The magnetic fields of starburst galaxies. I. Identification and characterization of the thermal polarization in the galactic disk and outflow

TL;DR

This study uses far-infrared polarization observations to map and characterize magnetic fields in the disks and outflows of three nearby starburst galaxies, revealing differences in dust properties and magnetic field structures.

Contribution

It provides the first detailed polarization-based analysis of magnetic fields in starburst galaxy outflows across multiple wavelengths and resolutions.

Findings

Polarized SEDs distinguish disks from outflows effectively.

Outflows have higher dust temperatures and emissivities than disks.

Magnetic fields extend up to 4 kpc and correlate with star formation rate.

Abstract

Far-infrared polarized emission by means of magnetically aligned dust grains is an excellent tracer of the magnetic fields (B-fields) in the cold phase of the galactic outflows in starburst galaxies. We present a comprehensive study of the B-fields in three nearby ($3.5$-$17.2$ Mpc) starbursts (M82, NGC 253, and NGC 2146) at $5$ pc-$1.5$ kpc resolutions using publicly available $53$-$890$ $\mu$m imaging polarimetric observations with SOFIA/HAWC+, JCMT/POL-2, and ALMA. We find that the polarized spectral energy distributions (SEDs) of the full galaxies are dominated by the polarized SEDs of the outflows with dust temperatures of $T_{\rm{d,outflow}}^{\rm{PI}}\sim45$ K and emissive index of $\beta_{\rm{outflow}}^{\rm{PI}}\sim2.3$. The disks are characterized by low $T_{\rm{d,disk}}^{\rm{PI}}=[24,31]$ K and $\beta_{\rm{disk}}^{\rm{PI}}\sim1$. We show that disk- and outflow-dominated galaxies can be better distinguished by using polarized SEDs instead of total SEDs. We compute the $53$-$850$ $\mu$m polarization spectrum of the disk and outflow and find that dust models of the diffuse ISM can reproduce the fairly constant polarization spectrum of the disk, $\langle P_{\rm{disk}} \rangle=1.2\pm0.5$%. The dust models of heterogenous clouds and two temperature components are required to explain the polarization spectrum of the outflow ($2$-$4$% at $53$ $\mu$m, $\sim1$% at $850$ $\mu$m, and a minimum within $89$-$154$ $\mu$m). We conclude that the polarized dust grains in the outflow arise from a dust population with higher dust temperature and emissivities than those from the total flux. The B-fields of the outflows have maximum extensions within $89$-$214$ $\mu$m reaching heights of $\sim4$ kpc, and flatter polarized fluxes than total fluxes. The extension of the B-field permeating the circumgalactic medium increases with increasing the star formation rate.