  Large-scale bars can fuel galaxy centers with molecular gas, often leading to
the development of dense ring-like structures where intense star formation
occurs, forming a very different environment compared to galactic disks. We
pair ~0.3" (30pc) resolution new JWST/MIRI imaging with archival ALMA CO(2-1)
mapping of the central ~5kpc of the nearby barred spiral galaxy NGC1365, to
investigate the physical mechanisms responsible for this extreme star
formation. The molecular gas morphology is resolved into two well-known bright
bar lanes that surround a smooth dynamically cold gas disk (R_gal ~ 475pc)
reminiscent of non-star-forming disks in early type galaxies and likely fed by
gas inflow triggered by stellar feedback in the lanes. The lanes host a large
number of JWST-identified massive young star clusters. We find some evidence
for temporal star formation evolution along the ring. The complex kinematics in
the gas lanes reveal strong streaming motions and may be consistent with
convergence of gas streamlines expected there. Indeed, the extreme line-widths
are found to be the result of inter-`cloud' motion between gas peaks; ScousePy
decomposition reveals multiple components with line widths of <sigma_CO,scouse>
~ 19km/s and surface densities of <Sigma_H2,scouse> ~ 800M_sun/pc^2, similar to
the properties observed throughout the rest of the central molecular gas
structure. Tailored hydro-dynamical simulations exhibit many of the observed
properties and imply that the observed structures are transient and highly
time-variable. From our study of NGC1365, we conclude that it is predominantly
the high gas inflow triggered by the bar that is setting the star formation in
its CMZ.
