We investigate the evolution of the bar fraction and length using an extendedJWST NIRCam imaging dataset of galaxies in the $1 \leq z \leq 4$ redshiftrange. We assess the wavelength dependence of the bar fraction in disc galaxiesand bar length evolution by selecting a nearly mass-complete CEERS disc sampleand performing independent visual classifications on the short (F200W) and long(F356W+F444W) wavelength channels. A similar bar fraction is observed for bothsamples, and combined we find a declining trend in the bar fraction:$0.16^{+0.03}_{-0.03}$ at $1 \leq z < 2$; $0.08^{+0.02}_{-0.01}$ at $2 \leq z <3$; $0.07^{+0.03}_{-0.01}$ at $3 \leq z \leq 4$. This corroborates our previouswork and other recent studies, suggesting that dynamically cold androtationally supported massive discs are present at Cosmic Noon. No evolutionin the F356W+F444W bar length is measured from $z = 4$ to $z = 1$, which has amean of 3.6\,kpc, but a slight increase of about 1\,kpc towards $z = 1$ ismeasured in the F200W sample, which has a mean of 2.9\,kpc. The bar sample isshorter in the short-wavelength channel due to the better physical spatialresolution; however, we also suggest that dust obscuration plays a role. Wefind that the correlation between bar length and galaxy mass for massivegalaxies observed at $z < 1$ is not seen at $z > 1$. By adding samples ofbarred galaxies at $z<1$, we show that there is a modest increase in the barlength ($\approx 2$\,kpc) towards $z=0$, but bars longer than $\approx8$\,kpcare only found at $z<1$. We show that bars and discs grow in tandem, for thebar length normalised by disc size does not evolve from $z = 4$ to $z = 0$. Notonly is a significant population of bars forming beyond $z = 1$, but ourresults also show that some of these bars are as long and strong as the averagebar at $z\approx0$.

El Gordo (ACT-CL J0102$-$4915) is a massive galaxy cluster with two majormass components at redshift $z=0.87$. Using SED fitting results fromJWST/NIRCam photometry, the fraction of quenched galaxies in this cluster wasmeasured in two bins of stellar mass: $9<\log{({M_*}/\mathrm{M}_{\odot})}<10$and $10\leq\log{({M_*}/\mathrm{M}_{\odot})}<12$. While there is no correlationbetween the quenched fraction and angular separation from the cluster's overallcenter of mass, there is a correlation between the quenched fraction andangular separation from the center of the nearest of the two mass componentsfor the less-massive galaxies. This suggests that environmental quenchingprocesses are in place at $z\sim1$, and that dwarf galaxies are more affectedby those processes than massive galaxies.