A New Optical Polarization Catalog for the Small Magellanic Cloud: The Magnetic Field Structure

TL;DR

This study presents a comprehensive optical polarization catalog for the Small Magellanic Cloud, revealing complex magnetic field structures and estimating magnetic field strengths, which enhances understanding of the galaxy's interstellar magnetic environment.

Contribution

It provides the largest optical polarization catalog for the SMC and offers new insights into its magnetic field structure and strength, especially the ordered and turbulent components.

Findings

Identified three main magnetic field trends at specific position angles.

Estimated the ordered magnetic field strength as approximately 0.95 μG.

Found the magnetic field is predominantly on the plane of the sky, with a ratio similar to the Milky Way.

Abstract

We present a new optical polarimetric catalog for the Small Magellanic Cloud (SMC). It contains a total of 7207 stars, located in the Northeast (NE) and Wing sections of the SMC and part of the Magellanic Bridge. This new catalog is a significant improvement compared to previous polarimetric catalogs for the SMC. We used it to study the sky-projected interstellar magnetic field structure of the SMC. Three trends were observed for the ordered magnetic field direction at position angles of $(65 \pm 10)$ deg, $(115 \pm 10)$ deg, and $(150 \pm 10)$ deg. Our results suggest the existence of an ordered magnetic field aligned with the Magellanic Bridge direction and SMC's Bar in the NE region, which have position angles roughly at $115.4$ deg and $45$ deg, respectively. However, the overall magnetic field structure is fairly complex. The trends at $115$ deg and $150$ deg may be correlated with the SMC's bimodal structure, observed in Cepheids' distances and HI velocities. We derived a value of $B_{sky} = (0.947 \pm 0.079)~\mu G$ for the ordered sky-projected magnetic field, and $\delta B = (1.465 \pm 0.069)~\mu G$ for the turbulent magnetic field. This estimate of $B_{sky}$ is significantly larger (by a factor of $\sim10$) than the line-of-sight field derived from Faraday rotation observations, suggesting that most of the ordered field component is on the plane of the sky. A turbulent magnetic field stronger than the ordered field agrees with observed estimates for other irregular and spiral galaxies. For the SMC the $B_{sky}/\delta B$ ratio is closer to what is observed for our Galaxy than other irregular dwarf galaxies.