The Magnetic Fields of the Dusty Nuclei and Molecular Outflows of Arp 220

Abstract Galaxy mergers trigger starburst activity and galactic outflows that enrich the circumgalactic medium (CGM), profoundly impacting galaxy evolution. These phenomena are intrinsically linked to the physical conditions of the medium, which is permeated by magnetic ( B ) fields affecting its transport and dynamics. Here, we spatially resolve, 0 . ″ 24 (96 pc), the B -fields in the dusty and molecular outflows of Arp 220, the closest (78 Mpc) ultraluminous infrared galaxy hosting two interacting nuclei, denoted as East and West. We perform Atacama Large Millimeter/submillimeter Array 870 μ m dust continuum polarization and CO(3–2) emission line polarization and report the first detection of CO(3–2) emission line polarization through the Goldreich–Kylafis effect in an outflow. Dust polarization shows that Arp 220 E has a spiral-like B -field on the disk with a linear polarization fraction of 0.4% ± 0.1% that may produce the detected circular polarization passing through foreground-aligned dust grains. Arp 220 W reveals a B -field parallel to the red- and blueshifted outflows in both the dust and emission line polarization maps. The outflows show a dust polarization of 0.2%, while the CO(3–2) emission line polarization is 1%–2% at 4 σ –6 σ significance across independent velocity channels. A highly polarized (3%–5%) dusty bridge has a B -field orientation of ∼110° connecting both nuclei. Mean B -field strengths of 1.1 and 9.5 mG for the blue- and redshifted outflows, respectively, are estimated. These strong B -fields are attributed to amplification by compression in nuclear clouds and supernova remnants. This amplified B -field is likely sustained by the turbulent kinetic energy in the outflow and may be critical in directing the transport of metals and cosmic rays into the CGM.