  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.

High Energy Astrophysical Phenomena;Astrophysics of Galaxies;Solar and Stellar Astrophysics