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The physical processes related to the effect of bar in the quenching of starformation in the region between the nuclear/central sub-kpc region and the endsof the bar (bar-region) of spiral galaxies is not fully understood. It ishypothesized that the bar can either stabilize the gas against collapse,inhibiting star formation or efficiently consume all the available gas, with nofuel for further star formation. We present a multi-wavelength study using thearchival data of an early-type barred spiral galaxy, Messier 95, which showssignatures of suppressed star formation in the bar-region. Using the optical,ultraviolet, infrared, CO and HI imaging data we study the pattern of starformation progression, stellar/gas distribution and try to provide insights onthe process responsible for the observed pattern. The FUV$-$NUV pixel colourmap reveals a cavity devoid of UV flux in the bar-region that interestinglymatches with the length of the bar ($\sim$ 4.2kpc). The central nuclear regionof the galaxy is showing a blue color clump and along the major-axis of thestellar bar the colour progressively becomes redder. Based on a comparison tosingle stellar population models, we show that the region of galaxy along themajor-axis of the bar (unlike the region outside the bar) is comprised ofstellar populations with ages $\geq$ 350 Myr, with a star-forming clump in thecenter of younger ages ($\sim$ 150Myr). Interestingly the bar-region is alsodevoid of neutral and molecular hydrogen but with an abundant molecularhydrogen present at the nuclear region of the galaxy. Our results areconsistent with a picture in which the stellar bar in Messier 95 isredistributing the gas by funneling gas inflows to nuclear region, thus makingthe bar-region devoid of fuel for star formation.

Insights on bar quenching from a multi-wavelength analysis: The case of Messier 95