  Supernova (SN) 1987A offers a unique opportunity to study how a spatially
resolved SN evolves into a young supernova remnant (SNR). We present and
analyze Hubble Space Telescope (HST) imaging observations of SN 1987A obtained
in 2022 and compare them with HST observations from 2009 to 2021. These
observations allow us to follow the evolution of the equatorial ring (ER), the
rapidly expanding ejecta, and emission from the center over a wide range in
wavelength from 2000 to 11 000 AA. The ER has continued to fade since it
reached its maximum ~8200 days after the explosion. In contrast, the ejecta
brightened until day ~11000 before their emission levelled off; the west side
brightened more than the east side, which we attribute to the stronger X-ray
emission by the ER on that side. The asymmetric ejecta expand homologously in
all filters, which are dominated by various emission lines from hydrogen,
calcium, and iron. From this overall similarity, we infer the ejecta are
chemically well-mixed on large scales. The exception is the diffuse morphology
observed in the UV filters dominated by emission from the Mg II resonance lines
that get scattered before escaping. The 2022 observations do not show any sign
of the compact object that was inferred from highly-ionized emission near the
remnant's center observed with JWST. We determine an upper limit on the flux
from a compact central source in the [O III] HST image. The non-detection of
this line indicates that the S and Ar lines observed with JWST originate from
the O free inner Si - S - Ar rich zone and/or that the observed [O III] flux is
strongly affected by dust scattering.
