We use spatially resolved spectroscopy from the Calar Alto Legacy Integral Field Area (CALIFA) survey to study the nature of the line emitting gas in galaxies of different Hubble types, focusing on the separation of star-forming (SF) regions from those better characterized as diffuse ionized gas (DIG). The diagnosis is carried out in terms of the equivalent width of Hα (W Hα ). Three nebular regimes are identified. Regions where W Hα < 3Å define what we call the hDIG, the component of the DIG where photoionization is dominated by hot, low-mass, evolved stars. Regions where W Hα > 14Å trace SF complexes. W Hα values in the intermediate 3-14Å range reflect a mixed regime (mDIG) where more than one process contributes.This three-tier scheme is inspired both by theoretical and empirical considerations. Its application to CALIFA galaxies of different types and inclinations leads to the following results: (i) the hDIG component is prevalent throughout ellipticals and S0's as well as in bulges, and explains the strongly bimodal distribution of W Hα both among and within galaxies. (ii) Earlytype spirals have some hDIG in their discs, but this component becomes progressively less relevant for later Hubble types. (iii) hDIG emission is also present above and below galactic discs, as seen in several edge-on spirals in our sample. (iv) The SF/mDIG proportion grows steadily from early-to late-type spirals, and from inner to outer radii. (v) Besides circumventing basic inconsistencies in conventional DIG/SF separation criteria based on the Hα surface brightness, our W Hα -based method produces results in agreement with a classical excitation diagram analysis.

We present optical integral field spectroscopy of the circum-nuclear gas of the Seyfert 2 galaxy NGC 1386. The data cover the central 7 × 9 (530 × 680 pc) at a spatial resolution of 0. 9 (68 pc), and the spectral range 5700-7000Å at a resolution of 66 km s −1 . The line emission is dominated by a bright central component, with two lobes extending ≈ 3 north and south of the nucleus. We identify three main kinematic components. The first has low velocity dispersion (σ ≈ 90 km s −1 ), extends over the whole field-of-view, and has a velocity field consistent with gas rotating in the galaxy disk. We interpret the lobes as resulting from photoionization of disk gas in regions where the AGN radiation cones intercept the disk. The second has higher velocity dispersion (σ ≈ 200 km s −1 ) and is observed in the inner 150 pc around the continuum peak. This component is double peaked, with redshifted and blueshifted components separated by ≈ 500 km s −1 . Together with previous HST imaging, these features suggest the presence of a bipolar outflow for which we estimate a mass outflow rate ofṀ 0.1 M yr −1 . The third component is revealed by velocity residuals associated with enhanced velocity dispersion and suggests that outflow and/or rotation is occurring approximately in the equatorial plane of the torus. A second system of velocity residuals may indicate the presence of streaming motions along dusty spirals in the disk.

We present two-dimensional gaseous kinematics of the inner 1.1 × 1.6 kpc 2 of the Seyfert 2 galaxy NGC 2110, from optical spectra (5600-7000Å) obtained with the GMOS integral field spectrograph on the Gemini South telescope at a spatial resolution of ≈ 100 pc. Gas emission is observed over the whole field-of-view, with complex -and frequently double -emissionline profiles. We have identified four components in the emitting gas, according to their velocity dispersion (σ), which we refer to as: (1) warm gas disk (σ = 100-220 km s −1 ); (2) cold gas disk (σ = 60-90 km s −1 ); (3) nuclear component (σ = 220-600 km s −1 ); and (4) northern cloud (σ = 60-80 km s −1 ). Both the cold and warm disk components are dominated by rotation and have similar gas densities, but the cold gas disk has lower velocity dispersions and reaches higher rotation velocities. We attribute the warm gas disk to a thick gas layer which encompasses the cold disk as observed in some edge-on spiral galaxies. After subtraction of a rotation model from the cold disk velocity field, we observe excess blueshifts of ≈ 50 km s −1 in the far side of the galaxy (NE) as well as similar excess redshifts in the near side (SW). These residuals can be interpreted as due to nuclear inflow in the cold gas, with an estimated ionized gas mass inflow rate of φ ≈ 2.2 × 10 −2 M ⊙ yr −1 . We have also subtracted a rotating model from the warm disk velocity field and found excess blueshifts of ≈ 100 km s −1 to the SW of the nucleus and excess redshifts of ≈ 40 km s −1 to the NE, which we attribute to gas disturbed by an interaction with a nuclear spherical outflow. This nuclear outflow is the origin of the nuclear component observed within the inner 300 pc and it has a mass outflow rate of 0.9 M ⊙ yr −1 . In a region between 1 ′′ and 4 ′′ north of the nucleus, which shows strong X-ray and [O III] λ5007Å emission, we find a new low σ component of ionized gas which we attribute to a high latitude cloud photoionized by the nuclear source. The identification of the 4 distinct kinematic components has clarified the nature of the apparent asymmetry in the rotation curve of the galaxy pointed out in previous studies: it results from the dominance of different components to the south and north of the nucleus. We conclude that a comprehensive two-dimensional coverage of the kinematics and geometry of the nuclear gas around the AGN is necessary to reveal the different processes at play, such as its feeding -via the cold inflowing gas -and the feedback, via the warm gas outflows.

We present optical integral field spectroscopy -obtained with the Gemini Multi-Object Spectrograph -of the inner 4.0 × 5.8 kpc 2 of the narrow line radio galaxy 3C 33 at a spatial resolution of 0.58 kpc. The gas emission shows three brightest structures: a strong knot of nuclear emission and two other knots at ≈ 1.4 kpc south-west and northeast of the nucleus along the ionization axis. We detect two kinematic components in the emission lines profiles, with a "broader component" (with velocity dispersion σ 150 km s −1 ) being dominant within a ∼ 1 kpc wide strip ("the nuclear strip") running from the south-east to the north-west, perpendicular to the radio jet, and a narrower component (σ 100 km s −1 ) dominating elsewhere. Centroid velocity maps reveal a rotation pattern with velocity amplitudes reaching ∼ ±350 km s −1 in the region dominated by the narrow component, while residual blueshifts and redshifts relative to rotation are observed in the nuclear strip, where we also observe the highest values of the [N ii]/Hα, [S ii]/Hα and [O i]/Hα line ratios, and an increase of the gas temperature (∼ 18000 K), velocity dispersion and electron density (∼ 500 cm −3 ). We interpret these residuals and increased line ratios as due to a lateral expansion of the ambient gas in the nuclear strip due to shocks produced by the passage of the radio jet. The effect of this expansion in the surrounding medium is very small, as its estimated kinetic power represents only 2.6 − 3.0 × 10 −5 of the AGN bolometric luminosity. A possible signature of inflow is revealed by an increase in the [O i]/Hα ratio values and velocity dispersions in the shape of two spiral arms extending to 2.3 kpc north-east and south-west from the nucleus.