Context : Tracing nuclear inflows and outflows in AGNs , determining the mass of gas involved in these , and their impact on the host galaxy and nuclear black hole , requires 3-D imaging studies of both the ionized and molecular gas .

Aims : We aim to map the distribution and kinematics of molecular and ionized gas in a sample of active galaxies , to quantify the nuclear inflows and outflows .
Here , we analyze the nuclear kinematics of NGC 1566 via ALMA observations of the CO J:2-1 emission at 24 pc spatial and \sim 2.6 km s ^ { -1 } spectral resolution , and Gemini-GMOS/IFU observations of ionized gas emission lines and stellar absorption lines at similar spatial resolution , and 123 km s ^ { -1 } of intrinsic spectral resolution .

Methods : The morphology and kinematics of stellar , molecular ( CO ) and ionized ( [ N II ] ) emission lines are compared to the expectations from rotation , outflows , and streaming inflows .

Results : While both ionized and molecular gas show rotation signatures , there are significant non-circular motions in the innermost 200 pc and along spiral arms in the central kpc ( CO ) .
The nucleus shows a double-peaked CO profile ( Full Width at Zero Intensity of 200 km s ^ { -1 } ) , and prominent ( \sim 80 km s ^ { -1 } ) blue and redshifted lobes are found along the minor axis in the inner arcseconds .
Perturbations by the large-scale bar can qualitatively explain all features in the observed velocity field .
We thus favour the presence of a molecular outflow in the disk with true velocities of \sim 180 km s ^ { -1 } in the nucleus and decelerating to 0 by \sim 72 pc .
The implied molecular outflow rate is 5.6 ~ { } [ M _ { \odot } yr ^ { -1 } ] , with this gas accumulating in the nuclear 2″ arms .
The ionized gas kinematics support an interpretation of a similar , but more spherical , outflow in the inner 100 pc , with no signs of deceleration .
There is some evidence of streaming inflows of \sim 50 km s ^ { -1 } along specific spiral arms , and the estimated molecular mass inflow rate , \sim 0.1 ~ { } [ M _ { \odot } yr ^ { -1 } ] , is significantly larger than the SMBH accretion rate ( \dot { m } = 4.8 \times 10 ^ { -5 } ~ { } [ M _ { \odot } yr ^ { -1 } ] ) .

Conclusions :