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The star formation efficiency (SFE) has been shown to vary across differentenvironments, particularly within galactic starbursts and deep within thebulges of galaxies. Various quenching mechanisms may be responsible, rangingfrom galactic dynamics to feedback from active galactic nuclei (AGN). Here, weuse spatially-resolved observations of warm ionised gas emission lines from theimaging Fourier transform spectrograph SITELLE at the Canada-France-HawaiiTelescope (CFHT) and cold molecular gas (CO(2-1)) from the Atacama LargeMillimeter/sub-millimeter Array (ALMA) to study the SFE in the bulge of theAGN-host galaxy NGC 3169. After distinguishing star-forming regions fromAGN-ionised regions using emission-line ratio diagnostics, we measurespatially-resolved molecular gas depletion times (\tau_dep = 1/SFE) with aspatial resolution of \approx 100 pc within a galactocentric radius of 1.8 kpc.We identify a star-forming ring located at radii 1.25 \pm 0.6 kpc with anaverage \tau_dep of 0.3 Gyr. At radii < 0.9 kpc, however, the molecular gassurface densities and depletion times increase with decreasing radius, thelatter reaching approximately 2.3 Gyr at a radius \approx 500 pc. Based onanalyses of the gas kinematics and comparisons with simulations, we identifyAGN feedback, bulge morphology and dynamics as the possible causes of theradial profile of SFE observed in the central region of NGC 3169.

WISDOM project -- XI. Star Formation Efficiency in the Bulge of the AGN-host Galaxy NGC 3169 with SITELLE and ALMA