellar Molecular Clouds. I. Comparison Between Simulations and Zeeman Observations
- Submillimeter and Far-Infrared Polarimetric Observations of Magnetic Fields in Star-Forming Regions
- Polarization of Dust Emission in Clumpy Molecular Clouds and Cores
- Change of Magnetic FieldGas Alignment at Gravity-Driven Alfvénic Transition in Molecular Clouds: Implications for Dust Polarization Observations
- New Results on the Submillimeter Polarization Spectrum of the Orion Molecular Cloud
- Dispersion of Magnetic Fields in Molecular Clouds. IV - Analysis of Interferometry Data
- A Stable, Accurate Methodology for High Mach Number, Strong Magnetic Field MHD Turbulence with Adaptive Mesh Refinement: Resolution and Refinement Studies
- Mapping the magnetic field in the Taurus/B211 filamentary cloud with SOFIA HAWC+ and comparing with simulation
- Submillimeter Polarization Spectrum in the Vela C Molecular Cloud
- First Observation of the Submillimeter Polarization Spectrum in a Translucent Molecular Cloud
- A New Method to Trace Three-dimensional Magnetic Field Structure within Molecular Clouds Using Dust Polarization
- The Davis-Chandrasekhar-Fermi Method Revisited
- Submillimeter Polarization Spectrum of the Carina Nebula
- HAWC+/SOFIA Polarimetry in L1688: Relative Orientation of Magnetic Field and Elongated Cloud Structure
- Size limit of superparamagnetic inclusions in dust grains and difficulty of magnetic grain alignment in protoplanetary disks
- The Submillimeter Polarization Spectrum of M17
- Far-Infrared Polarization Spectrum of the OMC-1 Star-Forming Region
- The Transition of Polarized Dust Thermal Emission from the Protostellar Envelope to the Disk Scale