# Ultraviolet Mg II emission from fast neutral ejecta around Eta Carinae

## TL;DR

This study presents the first UV imaging of eta Carinae's nebula revealing MgII emission that traces unshocked neutral gas, providing new insights into the nebula's structure and mass loss during the Great Eruption.

## Contribution

First UV images of eta Carinae's nebula showing MgII emission, revealing unshocked neutral gas and offering new constraints on polar mass loss.

## Key findings

- MgII emission is concentrated over the poles of the nebula.
- Diffuse MgII emission indicates resonant scattering from unshocked neutral gas.
- Estimated neutral gas mass is about 0.02 solar masses.

## Abstract

We present the first images of the nebula around eta Carinae obtained with HST/WFC3, including a UV image in the F280N filter that traces MgII emission, plus contemporaneous imaging in the F336W, F658N, and F126N filters that trace near-UV continuum, [NII], and [FeII], respectively. The F336W and F658N images are consistent with previous images in these filters, and F126N shows that for the most part, [FeII] 12567 traces clumpy shocked gas seen in [NII]. The F280N image, however, reveals MgII emission from structures that have not been seen in any previous line or continuum images of eta Carinae. This image shows diffuse MgII emission immediately outside the bipolar Homunculus nebula in all directions, but with the strongest emission concentrated over the poles. The diffuse structure with prominent radial streaks, plus an anticorrelation with ionized tracers of clumpy shocked gas, leads us to suggest that this is primarily MgII resonant scattering from unshocked, neutral atomic gas. We discuss the implied structure and geometry of the MgII emission, and its relation to the Homunculus lobes and various other complex nebular structures. An order of magnitude estimate of the neutral gas mass traced by MgII is 0.02Msun, with a corresponding kinetic energy around 1e47erg. This may provide important constraints on polar mass loss in the early phases of the Great Eruption. We argue that the MgII line may be an excellent tracer of significant reservoirs of freely expanding, unshocked, and otherwise invisible neutral atomic gas in a variety of stellar outflows.