  I discuss observational clues concerning episodic mass-loss properties of
massive stars in the time before the final supernova explosion. In particular,
I will focus on the mounting evidence that LBVs and related stars are
candidates for supernova progenitors, even though current paradigms place them
at the end of core-H burning. Namely, conditions in the immediate circumstellar
environment within a few 10$^2$ AU of Type IIn supernovae require very high
progenitor mass-loss rates. Those rates are so high that the only known stars
that come close are LBVs during rare giant eruptions. I will highlight evidence
from observations of some recent extraordinary supernovae suggesting that
explosive or episodic mass loss (a.k.a. LBV eruptions like the 19th century
eruption of Eta Car) occur in the 5-10 years immediately preceding the SN.
Finally, I will discuss some implications for stellar evolution from these SNe,
the most important of which is the observational fact that the most massive
stars can indeed make it to the ends of their lives with substantial H
envelopes intact, even at Solar metallicity.
