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The global properties of the interstellar medium with processes such asinfall and outflow of gas and a large scale circulation of matter and itsconsequences for star formation and chemical enrichment are important for theunderstanding of galaxy evolution. In this paper we studied the kinematics andmorphology of the diffuse ionized gas (DIG) in the disk and in the halo of thestar forming spiral galaxy NGC 4666 to derive information about its kinematicalproperties. Especially, we searched for infalling and outflowing ionized gas.We determined surface brightness, radial velocity, and velocity dispersion ofthe warm ionized gas via high spectral resolution (R ~ 9000) Fabry-P\'erotinterferometry. This allows the determination of the global velocity field andthe detection of local deviations from this verlocity field. We calculatedmodels of the DIG distribution and its kinematics for comparison with themeasured data. In this way we determined fundamental parameters such as theinclination and the scale height of NGC 4666, and established the need for anadditional gas component to fit our observed data. We found individual areas,especially along the minor axis, with gas components reaching into the halowhich we interpret as an outflowing component of the diffuse ionized gas. Asthe main result of our study, we were able to determine that the verticalstructure of the DIG distribution in NGC 4666 is best modeled with twocomponents of ionized gas, a thick and a thin disk with 0.8 kpc and 0.2 kpcscale height, respectively. Therefore, the enhanced star formation in NGC 4666drives an outflow and also maintains a thick ionized gas layer reminiscent ofthe Reynold's layer in the Milky Way.

The kinematics of the diffuse ionized gas in NGC 4666