  We compare the abundant prolate shaped galaxies reported beyond z$>$3 in deep
JWST surveys, with the predicted {\it stellar} appearance of young galaxies in
detailed hydro-simulations of three main dark matter contenders: Cold (CDM),
Wave/Fuzzy ($\psi$DM) and Warm Dark Matter (WDM). We find the observed galaxy
images closely resemble the elongated stellar appearance of young galaxies
predicted for both $\psi$DM and WDM, during the first $\simeq$ 500Myr while
material steadily accretes from long, smooth filaments. The dark mater halos of
WDM and $\psi$DM also have pronounced, prolate elongation similar to the stars,
indicating a shared, highly triaxial equilibrium. This is unlike CDM where the
early stellar morphology is mainly spheroidal formed from fragmented filaments
with frequent merging, resulting in modest triaxiality. Quantitatively, the
excess of prolate galaxies observed by JWST matches well WDM and $\psi$DM for
particle masses of 1.4KeV and $2.5\times 10^{-22}$ eV respectively. For CDM,
several visible subhalos are typically predicted to orbit within the virial
radius of each galaxy from subhalo accretion, whereas merging is initially rare
for WDM and $\psi$DM. We also verify with our simulations that $\psi$DM may be
distinguished from WDM by the form of the core, which is predicted to be smooth
and centered for WDM, but is a dense soliton for $\psi$DM traced by stars and
measurably offset from the galaxy center by random wave perturbations in the
simulations. We emphasise that long smooth filaments absent of galaxies may
prove detectable with JWST, traced by stars and gas with comoving lengths of
150kpc predicted at z$\simeq$10, depending on the particle mass of $\psi$DM or
WDM.
