  The underlying nature of the process of star formation quenching in the
central regions of barred disc galaxies that is due to the action of stellar
bar is not fully understood. We present a multi-wavelength study of four barred
galaxies using the archival data from optical, ultraviolet, infrared, CO, and
HI imaging data on star formation progression and stellar and gas distribution
to better understand the process of bar quenching. We found that for three
galaxies, the region between the nuclear or central sub-kiloparsec region and
the end of the bar (bar region) is devoid of neutral and molecular hydrogen.
While the detected neutral hydrogen is very negligible, we note that molecular
hydrogen is present abundantly in the nuclear or central sub-kiloparsec regions
of all four galaxies. The bar co-rotation radius is also devoid of recent star
formation for three out of four galaxies. One galaxy shows significant
molecular hydrogen along the bar, which might mean that the gas is still being
funnelled to the centre by the action of the stellar bar. Significant star
formation is also present along the bar co-rotation radius of this galaxy. The
study presented here supports a scenario in which gas redistribution as a
result of the action of stellar bar clears the bar region of fuel for further
star formation and eventually leads to star formation quenching in the bar
region.
