  The dS swampland conjecture $|\nabla V|/V \geq c$, where $c$ is presumed to
be a positive constant of order unity, implies that the dark energy density of
our Universe can not be a cosmological constant, but mostly the potential
energy of an evolving quintessence scalar field. As the dark energy includes
the effects of the electroweak symmetry breaking and the QCD chiral symmetry
breaking, if the dS swampland conjecture is applicable for the low energy
quintessence potential, it can be applied for the Higgs and pion potential
also. On the other hand, the Higgs and pion potential has the well-known dS
extrema, and applying the dS swampland conjecture to those dS extrema may
provide stringent constraints on the viable quintessence, as well as on the
conjecture itself. We examine this issue and find that the pion dS extremum at
$\cos(\pi_0/f_\pi)=-1$ implies $c\lesssim {\cal O}(10^{-2}-10^{-5})$ for
$arbitrary$ form of the quintessence potential and couplings, where the weaker
bound ($10^{-2}$) is available $only$ for a specific type of quintessence whose
couplings respect the equivalence principle, while the stronger bound
($10^{-5}$) applies for generic quintessence violating the equivalence
principle. We also discuss the possibility to relax this bound with an
additional scalar field, e.g. a light modulus which has a runaway behavior at
the pion dS extremum. We argue that such possibility is severely constrained by
a variety of observational constraints which do not leave a room to
significantly relax the bound. We make a similar analysis for the Higgs dS
extremum at $H=0$, which results in a weaker bound on $c$.
