  We review the pNGB quintessence models, and point out that the reason why the
large decay constants $f_a \ga {\cal O}(1)M_{Pl}$ are really needed is to tame
a tachyonic instability present for a wide range of initial $vev$s. Starting
very close to potential maxima does not help because quantum fluctuations
during early inflation at a scale $H_I$ perturb the quintessence $vev$,
displacing it from the maxima. This issue is quite interesting for pNGB dark
energy in light of the recently discussed difficulties with embedding models
with $f_a > M_{Pl}$ in fundamental theory. A possible way around is provided by
models with several ultralight pNGBs, which can drive a short burst of very
late inflation {\it together} even if all of their decay constants obey $f_a <
M_{Pl}$. Starting with their $vev \sim f_a$, the pNGBs will hold each other up
on the potential for a longer time period. Their effective dynamics is captured
by a collective mode, containing admixtures of all of the rolling pNGBs, which
behaves as an ultralight field with $f_{eff} > M_{Pl}$. We point out that there
may be potentially observable large scale disturbances in the sea of dark
energy in such models.
