The Complex Structure of the Multi-Phase Galactic Wind in a Starburst Merger

TL;DR

This study maps and analyzes the complex multi-phase neutral and ionized outflows in a ULIRG, revealing asymmetries and unique kinematic features that differ from typical galaxy outflows.

Contribution

First 2-D kinematic mapping of neutral outflows in a ULIRG using IFU, revealing complex asymmetries and differences from quiescent galaxy outflows.

Findings

Neutral outflow extends at least 3 kpc from nucleus.

Outflow velocities show a major-axis gradient opposite to disk rotation.

Ionized and neutral outflows are decoupled and asymmetric.

Abstract

Neutral outflows have been detected in many ultraluminous infrared galaxies (ULIRGs) via the Na I D $\lambda\lambda 5890, 5896$ absorption-line doublet. For the first time, we have mapped and analyzed the 2-D kinematics of a cool neutral outflow in a ULIRG, F10565+2448, using the integral field unit (IFU) on Gemini North to observe the Na I D feature. At the same time we have mapped the ionized outflow with the [NII] and H$\alpha$ emission lines. We find a systemic rotation curve that is consistent with the rotation of the molecular disk determined from previous CO observations. The absorption lines show evidence of a nuclear outflow with a radial extent of at least 3 kpc, consistent with previous observations. The strength of the Na I D lines have a strong, spatially resolved correlation with reddening, suggesting that dust is present in the outflow. Surprisingly, the outflow velocities of the neutral gas show a strong asymmetry in the form of a major-axis gradient that is opposite in sign to disk rotation. This is inconsistent with entrained material rotating along with the galaxy or with a tilted minor-axis outflow. We hypothesize that this unusual behavior is due to an asymmetry in the distribution of the ambient gas. We also see evidence of asymmetric ionized outflow in the emission-line velocity map, which appear to be decoupled from the neutral outflow. Our results strengthen the hypothesis that ULIRG outflows differ in morphology from those in more quiescent disk galaxies.