Constraining Galactic Magnetic Field Models with Starlight Polarimetry

TL;DR

This study predicts starlight polarization patterns to help distinguish different models of the Galactic magnetic field, focusing on the poloidal component, using simulations and radiative transfer modeling.

Contribution

It introduces a method combining dynamo simulations, dust distributions, and radiative transfer to test and constrain Galactic magnetic field models through polarization predictions.

Findings

Identifies specific sky directions for model discrimination.

Proposes cumulative polarization distributions as diagnostic tools.

Analyzes the impact of magnetic pitch angle on polarization patterns.

Abstract

This paper provides testable predictions about starlight polarizations to constrain the geometry of the Galactic magnetic field, in particular the nature of the poloidal component. Galactic dynamo simulations and Galactic dust distributions from the literature are combined with a Stokes radiative transfer model to predict the observed polarizations and position angles of near-infrared starlight, assuming the light is polarized by aligned anisotropic dust grains. S0 and A0 magnetic field models and the role of magnetic pitch angle are all examined. All-sky predictions are made, and particular directions are identified as providing diagnostic power for discriminating among the models. Cumulative distribution functions of the normalized degree of polarization and plots of polarization position angle vs. Galactic latitude are proposed as tools for testing models against observations.