2018A&A...614A..94H

We present two-dimensional stellar and gaseous kinematics of the inner 0.7 x 1.2 kpc² of the Seyfert 1.5 galaxy ESO 362-G18, derived from optical (4092-7338 Å) spectra obtained with the GMOS integral field spectrograph on the Gemini South telescope at a spatial resolution of ≃170 pc and spectral resolution of 36 km s^–1. ESO 362-G18 is a strongly perturbed galaxy of morphological type Sa or S0/a, with a minor merger approaching along the NE direction. Previous studies have shown that the [OIII] emission shows a fan-shaped extension of ≃10'' to the SE. We detect the [OIII] doublet, [NII] and Hα emission lines throughout our field of view.The stellar kinematics is dominated by circular motions in the galaxy plane, with a kinematic position angle of ≃137° and is centred approximately on the continuum peak. The gas kinematics is also dominated by rotation, with kinematic position angles ranging from 122° to 139°, projected velocity amplitudes of the order of 100 km s^–1, and a mean velocity dispersion of 100 km s^–1. A double-Gaussian fit to the [OIII]λ5007 and Hα lines, which have the highest signal to noise ratios of the emission lines, reveal two kinematic components: (1) a component at lower radial velocities which we interpret as gas rotating in the galactic disk; and (2) a component with line of sight velocities 100-250 km s^–1 higher than the systemic velocity, interpreted as originating in the outflowing gas within the AGN ionization cone. We estimate a mass outflow rate of 7.4 x 10^–2 M_☉ yr^–1 in the SE ionization cone (this rate doubles if we assume a biconical configuration), and a mass accretion rate on the supermassive black hole (SMBH) of 2.2 x 10^–2 M_☉ yr^–1. The total ionized gas mass within ∼84 pc of the nucleus is 3.3 x 10⁵ M_☉; infall velocities of ∼34 km s^–1 in this gas would be required to feed both the outflow and SMBH accretion.