  JWST/NIRCam obtained high angular-resolution (0.05-0.1''), deep near-infrared
1--5 micron imaging of Supernova (SN) 1987A taken 35 years after the explosion.
In the NIRCam images, we identify: 1) faint H2 crescents, which are emissions
located between the ejecta and the equatorial ring, 2) a bar, which is a
substructure of the ejecta, and 3) the bright 3-5 micron continuum emission
exterior to the equatorial ring. The emission of the remnant in the NIRCam
1-2.3 micron images is mostly due to line emission, which is mostly emitted in
the ejecta and in the hot spots within the equatorial ring. In contrast, the
NIRCam 3-5 micron images are dominated by continuum emission. In the ejecta,
the continuum is due to dust, obscuring the centre of the ejecta. In contrast,
in the ring and exterior to the ring, synchrotron emission contributes a
substantial fraction to the continuum.
  Dust emission contributes to the continuum at outer spots and diffuse
emission exterior to the ring, but little within the ring. This shows that dust
cooling and destruction time scales are shorter than the synchrotron cooling
time scale, and the time scale of hydrogen recombination in the ring is even
longer than the synchrotron cooling time scale.
  With the advent of high sensitivity and high angular resolution images
provided by JWST/NIRCam, our observations of SN 1987A demonstrate that NIRCam
opens up a window to study particle-acceleration and shock physics in
unprecedented details, probed by near-infrared synchrotron emission, building a
precise picture of how a SN evolves.
