# A 3D view of molecular hydrogen in Supernova 1987A

## TL;DR

This study presents 3D mapping of molecular hydrogen in Supernova 1987A, revealing its distribution, excitation mechanisms, and relation to other ejecta components, providing insights into supernova chemistry and explosion dynamics.

## Contribution

It provides the first detailed 3D spatial and velocity distribution of H_2 in SN 1987A using new VLT/SINFONI data, highlighting its formation and excitation in the ejecta.

## Key findings

- H_2 emission is dominated by a single southern clump.
- H_2 is powered by 44Ti decay, not X-ray emission.
- Brightest H_2 regions differ from dust and other molecules.

## Abstract

Supernova (SN) 1987A is the only young SN in which H_2 has been detected in the ejecta. The properties of the H_2 are important for understanding the explosion and the ejecta chemistry. Here, we present new VLT/SINFONI observations of H_2 in SN 1987A, focussing on the 2.12 \mu m (1,0)S(1) line. We find that the 3D emissivity is dominated by a single clump in the southern ejecta, with weaker emission being present in the north along the plane of the circumstellar ring. The lowest observed velocities are in the range 400-800 km/s, in agreement with previous limits on inward mixing of H. The brightest regions of H_2 coincide with faint regions of H\alpha, which can be explained by H\alpha being powered by X-ray emission from the ring, while the H_2 is powered by 44Ti. A comparison with ALMA observations of other molecules and dust shows that the brightest regions of H_2, CO and SiO occupy different parts of the inner ejecta and that the brightest H_2 clump coincides with a region of very weak dust emission. The latter is consistent with theoretical predictions that the H_2 should form in the gas phase rather than on dust grains.