Soto-Pinto, Pamela, Nagar, Neil M., Finlez, Carolina, Ramakrishnan, Venkatessh, Muñoz-Vergara, Dania, Slater, Roy, Humire, Pedro K., Storchi-Bergmann, Thaisa, Lena, Davide, Kraemer, Steven B., Fischer, Travis C., Schmitt, Henrique R., Riffel, Rogemar A., Schnorr-Müller, Allan, Robinson, Andrew, Crenshaw, D. Michael, and Elvis, Martin S. 2019. "Outflowing gas in a compact ionization cone in the Seyfert 2 galaxy ESO 153-G20." Monthly Notices of the Royal Astronomical Society, 489 4111–4124. https://doi.org/10.1093/mnras/stz2333.
We present two-dimensional ionized gas and stellar kinematics in the inner 1.4 × 1.9 kpc2 of the Seyfert 2 galaxy ESO 153-G20 obtained with the Gemini-South/Gemini multi-object spectrograph integral field unit (GMOS-IFU) at a spatial resolution of 250 pc and spectral resolution of 36 km s-1. Strong [O III], Hα, [N II] and [S II] emission lines are detected over the entire field of view. The stellar kinematics trace circular rotation with a projected velocity amplitude of ±96 km s-1, a kinematic major axis in position angle of 11°, and an average velocity dispersion of 123 km s-1. To analyse the gas kinematics, we used aperture spectra, position-velocity diagrams and single/double Gaussian fits to the emission lines. All lines show two clear kinematic components: a rotating component that follows the stellar kinematics, and a larger- dispersion component, close to the systemic velocity (from which most of the [O III] emission comes), mainly detected to the south-west. We interpret this second component as gas outflowing at ∼400 km s-1 in a compact (300 pc) ionization cone with a half-opening angle ≤40°. The counter-cone is probably obscured behind a dust lane. We estimate a mass outflow rate of 1.1 M☉ yr-1, 200 times larger than the estimated accretion rate on to the supermassive black hole, and a kinetic to radiative power ratio of 1.7 × 10-3. Bar-induced perturbations probably explain the remaining disturbances observed in the velocity field of the rotating gas component.
