  The properties of blue supergiants are key for constraining the end of the
main sequence (MS) of massive stars. Whether the observed drop in the relative
number of fast-rotating stars below $\sim$21$\,$kK is due to enhanced mass-loss
rates at the location of the bistability jump, or the result of the end of the
MS is still debated. Here, we combine newly derived estimates of photospheric
and wind parameters with Gaia distances and wind terminal velocities from the
literature to obtain upper limits on the mass-loss rates for a sample of 116
Galactic luminous blue supergiants. The parameter space covered by the sample
ranges between 35-15$\,$kK in $T_{\rm eff}$ and 4.8-5.8$\,$dex in
log(L/L$_{\odot}$). Our results show no increase in the mass-loss rates over
the bistability jump. Therefore, we argue that the drop in rotational
velocities cannot be explained by enhanced mass loss. Since a large jump in the
mass-loss rates is commonly included in evolutionary models, we suggest an
urgent revision of the currently used default prescriptions.
