Three-dimensional distribution of Ejecta in supernova 1987A at 10,000 days

Larsson, J.; Fransson, C.; Spyromilio, J.; Leibundgut, B.; Challis, P.; Chevalier, R. A.; France, K.; Jerkstrand, A.; Kirshner, R. P.; Lundqvist, P.; Matsuura, M.; McCray, R.; Smith, N.; Sollerman, J.; Garnavich, P.; Heng, Kevin; Lawrence, S.; Mattila, S.; Migotto, K.; Sonneborn, G.; ... (2016). Three-dimensional distribution of Ejecta in supernova 1987A at 10,000 days. Astrophysical journal, 833(2), p. 147. Institute of Physics Publishing IOP 10.3847/1538-4357/833/2/147

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Due to its proximity, SN 1987A offers a unique opportunity to directly observe the geometry of a stellar explosion as it unfolds. Here we present spectral and imaging observations of SN 1987A obtained ~10,000 days after the explosion with HST/STIS and VLT/SINFONI at optical and near-infrared wavelengths. These observations allow us to produce the most detailed 3D map of Hα to date, the first 3D maps for [Ca II] λλ7292,7324, [O I] λλ6300,6364, and Mg II λλ9218, 9244, as well as new maps for [Si I]+[Fe II] 1.644 μm and He I 2.058 μm. A comparison with previous observations shows that the [Si I]+[Fe II] flux and morphology have not changed significantly during the past ten years, providing evidence that this line is powered by ⁴⁴Ti. The time evolution of Hα shows that it is predominantly powered by X-rays from the ring, in agreement with previous findings. All lines that have sufficient signal show a similar large-scale 3D structure, with a north–south asymmetry that resembles a broken dipole. This structure correlates with early observations of asymmetries, showing that there is a global asymmetry that extends from the inner core to the outer envelope. On smaller scales, the two brightest lines, Hα and [Si I]+[Fe II] 1.644 μm, show substructures at the level of ~200–1000 km s–1and clear differences in their 3D geometries. We discuss these results in the context of explosion models and the properties of dust in the ejecta.

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