  Dark Energy (DE) acts as a repulsive force that opposes gravitational
attraction. Assuming galaxies maintain a steady state over extended periods,
the estimated upper bound on DE studies its resistance to the attractive
gravitational force from dark matter. Using the SPARC dataset, we fit the
Navarro-Frenk-White (NFW) and Hernquist models to identify the most suitable
galaxies for these models. Introducing the presence of DE in these galaxies
helps establish the upper limit on its repulsive force. This upper bound on DE
sits around $\rho_{\left(<\Lambda\right)} \sim 10^{-25}$~kg/m$^3$, only two
orders of magnitude higher than the one measured by Planck. We discuss the
conditions for detecting DE in different systems and show the consistency of
the upper bound from galaxies to other systems. The upper bound is of the same
order of magnitude as $\rho_{200} = 200 \rho_c$ for both dark matter profiles.
We also address the implications for future measurements on that upper bound
and the condition for detecting the impact of $\Lambda$ on galactic scales.
