Multi-scale Magnetic Fields in the Central Molecular Zone: Inference from the Gradient Technique

TL;DR

This study employs the Gradient Technique to map and analyze magnetic fields in the Central Molecular Zone across multiple wavelengths, revealing their dynamic role and alignment with polarization data, down to scales of 0.1 parsecs.

Contribution

The paper introduces the application of the Gradient Technique to multi-wavelength data for detailed magnetic field mapping in the galactic center, demonstrating its consistency with polarization measurements.

Findings

Magnetic fields in the CMZ are aligned with polarization data across multiple wavelengths.

The Gradient Technique effectively traces magnetic fields from 0.1 to 10 parsecs.

Magnetic field components in the Radio Arc are predominantly poloidal.

Abstract

The central molecular zone (CMZ) plays an essential role in regulating the nuclear ecosystem of our Galaxy. To get an insight into the magnetic fields of the CMZ, we employ the Gradient Technique (GT), which is rooted in the anisotropy of magnetohydrodynamic turbulence. Our analysis is based on the data of multiple wavelengths, including molecular emission lines, radio 1.4 GHz continuum image, and Herschel 70 $\mu$m image, as well as ionized [Ne II] and Paschen-alpha emissions. The results are compared with the observations of Planck 353 GHz and High-resolution Airborne Wideband Camera Plus (HWAC+) 53 $\mu$m polarized dust emissions. We map the orientation of the magnetic field at multiple wavelengths across the central molecular zone, including close-ups of the Radio Arc and Sagittarius A West regions, on multi scales from $\sim$ 0.1 pc to 10 pc. The magnetic fields towards the central molecular zone traced by GT are globally compatible with the polarization measurements, accounting for the contribution from the galactic foreground and background. This correspondence suggests that the magnetic field and turbulence are dynamically crucial in the galactic center. We find that the magnetic fields associated with the Arched filaments and the thermal components of the Radio Arc are in good agreement with the HAWC+ polarization. Our measurement towards the non-thermal Radio Arc reveals the poloidal magnetic field components in the galactic center. For Sagittarius A West region, we find a great agreement between the GT measurement using [Ne II] emission and HWAC+ 53 $\mu$m observation. We use GT to predict the magnetic fields associated with ionized Paschen-alpha gas down to scales of 0.1 pc.