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We present high angular resolution (~80 mas) ALMA continuum images of the SN1987A system, together with CO $J$=2 $\!\rightarrow\!$ 1, $J$=6$\!\rightarrow\!$ 5, and SiO $J$=5 $\!\rightarrow\!$ 4 to $J$=7$\!\rightarrow\!$ 6 images, which clearly resolve the ejecta (dust continuumand molecules) and ring (synchrotron continuum) components. Dust in the ejectais asymmetric and clumpy, and overall the dust fills the spatial void seen inH$\alpha$ images, filling that region with material from heavier elements. Thedust clumps generally fill the space where CO $J$=6 $\!\rightarrow\!$ 5 isfainter, tentatively indicating that these dust clumps and CO are locationallyand chemically linked. In these regions, carbonaceous dust grains might haveformed after dissociation of CO. The dust grains would have cooled byradiation, and subsequent collisions of grains with gas would also cool thegas, suppressing the CO $J$=6 $\!\rightarrow\!$ 5 intensity. The data show adust peak spatially coincident with the molecular hole seen in previous ALMA CO$J$=2 $\!\rightarrow\!$ 1 and SiO $J$=5 $\!\rightarrow\!$ 4 images. That dustpeak, combined with CO and SiO line spectra, suggests that the dust and gascould be at higher temperatures than the surrounding material, though higherdensity cannot be totally excluded. One of the possibilities is that a compactsource provides additional heat at that location. Fits to thefar-infrared--millimeter spectral energy distribution give ejecta dusttemperatures of 18--23K. We revise the ejecta dust mass to $\mathrm{M_{dust}} =0.2-0.4$M$_\odot$ for carbon or silicate grains, or a maximum of$<0.7$M$_\odot$ for a mixture of grain species, using the predictednucleosynthesis yields as an upper limit.

High angular resolution ALMA images of dust and molecules in the SN 1987A ejecta