We study the evolution of the bar fraction in disc galaxies between $0.5 < z< 4.0$ using multi-band coloured images from JWST CEERS. These images wereclassified by citizen scientists in a new phase of the Galaxy Zoo projectcalled GZ CEERS. Citizen scientists were asked whether a strong or weak bar wasvisible in the host galaxy. After considering multiple corrections forobservational biases, we find that the bar fraction decreases with redshift inour volume-limited sample (n = 398); from $25^{+6}_{-4}$% at $0.5 < z < 1.0$ to$3^{+6}_{-1}$% at $3.0 < z < 4.0$. However, we argue it is appropriate tointerpret these fractions as lower limits. Disentangling real changes in thebar fraction from detection biases remains challenging. Nevertheless, we find asignificant number of bars up to $z = 2.5$. This implies that discs aredynamically cool or baryon-dominated, enabling them to host bars. This alsosuggests that bar-driven secular evolution likely plays an important role athigher redshifts. When we distinguish between strong and weak bars, we findthat the weak bar fraction decreases with increasing redshift. In contrast, thestrong bar fraction is constant between $0.5 < z < 2.5$. This implies that thestrong bars found in this work are robust long-lived structures, unless therate of bar destruction is similar to the rate of bar formation. Finally, ourresults are consistent with disc instabilities being the dominant mode of barformation at lower redshifts, while bar formation through interactions andmergers is more common at higher redshifts.

The radial acceleration relation (RAR) is a fundamental relation linkingbaryonic and dark matter in galaxies by relating the observed accelerationderived from dynamics to the one estimated from the baryonic mass. Thisrelation exhibits small scatter, thus providing key constraints for models ofgalaxy formation and evolution -- allowing us to map the distribution of darkmatter in galaxies -- as well as models of modified dynamics. However, it hasonly been extensively studied in the very local Universe with largelyheterogeneous samples. We present a new measurement of the RAR, utilising ahomogeneous, unbiased sample of H{\sc i}-selected galaxies. We introduce anovel approach of measuring resolved stellar masses using spectral energydistribution (SED) fitting across 10 photometric bands to determine theresolved mass-to-light ratio, which we show is essential for measuring theacceleration due to baryons in the low-acceleration regime. We find that thestellar mass-to-light ratio varies across galaxies and radially, favouringlower mass-to-light ratios compared to previous studies. Our results reveal atight RAR with a low-acceleration power-law slope of $\sim 0.5$, consistentwith previous studies. Adopting a spatially varying mass-to-light ratio yieldsthe tightest RAR with an intrinsic scatter of only $0.045 \pm 0.022$ dex. Wealso find the first tentative evidence for redshift evolution in theacceleration scale, but more data will be required to confirm this. Theseresults highlight the importance of resolved stellar mass measurements inaccurately characterizing the gravitational contribution of the baryons inlow-mass, gas-rich galaxies.