  The suppression of star formation in the inner kiloparsec regions of barred
disk galaxies due to the action of bars is known as bar quenching. We
investigate here the significance of bar quenching in the global quenching of
star formation in the barred galaxies and their transformation to passive
galaxies in the local Universe. We do this by measuring the offset of quenched
barred galaxies from star-forming main sequence galaxies in the star formation
rate-stellar mass plane and comparing it with the length of the bar, which is
considered as a proxy of bar quenching. We constructed the star formation
rate-stellar mass plane of 2885 local Universe face-on strong barred disk
galaxies ($z<0.06$) identified by Galaxy Zoo. The barred disk galaxies studied
here fall on the star formation main sequence relation with a significant
scatter for galaxies above stellar mass 10$^{10.2}$ M$\odot$. We found that
34.97 $\%$ galaxies are within the intrinsic scatter (0.3 dex) of the main
sequence relation, with a starburst population of 10.78 $\%$ (above the 0.3
dex) and a quenched population of 54.25 $\%$ (below the -0.3 dex) of the total
barred disk galaxies in our sample. Significant neutral hydrogen (M$_{HI}$
>10$^{9}$ M$\odot$ with log M$_{HI}$/M$\star$ $\sim$ -1.0 to -0.5) is detected
in the quenched barred galaxies with a similar gas content to that of the
star-forming barred galaxies. We found that the offset of the quenched barred
galaxies from the main sequence relation is not dependent on the length of the
stellar bar. This implies that the bar quenching may not contribute
significantly to the global quenching of star formation in barred galaxies.
However, this observed result could also be due to other factors such as the
dissolution of bars over time after star formation quenching, the effect of
other quenching processes acting simultaneously, and/or the effects of
environment.
